PDS/PPI Home Page

QUICK SEARCH

Search By Missions

QUICK LINKS

FAQ
Citation Policy
Errata for all volumes
Help for Data Users
Help for Data Reviewers
Help for Data Providers

PDS NODES

PDS Home
Atmospheres
Geosciences
Cartography and Imaging Sciences
NAIF - SPICE
Ring-Moon Systems
Small Bodies

Cassini >> MIMI

CASSINI SATURN MIMI LEMMS CALIBRATED DATA ARCHIVE
CO-S-MIMI-4-LEMMS-CALIB-V1.0	PDS 3 CERTIFIED

Start Time: 2004-01-01 08:00:00 - Stop Time: 2017-09-16 10:00:00

This contains calibrated Saturn tour data collected by the LEMMS sensor of the MIMI instrument aboard the Cassini spacecraft for the Cassini mission.

Citiation Information

Author	Vandegriff J., Kusterer M.B.
Title	CASSINI SATURN MIMI LEMMS CALIBRATED DATA ARCHIVE
Publisher	NASA Planetary Data System
Publication Year	2018
doi	https://doi.org/10.17189/1519608

Top/ DATA/ LPHAAVG0_1MIN/ 2010 /

LPHAAVG0_1MIN_2010001_01

Start Time:	2010-001T00:00	Stop Time:	2010-002T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010002_01

Start Time:	2010-002T00:00	Stop Time:	2010-003T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010003_01

Start Time:	2010-003T00:00	Stop Time:	2010-004T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010004_01

Start Time:	2010-004T00:00	Stop Time:	2010-005T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010005_01

Start Time:	2010-005T00:00	Stop Time:	2010-006T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010006_01

Start Time:	2010-006T00:00	Stop Time:	2010-007T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010007_01

Start Time:	2010-007T00:00	Stop Time:	2010-008T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010008_01

Start Time:	2010-008T00:00	Stop Time:	2010-009T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010009_01

Start Time:	2010-009T00:00	Stop Time:	2010-010T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010010_01

Start Time:	2010-010T00:00	Stop Time:	2010-011T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010011_01

Start Time:	2010-011T00:00	Stop Time:	2010-012T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010012_01

Start Time:	2010-012T00:00	Stop Time:	2010-013T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010013_01

Start Time:	2010-013T00:00	Stop Time:	2010-014T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010014_01

Start Time:	2010-014T00:00	Stop Time:	2010-015T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010015_01

Start Time:	2010-015T00:00	Stop Time:	2010-016T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010016_01

Start Time:	2010-016T00:00	Stop Time:	2010-017T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010017_01

Start Time:	2010-017T00:00	Stop Time:	2010-018T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010018_01

Start Time:	2010-018T00:00	Stop Time:	2010-019T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010019_01

Start Time:	2010-019T00:00	Stop Time:	2010-020T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010020_01

Start Time:	2010-020T00:00	Stop Time:	2010-021T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010021_01

Start Time:	2010-021T00:00	Stop Time:	2010-022T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010022_01

Start Time:	2010-022T00:00	Stop Time:	2010-023T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010023_01

Start Time:	2010-023T00:00	Stop Time:	2010-024T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010024_01

Start Time:	2010-024T00:00	Stop Time:	2010-025T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010025_01

Start Time:	2010-025T00:00	Stop Time:	2010-026T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010026_01

Start Time:	2010-026T00:00	Stop Time:	2010-027T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010027_01

Start Time:	2010-027T00:00	Stop Time:	2010-028T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010028_01

Start Time:	2010-028T00:00	Stop Time:	2010-029T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010029_01

Start Time:	2010-029T00:00	Stop Time:	2010-030T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010030_01

Start Time:	2010-030T00:00	Stop Time:	2010-031T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010031_01

Start Time:	2010-031T00:00	Stop Time:	2010-032T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010032_01

Start Time:	2010-032T00:00	Stop Time:	2010-033T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010033_01

Start Time:	2010-033T00:00	Stop Time:	2010-034T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010034_01

Start Time:	2010-034T00:00	Stop Time:	2010-035T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010035_01

Start Time:	2010-035T00:00	Stop Time:	2010-036T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010036_01

