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VOYAGER 2 SAT LOW ENERGY CHARGED PARTICLE CALIB. 15MIN
THIS DATA SET CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 2 WHILE THE SPACECRAFT WAS IN THE VICINITY OF SATURN. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. THUS, THE FULL ANGULAR ANISOTROPY INFORMATION IS PRESERVED WITH THIS DATA. THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET. Also included with this data are one standard deviation statistical uncertainties for the directional data (sectors 1 through 8) expressed as a percent. Unknown values are generally coded as su
VOYAGER 2 SATURN PLASMA DERIVED ION MOMENTS 96 SEC
THIS DATA SET CONTAINS ESTIMATES OF THE ION MOMENT DENSITY IN THE PLS VOLTAGE RANGE (10-5950 EV/Q) AT SATURN DURING THE VOYAGER 2 ENCOUNTER. RIGID COROTATION IS ASSUMED, WHICH LEADS TO AN UNDERESTIMATE OF THE DENSITY IN SOME REGIONS, AS DOES THE USE OF AN ACCEPTANCE AREA RELEVANT FOR A COLD BEAM FOR PLASMA WHICH IS TRANSONIC IN SOME REGIONS. DENSITIES MAY BE UNDERESTIMATED BY A FACTOR OF 2-3 IN THE INNER MAGNETOSPHERE, SO THIS DATA SET SHOULD BE USED PRIMARILY FOR STUDIES USING VARIATIONS IN PLASMA DENSITY. THE FIT DENSITIES GIVE A BETTER ESTIMATE OF THE ABSOLUTE DENSITY.
VOYAGER 1 SATURN MAGNETOMETER RESAMPLED DATA 48.0 SEC
This data set includes Voyager 1 Saturn encounter magnetometer data that have been resampled at a 48.0 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus Saturn Longitude System (-SLS). All of the magnetic field data are calibrated (see the instrument calibration description for more details). The SLS coordinate system is defined in Desch and Kaiser, 1981 and the reference documents for this dataset are: Ness et al, 1982 Acuna,Connerney,and Ness, 1983 Connerney,Acuna,and Ness, 1983 Behannon,Lepping,and Ness, 1983
VOYAGER 1 SATURN MAGNETOMETER RESAMPLED DATA 9.60 SEC
This data set includes Voyager 1 Saturn encounter magnetometer data that have been resampled at a 9.6 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus Saturn Longitude System (-SLS). All of the magnetic field data are calibrated (see the instrument calibration description for more details). The SLS coordinate system is defined in Desch and Kaiser, 1981 and the reference documents for this dataset are: Ness et al, 1982 Acuna,Connerney,and Ness, 1983 Connerney,Acuna,and Ness, 1983 Behannon,Lepping,and Ness, 1983
VOYAGER 1&2 JUPITER BRIGHTNESS NORTH/SOUTH MAP SET V1.0
This data set contains Voyager 1 and 2 measurements of the brightness of Jupiter at H Lyman alpha and in the H2 Lyman and Werner bands shortward of H Lyman alpha. Pointing has been corrected by the C-Smithing process, and these data were derived from the pre-encounter North-South Map sequences. In this sequence, the UVS field of view was located near the central meridian of the planet. The field of view stepped slowly from north to south, and then rapidly repositioned to the north. These scans were repeated until all Jovian longitudes had been sampled. Coverage in longitude was not continuous in time. Rather, some longitude ranges were covered on the preceding or following rotation of Jupiter.
VOYAGER 1 DAILY POSITION V1.0
This dataset contains Voyager 1 trajectory data from the interplanetary cruise sampled daily in Solar Ecliptic and Heliographic coordinates.
Voyager 1 Saturn CRS D1/D2 Averaged 192 Second Counting Rate Data Bundle
This bundle contains the counting rate data from detectors D1 and D2 in the Cosmic Ray System (CRS) electron telescope (TET) on Voyager 1 during the Saturn encounter. The D1 detector nominally responds to electrons with kinetic energies above approximately 1 MeV, and the D2 detector, above approximately 2.5 MeV.