Start Time:	2010-036T00:00	Stop Time:	2010-037T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010037_01

Start Time:	2010-037T00:00	Stop Time:	2010-038T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010038_01

Start Time:	2010-038T00:00	Stop Time:	2010-039T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010039_01

Start Time:	2010-039T00:00	Stop Time:	2010-040T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010040_01

Start Time:	2010-040T00:00	Stop Time:	2010-041T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010041_01

Start Time:	2010-041T00:00	Stop Time:	2010-042T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010042_01

Start Time:	2010-042T00:00	Stop Time:	2010-043T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010043_01

Start Time:	2010-043T00:00	Stop Time:	2010-044T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010044_01

Start Time:	2010-044T00:00	Stop Time:	2010-045T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010045_01

Start Time:	2010-045T00:00	Stop Time:	2010-046T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010046_01

Start Time:	2010-046T00:00	Stop Time:	2010-047T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010047_01

Start Time:	2010-047T00:00	Stop Time:	2010-048T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010048_01

Start Time:	2010-048T00:00	Stop Time:	2010-049T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010049_01

Start Time:	2010-049T00:00	Stop Time:	2010-050T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010050_01

Start Time:	2010-050T00:00	Stop Time:	2010-051T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010051_01

Start Time:	2010-051T00:00	Stop Time:	2010-052T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010052_01

Start Time:	2010-052T00:00	Stop Time:	2010-053T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010053_01

Start Time:	2010-053T00:00	Stop Time:	2010-054T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010054_01

Start Time:	2010-054T00:00	Stop Time:	2010-055T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010055_01

Start Time:	2010-055T00:00	Stop Time:	2010-056T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010056_01

Start Time:	2010-056T00:00	Stop Time:	2010-057T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010057_01

Start Time:	2010-057T00:00	Stop Time:	2010-058T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010058_01

Start Time:	2010-058T00:00	Stop Time:	2010-059T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010059_01

Start Time:	2010-059T00:00	Stop Time:	2010-060T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010060_01

Start Time:	2010-060T00:00	Stop Time:	2010-061T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010061_01

Start Time:	2010-061T00:00	Stop Time:	2010-062T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010062_01

Start Time:	2010-062T00:00	Stop Time:	2010-063T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010063_01

Start Time:	2010-063T00:00	Stop Time:	2010-064T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010064_01

Start Time:	2010-064T00:00	Stop Time:	2010-065T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010065_01

Start Time:	2010-065T00:00	Stop Time:	2010-066T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010066_01

Start Time:	2010-066T00:00	Stop Time:	2010-067T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010067_01

Start Time:	2010-067T00:00	Stop Time:	2010-068T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010068_01

Start Time:	2010-068T00:00	Stop Time:	2010-069T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010069_01

Start Time:	2010-069T00:00	Stop Time:	2010-070T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010070_01

Start Time:	2010-070T00:00	Stop Time:	2010-071T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010071_01

Start Time:	2010-071T00:00	Stop Time:	2010-072T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010072_01

Start Time:	2010-072T00:00	Stop Time:	2010-073T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010073_01

Start Time:	2010-073T00:00	Stop Time:	2010-074T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010074_01

Start Time:	2010-074T00:00	Stop Time:	2010-075T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010075_01

Start Time:	2010-075T00:00	Stop Time:	2010-076T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010076_01

Start Time:	2010-076T00:00	Stop Time:	2010-077T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010077_01

Start Time:	2010-077T00:00	Stop Time:	2010-078T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010078_01

Start Time:	2010-078T00:00	Stop Time:	2010-079T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010079_01

Start Time:	2010-079T00:00	Stop Time:	2010-080T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010080_01

Start Time:	2010-080T00:00	Stop Time:	2010-081T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010081_01

Start Time:	2010-081T00:00	Stop Time:	2010-082T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010082_01

Start Time:	2010-082T00:00	Stop Time:	2010-083T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010083_01

Start Time:	2010-083T00:00	Stop Time:	2010-084T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010084_01

Start Time:	2010-084T00:00	Stop Time:	2010-085T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010085_01

Start Time:	2010-085T00:00	Stop Time:	2010-086T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010086_01

Start Time:	2010-086T00:00	Stop Time:	2010-087T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010087_01

Start Time:	2010-087T00:00	Stop Time:	2010-088T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010088_01

Start Time:	2010-088T00:00	Stop Time:	2010-089T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010089_01

Start Time:	2010-089T00:00	Stop Time:	2010-090T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010090_01

Start Time:	2010-090T00:00	Stop Time:	2010-091T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010091_01

Start Time:	2010-091T00:00	Stop Time:	2010-092T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010092_01

Start Time:	2010-092T00:00	Stop Time:	2010-093T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010093_01

Start Time:	2010-093T00:00	Stop Time:	2010-094T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010094_01

Start Time:	2010-094T00:00	Stop Time:	2010-095T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010095_01

Start Time:	2010-095T00:00	Stop Time:	2010-096T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010096_01

Start Time:	2010-096T00:00	Stop Time:	2010-097T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010097_01

Start Time:	2010-097T00:00	Stop Time:	2010-098T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010098_01

Start Time:	2010-098T00:00	Stop Time:	2010-099T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010099_01

Start Time:	2010-099T00:00	Stop Time:	2010-100T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010100_01

Start Time:	2010-100T00:00	Stop Time:	2010-101T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010101_01

Start Time:	2010-101T00:00	Stop Time:	2010-102T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010102_01

Start Time:	2010-102T00:00	Stop Time:	2010-103T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010103_01

Start Time:	2010-103T00:00	Stop Time:	2010-104T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010104_01

Start Time:	2010-104T00:00	Stop Time:	2010-105T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010105_01

Start Time:	2010-105T00:00	Stop Time:	2010-106T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010106_01

Start Time:	2010-106T00:00	Stop Time:	2010-107T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010107_01

Start Time:	2010-107T00:00	Stop Time:	2010-108T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010108_01

Start Time:	2010-108T00:00	Stop Time:	2010-109T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010109_01

Start Time:	2010-109T00:00	Stop Time:	2010-110T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010110_01

Start Time:	2010-110T00:00	Stop Time:	2010-111T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010111_01

Start Time:	2010-111T00:00	Stop Time:	2010-112T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010112_01

Start Time:	2010-112T00:00	Stop Time:	2010-113T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010113_01

Start Time:	2010-113T00:00	Stop Time:	2010-114T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010114_01

Start Time:	2010-114T00:00	Stop Time:	2010-115T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010115_01

Start Time:	2010-115T00:00	Stop Time:	2010-116T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010116_01

Start Time:	2010-116T00:00	Stop Time:	2010-117T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010117_01

Start Time:	2010-117T00:00	Stop Time:	2010-118T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010118_01

Start Time:	2010-118T00:00	Stop Time:	2010-119T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010119_01

Start Time:	2010-119T00:00	Stop Time:	2010-120T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010120_01

Start Time:	2010-120T00:00	Stop Time:	2010-121T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010121_01

Start Time:	2010-121T00:00	Stop Time:	2010-122T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010122_01

Start Time:	2010-122T00:00	Stop Time:	2010-123T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010123_01

Start Time:	2010-123T00:00	Stop Time:	2010-124T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010124_01

Start Time:	2010-124T00:00	Stop Time:	2010-125T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010125_01

Start Time:	2010-125T00:00	Stop Time:	2010-126T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010126_01

Start Time:	2010-126T00:00	Stop Time:	2010-127T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010127_01

Start Time:	2010-127T00:00	Stop Time:	2010-128T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010128_01

Start Time:	2010-128T00:00	Stop Time:	2010-129T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010129_01

Start Time:	2010-129T00:00	Stop Time:	2010-130T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010130_01

Start Time:	2010-130T00:00	Stop Time:	2010-131T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010131_01

Start Time:	2010-131T00:00	Stop Time:	2010-132T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010132_01

Start Time:	2010-132T00:00	Stop Time:	2010-133T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010133_01

Start Time:	2010-133T00:00	Stop Time:	2010-134T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010134_01

Start Time:	2010-134T00:00	Stop Time:	2010-135T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010135_01

Start Time:	2010-135T00:00	Stop Time:	2010-136T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010136_01

Start Time:	2010-136T00:00	Stop Time:	2010-137T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010137_01