VOYAGER 1 SAT LOW ENERGY CHARGED PARTICLE CALIB. 15MIN
THIS DATA SET CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 1 WHILE THE SPACECRAFT WAS IN THE VICINITY OF SATURN. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. THUS, THE FULL ANGULAR ANISOTROPY INFORMATION IS PRESERVED WITH THIS DATA. THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET. Also included with this data are one standard deviation statistical uncertainties for the directional data (sectors 1 through 8) expressed as a percent. Unknown values are generally coded as su
VOYAGER 1 JUPITER MAGNETOMETER RESAMPLED DATA 9.60 SEC
This data set includes Voyager 1 Jupiter encounter magnetometer data that have been resampled at a 9.6 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus System III. All of the magnetic field data are calibrated (see the instrument calibration description for more details). The Jupiter System III coordinate system is defined in Dessler 1983 and the reference documents for this dataset are: Ness et al, 1979 Lepping et al, 1981 Connerney,Acuna,Ness, 1981 Behannon,Burlaga,Ness, 1981
VOYAGER 2 TRITON RADIO OCCULTATION REDUCED DATA V1.0
This data set consists of several tables and supporting documentation from final analysis of the Voyager 2 radio occultation by Triton. The data set is based on a Ph.D. dissertation by Eric M. Gurrola of Stanford University [GURROLA1995]. The tabulated data were derived from raw radio science observations, which are being archived separately. General principles for conducting these types of experiments have been described by [TYLER1987] results of the Triton analysis were published by [TYLERETAL1989].
VOYAGER 2 SAT LOW ENERGY CHARGED PARTICLE CALIB. BR 15MIN
THIS BROWSE DATA CONSISTS OF RESAMPLED DATA FROM THE LOW ENERGY CHARGED PARTICLE (LECP) EXPERIMENT ON VOYAGER 2 WHILE THE SPACECRAFT WAS IN THE VICINITY OF SATURN. THIS INSTRUMENT MEASURES THE INTENSITIES OF IN-SITU CHARGED PARTICLES (>26 KEV ELECTRONS AND >30 KEV IONS) WITH VARIOUS LEVELS OF DISCRIMINATION BASED ON ENERGY, MASS SPECIES, AND ANGULAR ARRIVAL DIRECTION. A SUBSET OF ALMOST 100 LECP CHANNELS ARE INCLUDED WITH THIS DATA SET. THE LECP DATA ARE GLOBALLY CALIBRATED TO THE EXTENT POSSIBLE (SEE BELOW) AND THEY ARE TIME AVERAGED TO ABOUT 15 MINUTE TIME INTERVALS WITH THE EXACT BEGINNING AND ENDING TIMES FOR THOSE INTERVALS MATCHING THE LECP INSTRUMENTAL CYCLE PERIODS (THE ANGULAR SCANNING PERIODS). THE LECP INSTUMENT HAS A ROTATING HEAD FOR OBTAINING ANGULAR ANISOTROPY MEASUREMENTS OF THE MEDIUM ENERGY CHARGED PARTICLES THAT IT MEASURES. THE CYCLE TIME FOR THE ROTATION IF VARIABLE, BUT DURING ENCOUNTERS IT IS ALWAYS FASTER THAN 15 MINUTES. FOR THIS BROWSE DATA SET ONLY SCAN AVERAGE DATA IS GIVEN (NO ANGULAR INFORMATION). THE DATA IS IN THE FORM OF 'RATE' DATA WHICH HAS NOT BEEN CONVERTED TO