Start Time:	2010-137T00:00	Stop Time:	2010-138T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010138_01

Start Time:	2010-138T00:00	Stop Time:	2010-139T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010139_01

Start Time:	2010-139T00:00	Stop Time:	2010-140T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010140_01

Start Time:	2010-140T00:00	Stop Time:	2010-141T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010141_01

Start Time:	2010-141T00:00	Stop Time:	2010-142T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010142_01

Start Time:	2010-142T00:00	Stop Time:	2010-143T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010143_01

Start Time:	2010-143T00:00	Stop Time:	2010-144T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010144_01

Start Time:	2010-144T00:00	Stop Time:	2010-145T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010145_01

Start Time:	2010-145T00:00	Stop Time:	2010-146T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010146_01

Start Time:	2010-146T00:00	Stop Time:	2010-147T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010147_01

Start Time:	2010-147T00:00	Stop Time:	2010-148T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010148_01

Start Time:	2010-148T00:00	Stop Time:	2010-149T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010149_01

Start Time:	2010-149T00:00	Stop Time:	2010-150T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010150_01

Start Time:	2010-150T00:00	Stop Time:	2010-151T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010151_01

Start Time:	2010-151T00:00	Stop Time:	2010-152T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010152_01

Start Time:	2010-152T00:00	Stop Time:	2010-153T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010153_01

Start Time:	2010-153T00:00	Stop Time:	2010-154T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010154_01

Start Time:	2010-154T00:00	Stop Time:	2010-155T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010155_01

Start Time:	2010-155T00:00	Stop Time:	2010-156T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010156_01

Start Time:	2010-156T00:00	Stop Time:	2010-157T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010157_01

Start Time:	2010-157T00:00	Stop Time:	2010-158T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010158_01

Start Time:	2010-158T00:00	Stop Time:	2010-159T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010159_01

Start Time:	2010-159T00:00	Stop Time:	2010-160T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010160_01

Start Time:	2010-160T00:00	Stop Time:	2010-161T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010161_01

Start Time:	2010-161T00:00	Stop Time:	2010-162T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010162_01

Start Time:	2010-162T00:00	Stop Time:	2010-163T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010163_01

Start Time:	2010-163T00:00	Stop Time:	2010-164T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010164_01

Start Time:	2010-164T00:00	Stop Time:	2010-165T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010165_01

Start Time:	2010-165T00:00	Stop Time:	2010-166T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010166_01

Start Time:	2010-166T00:00	Stop Time:	2010-167T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010167_01

Start Time:	2010-167T00:00	Stop Time:	2010-168T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010168_01

Start Time:	2010-168T00:00	Stop Time:	2010-169T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010169_01

Start Time:	2010-169T00:00	Stop Time:	2010-170T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010170_01

Start Time:	2010-170T00:00	Stop Time:	2010-171T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010171_01

Start Time:	2010-171T00:00	Stop Time:	2010-172T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010172_01

Start Time:	2010-172T00:00	Stop Time:	2010-173T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010173_01

Start Time:	2010-173T00:00	Stop Time:	2010-174T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010174_01

Start Time:	2010-174T00:00	Stop Time:	2010-175T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010175_01

Start Time:	2010-175T00:00	Stop Time:	2010-176T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010176_01

Start Time:	2010-176T00:00	Stop Time:	2010-177T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010177_01

Start Time:	2010-177T00:00	Stop Time:	2010-178T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010178_01

Start Time:	2010-178T00:00	Stop Time:	2010-179T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010179_01

Start Time:	2010-179T00:00	Stop Time:	2010-180T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010180_01

Start Time:	2010-180T00:00	Stop Time:	2010-181T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010181_01

Start Time:	2010-181T00:00	Stop Time:	2010-182T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010182_01

Start Time:	2010-182T00:00	Stop Time:	2010-183T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010183_01

Start Time:	2010-183T00:00	Stop Time:	2010-184T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010184_01

Start Time:	2010-184T00:00	Stop Time:	2010-185T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010185_01

Start Time:	2010-185T00:00	Stop Time:	2010-186T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010186_01

Start Time:	2010-186T00:00	Stop Time:	2010-187T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010187_01

Start Time:	2010-187T00:00	Stop Time:	2010-188T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010188_01

Start Time:	2010-188T00:00	Stop Time:	2010-189T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010189_01

Start Time:	2010-189T00:00	Stop Time:	2010-190T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010190_01

Start Time:	2010-190T00:00	Stop Time:	2010-191T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010191_01

Start Time:	2010-191T00:00	Stop Time:	2010-192T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010192_01

Start Time:	2010-192T00:00	Stop Time:	2010-193T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010193_01

Start Time:	2010-193T00:00	Stop Time:	2010-194T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010194_01

Start Time:	2010-194T00:00	Stop Time:	2010-195T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010195_01

Start Time:	2010-195T00:00	Stop Time:	2010-196T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010196_01

Start Time:	2010-196T00:00	Stop Time:	2010-197T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010197_01

Start Time:	2010-197T00:00	Stop Time:	2010-198T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010198_01

Start Time:	2010-198T00:00	Stop Time:	2010-199T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010199_01

Start Time:	2010-199T00:00	Stop Time:	2010-200T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010200_01

Start Time:	2010-200T00:00	Stop Time:	2010-201T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010201_01

Start Time:	2010-201T00:00	Stop Time:	2010-202T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010202_01

Start Time:	2010-202T00:00	Stop Time:	2010-203T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010203_01

Start Time:	2010-203T00:00	Stop Time:	2010-204T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010204_01

Start Time:	2010-204T00:00	Stop Time:	2010-205T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010205_01

Start Time:	2010-205T00:00	Stop Time:	2010-206T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010206_01

Start Time:	2010-206T00:00	Stop Time:	2010-207T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010207_01

Start Time:	2010-207T00:00	Stop Time:	2010-208T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010208_01

Start Time:	2010-208T00:00	Stop Time:	2010-209T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010209_01

Start Time:	2010-209T00:00	Stop Time:	2010-210T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010210_01

Start Time:	2010-210T00:00	Stop Time:	2010-211T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010211_01

Start Time:	2010-211T00:00	Stop Time:	2010-212T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010212_01

Start Time:	2010-212T00:00	Stop Time:	2010-213T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010213_01

Start Time:	2010-213T00:00	Stop Time:	2010-214T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010214_01

Start Time:	2010-214T00:00	Stop Time:	2010-215T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010215_01

Start Time:	2010-215T00:00	Stop Time:	2010-216T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010216_01

Start Time:	2010-216T00:00	Stop Time:	2010-217T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010217_01

Start Time:	2010-217T00:00	Stop Time:	2010-218T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010218_01

Start Time:	2010-218T00:00	Stop Time:	2010-219T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010219_01

Start Time:	2010-219T00:00	Stop Time:	2010-220T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010220_01

Start Time:	2010-220T00:00	Stop Time:	2010-221T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010221_01

Start Time:	2010-221T00:00	Stop Time:	2010-222T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010222_01

Start Time:	2010-222T00:00	Stop Time:	2010-223T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010223_01

Start Time:	2010-223T00:00	Stop Time:	2010-224T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010224_01

Start Time:	2010-224T00:00	Stop Time:	2010-225T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010225_01

Start Time:	2010-225T00:00	Stop Time:	2010-226T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010226_01

Start Time:	2010-226T00:00	Stop Time:	2010-227T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010227_01

Start Time:	2010-227T00:00	Stop Time:	2010-228T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010228_01

Start Time:	2010-228T00:00	Stop Time:	2010-229T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010229_01

Start Time:	2010-229T00:00	Stop Time:	2010-230T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010230_01

Start Time:	2010-230T00:00	Stop Time:	2010-231T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010231_01

Start Time:	2010-231T00:00	Stop Time:	2010-232T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010232_01

Start Time:	2010-232T00:00	Stop Time:	2010-233T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010233_01

Start Time:	2010-233T00:00	Stop Time:	2010-234T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010234_01

Start Time:	2010-234T00:00	Stop Time:	2010-235T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010235_01

Start Time:	2010-235T00:00	Stop Time:	2010-236T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010236_01

Start Time:	2010-236T00:00	Stop Time:	2010-237T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010237_01

Start Time:	2010-237T00:00	Stop Time:	2010-238T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010238_01

Start Time:	2010-238T00:00	Stop Time:	2010-239T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010239_01

Start Time:	2010-239T00:00	Stop Time:	2010-240T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010240_01

Start Time:	2010-240T00:00	Stop Time:	2010-241T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010241_01

Start Time:	2010-241T00:00	Stop Time:	2010-242T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010242_01

Start Time:	2010-242T00:00	Stop Time:	2010-243T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010243_01

Start Time:	2010-243T00:00	Stop Time:	2010-244T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010244_01

Start Time:	2010-244T00:00	Stop Time:	2010-245T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010245_01

Start Time:	2010-245T00:00	Stop Time:	2010-246T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010246_01

Start Time:	2010-246T00:00	Stop Time:	2010-247T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010247_01

Start Time:	2010-247T00:00	Stop Time:	2010-248T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010248_01

Start Time:	2010-248T00:00	Stop Time:	2010-249T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010249_01

Start Time:	2010-249T00:00	Stop Time:	2010-250T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010250_01

Start Time:	2010-250T00:00	Stop Time:	2010-251T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010251_01

Start Time:	2010-251T00:00	Stop Time:	2010-252T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010252_01

Start Time:	2010-252T00:00	Stop Time:	2010-253T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010253_01

Start Time:	2010-253T00:00	Stop Time:	2010-254T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010254_01

Start Time:	2010-254T00:00	Stop Time:	2010-255T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010255_01

Start Time:	2010-255T00:00	Stop Time:	2010-256T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010256_01

Start Time:	2010-256T00:00	Stop Time:	2010-257T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010257_01

Start Time:	2010-257T00:00	Stop Time:	2010-258T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010258_01

Start Time:	2010-258T00:00	Stop Time:	2010-259T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010259_01

Start Time:	2010-259T00:00	Stop Time:	2010-260T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010260_01

Start Time:	2010-260T00:00	Stop Time:	2010-261T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010261_01

Start Time:	2010-261T00:00	Stop Time:	2010-262T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010262_01

Start Time:	2010-262T00:00	Stop Time:	2010-263T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010263_01

Start Time:	2010-263T00:00	Stop Time:	2010-264T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010264_01

Start Time:	2010-264T00:00	Stop Time:	2010-265T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010265_01

Start Time:	2010-265T00:00	Stop Time:	2010-266T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010266_01

Start Time:	2010-266T00:00	Stop Time:	2010-267T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010267_01

Start Time:	2010-267T00:00	Stop Time:	2010-268T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010268_01

Start Time:	2010-268T00:00	Stop Time:	2010-269T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010269_01

Start Time:	2010-269T00:00	Stop Time:	2010-270T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010270_01

Start Time:	2010-270T00:00	Stop Time:	2010-271T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010271_01

Start Time:	2010-271T00:00	Stop Time:	2010-272T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010272_01

Start Time:	2010-272T00:00	Stop Time:	2010-273T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010273_01

Start Time:	2010-273T00:00	Stop Time:	2010-274T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010274_01

Start Time:	2010-274T00:00	Stop Time:	2010-275T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010275_01

Start Time:	2010-275T00:00	Stop Time:	2010-276T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010276_01

Start Time:	2010-276T00:00	Stop Time:	2010-277T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010277_01

Start Time:	2010-277T00:00	Stop Time:	2010-278T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010278_01

Start Time:	2010-278T00:00	Stop Time:	2010-279T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010279_01

Start Time:	2010-279T00:00	Stop Time:	2010-280T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010280_01

Start Time:	2010-280T00:00	Stop Time:	2010-281T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010281_01

Start Time:	2010-281T00:00	Stop Time:	2010-282T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010282_01

Start Time:	2010-282T00:00	Stop Time:	2010-283T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010283_01

Start Time:	2010-283T00:00	Stop Time:	2010-284T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010284_01

Start Time:	2010-284T00:00	Stop Time:	2010-285T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010285_01

Start Time:	2010-285T00:00	Stop Time:	2010-286T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010286_01

Start Time:	2010-286T00:00	Stop Time:	2010-287T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010287_01

Start Time:	2010-287T00:00	Stop Time:	2010-288T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010288_01

Start Time:	2010-288T00:00	Stop Time:	2010-289T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010289_01

Start Time:	2010-289T00:00	Stop Time:	2010-290T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010290_01

Start Time:	2010-290T00:00	Stop Time:	2010-291T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010291_01

Start Time:	2010-291T00:00	Stop Time:	2010-292T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010292_01

Start Time:	2010-292T00:00	Stop Time:	2010-293T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010293_01

Start Time:	2010-293T00:00	Stop Time:	2010-294T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010294_01

Start Time:	2010-294T00:00	Stop Time:	2010-295T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010295_01

Start Time:	2010-295T00:00	Stop Time:	2010-296T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010296_01

Start Time:	2010-296T00:00	Stop Time:	2010-297T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010297_01

Start Time:	2010-297T00:00	Stop Time:	2010-298T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010298_01

Start Time:	2010-298T00:00	Stop Time:	2010-299T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010299_01

Start Time:	2010-299T00:00	Stop Time:	2010-300T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010300_01

Start Time:	2010-300T00:00	Stop Time:	2010-301T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010301_01

Start Time:	2010-301T00:00	Stop Time:	2010-302T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010302_01

Start Time:	2010-302T00:00	Stop Time:	2010-303T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010303_01

Start Time:	2010-303T00:00	Stop Time:	2010-304T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010304_01

Start Time:	2010-304T00:00	Stop Time:	2010-305T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010305_01

Start Time:	2010-305T00:00	Stop Time:	2010-306T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010306_01

Start Time:	2010-306T00:00	Stop Time:	2010-307T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010319_01

Start Time:	2010-319T00:00	Stop Time:	2010-320T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010320_01

Start Time:	2010-320T00:00	Stop Time:	2010-321T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010321_01

Start Time:	2010-321T00:00	Stop Time:	2010-322T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010322_01

Start Time:	2010-322T00:00	Stop Time:	2010-323T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010323_01

Start Time:	2010-323T00:00	Stop Time:	2010-324T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010324_01

Start Time:	2010-324T00:00	Stop Time:	2010-325T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010325_01

Start Time:	2010-325T00:00	Stop Time:	2010-326T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010326_01

Start Time:	2010-326T00:00	Stop Time:	2010-327T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010327_01

Start Time:	2010-327T00:00	Stop Time:	2010-328T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010328_01

Start Time:	2010-328T00:00	Stop Time:	2010-329T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010329_01

Start Time:	2010-329T00:00	Stop Time:	2010-330T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010330_01

Start Time:	2010-330T00:00	Stop Time:	2010-331T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010331_01

Start Time:	2010-331T00:00	Stop Time:	2010-332T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010332_01

Start Time:	2010-332T00:00	Stop Time:	2010-333T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010333_01

Start Time:	2010-333T00:00	Stop Time:	2010-334T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010334_01

Start Time:	2010-334T00:00	Stop Time:	2010-335T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010335_01

Start Time:	2010-335T00:00	Stop Time:	2010-336T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010336_01

Start Time:	2010-336T00:00	Stop Time:	2010-337T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010337_01

Start Time:	2010-337T00:00	Stop Time:	2010-338T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010339_01

Start Time:	2010-339T00:00	Stop Time:	2010-340T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010340_01

Start Time:	2010-340T00:00	Stop Time:	2010-341T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010341_01

Start Time:	2010-341T00:00	Stop Time:	2010-342T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010342_01

Start Time:	2010-342T00:00	Stop Time:	2010-343T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010343_01

Start Time:	2010-343T00:00	Stop Time:	2010-344T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010344_01

Start Time:	2010-344T00:00	Stop Time:	2010-345T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010345_01

Start Time:	2010-345T00:00	Stop Time:	2010-346T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010346_01

Start Time:	2010-346T00:00	Stop Time:	2010-347T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010347_01

Start Time:	2010-347T00:00	Stop Time:	2010-348T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010348_01

Start Time:	2010-348T00:00	Stop Time:	2010-349T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010349_01

Start Time:	2010-349T00:00	Stop Time:	2010-350T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010350_01

Start Time:	2010-350T00:00	Stop Time:	2010-351T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010351_01

Start Time:	2010-351T00:00	Stop Time:	2010-352T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010352_01

Start Time:	2010-352T00:00	Stop Time:	2010-353T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010353_01

Start Time:	2010-353T00:00	Stop Time:	2010-354T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010354_01

Start Time:	2010-354T00:00	Stop Time:	2010-355T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010355_01

Start Time:	2010-355T00:00	Stop Time:	2010-356T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010356_01

Start Time:	2010-356T00:00	Stop Time:	2010-357T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010357_01

Start Time:	2010-357T00:00	Stop Time:	2010-358T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010358_01

Start Time:	2010-358T00:00	Stop Time:	2010-359T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010359_01

Start Time:	2010-359T00:00	Stop Time:	2010-360T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010360_01

Start Time:	2010-360T00:00	Stop Time:	2010-361T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010361_01

Start Time:	2010-361T00:00	Stop Time:	2010-362T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010362_01

Start Time:	2010-362T00:00	Stop Time:	2010-363T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010363_01

Start Time:	2010-363T00:00	Stop Time:	2010-364T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010364_01

Start Time:	2010-364T00:00	Stop Time:	2010-365T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

LPHAAVG0_1MIN_2010365_01

Start Time:	2010-365T00:00	Stop Time:	2011-001T00:00
The data columns contain 1 minute averages of LEMMS PHA data. The data are averaged by first defining fixed one minute intervals throughout the day and then averaging any data points that fall in the intervals. If an interval contains no data, it is still listed in the file, but all data intensity values will be fill. The fill value for data in this file is -1.0E38. These data are background subtracted, and thus occasionally there will be negative values when the count rate falls below the background level. Also, the uncertainties are based on the counting statistics, and thus because of the background subtraction, the uncertainties can be larger than the data value. The background levels change over time and each channel's background level as a function of time in counts/sec is listed in the MIMI calibration file (described in the MIMI Data User Guide, the SIS for this dataset, and also in SIS for the uncalibrated MIMI data). There are three types of channels included in these averages: the A channels, the E channels and the F1 channels. The A channels measure ions, mostly protons. The E and F1 channels measure electrons. The MIMI instrument paper describes these channels, as does the MIMI Data User Guide. For the A channels, channel indices 8 through 62 are present (energies of 26-758 keV). For the E channels, indices 15 to 62 (20-410 keV), and for F1, 26 through 59 (206-1717 keV). Note that a subset of the available PHA channels are typically used for science analysis, and only these channels are plotted here. The dataset catalog file details the reasons for this. Essentially, the efficiencies are unknown or uncertain for omitted channels. The file header and leading columns of the file are present to make the format consistent with other MIMI data in the PDS. Note that much of the values for the leading columns are -1, indicating that they do not have useful values, but their presence allows this file to be parsed by the same code that reads other MIMI PDS data. The first column is always the string 'sci', the next column is a UTC string, and then these prefix columns have no data in them but are just there to preserve the format: UTC SCLOCK Start_Ephemeris_s End_Ephemeris_s Spin_Counter Sector Start_Sector_Sclock_major Subsector Microsectors_Covered Spin_Period_s Staring Sensor_Bitrate Just before the data columns are three columns giving the position of the Cassini spacecraft relavtive to Saturn in the SZS frame. The position is given for the middle of the time interval. The units are Saturn radii (60268 km) and the SZS frame is defined as: +Z is Saturn spin axis, +Y is +Z cross the Saturn-Sun line, and +X is +Y cross +Z.

ICON LEGEND
For links to data holdings various icons are used to represent services or actions you can take. Those icons are:
	Order the volume (CD-ROM/DVD) containing the listed data. The volume will be mailed to you.	The volume (CD-ROM/DVD) contains some errors which are documented in an errata log.
	Launch a custom web browser for the resource.	Launch a map based browser for the resource.
	Toggle viewing into brief mode (shorter descriptions are displayed).	Toggle viewing into expanded mode (longer descriptions are displayed).
	Download the volume containing the listed data.

NEW RELEASES

More.....

PDS RESOURCES

Archive Planning Guide
      Individuals
      Missions
Data Dictionary Search
      Lookup Tool
      Document
PDS4 Standards Documents
PDS Subscription Service

PDS3 Standards

OTHER RESOURCES

ADS Search
Science Data Licenses

	Search For:

	in