THE USUAL PHYSICAL UNITS. THE REASON IS THAT SUCH A CONVERSION WOULD DEPEND ON UNCERTAIN DETERMINATIONS SUCH AS THE MASS SPECIES OF THE PARTICLES AND THE LEVEL OF BACKGROUND. BOTH MASS SPECIES AND BACKGROUND ARE GENERALLY DETERMINED FROM CONTEXT DURING THE STUDY OF PARTICULAR REGIONS. TO CONVERT 'RATE' TO 'INTENSITY' FOR A PARTICULAR CHANNEL ONE PERFORMS THE FOLLOWING TASKS: 1) DECIDE ON THE LEVEL OF BACKGROUND CONTAMINATION AND SUBTRACT THAT OFF THE GIVEN RATE LEVEL. BACKGROUND IS TO BE DETERMINED FROM CONTEXT AND FROM MAKING USE OF SECTOR 8 RATES (SECTOR 8 HAS A 2 mm AL SHIELD COVERING IT). 2) DIVIDE THE BACKGROUND CORRECTED RATE BY THE CHANNEL GEOMETRIC FACTOR AND BY THE ENERGY BANDPASS OF THE CHANNEL. THE GEOMETRIC FACTOR IS FOUND IN ENTRY 'channel_geometric_ factor' AS ASSOCIATED WITH EACH CHANNEL 'channel_id'. TO DETERMINE THE ENERGY BANDPASS, ONE MUST JUDGE THE MASS SPECIES OF THE OF THE DETECTED PARTICLES (FOR IONS BUT NOT FOR ELECTRONS). THE ENERGY BAND PASSES ARE GIVEN IN ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPENERGY', AND ARE GIVEN IN THE FORM 'ENERGY/NUCLEON'. FOR CHANNELS THAT BEGIN THEIR NAMES WITH THE DESIGNATIONS 'CH' THESE BANDPASSES CAN BE USED ON MASS SPECIES THAT ARE ACCEPTED INTO THAT CHANNEL (SEE ENTRIES 'minimum_instrument_parameter' and 'maximum_instrument_ parameter' IN TABLE 'FPLECPCHANZ', WHICH GIVE THE MINIMUM AND MAXIMUM 'Z' VALUE ACCEPTED -- THESE ENTRIES ARE BLANK FOR ELECTRON CHANNELS). FOR OTHER CHANNELS THE GIVEN BANDPASS REFERS ONLY TO THE LOWEST 'Z' VALUE ACCEPTED. THE BANDPASSES FOR OTHER 'Z' VALUES ARE NOT ALL KNOWN, BUT SOME ARE GIVEN IN THE LITERATURE (E.G. KRIMIGIS ET AL., 1979). THE FINAL PRODUCT OF THESE INSTRUCTIONS WILL BE THE PARTICLE INTENSITY WITH THE UNITS: COUNTS/(CM**2.STR.SEC.KEV). SOME CHANNELS ARE SUBJECT TO SERIOUS CONTAMINATIONS, AND MANY OF THESE CONTAMINATIONS CANNOT BE REMOVED EXCEPT WITH A REGION-BY-REGION ANALYSIS, WHICH HAS NOT BEEN DONE FOR THIS DATA. THUS, TO USE THIS DATA IT IS ABSOLUTELY VITAL THAT THE CONTAMINATION TYPES ('contamination_id' , 'contamination_desc') AND THE LEVELS OF CONTAMINATION ('data_quality_id' CORRESPONDING TO THE DEFINITIONS 'data_quality_desc') BE CAREFULLY EXAMINED FOR ALL REGIONS OF STUDY. A DEAD TIME CORRECTION PROCEDURE HAS BEEN APPLIED IN AN ATTEMPT TO CORRECT THE LINEAR EFFECTS OF DETECTOR OVERDRIVE (PULSE-PILEUP). THIS PROCEDURE DOES NOT FIX SEVERELY OVERDRIVEN DETECTORS. A PROCEDURE IS AVAILABLE FOR CORRECTING VOYAGER 2 LECP ELECTRON CONTAMINATION OF LOW ENERGY ION CHANNELS, BUT ITS EFFECTIVENESS HAS BEEN EVALUATED ONLY FOR THE URANUS DATA SET. THUS, CORRECTIONS HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET.
VOYAGER 1 SATURN PLASMA DERIVED ELECTRON PARAMETERS 96 SEC
THIS DATA SET CONTAINS ELECTRON P ARAMETERS IN THE PLS ENERGY RANGE (10-5950 EV) AT SATURN DURING THE VOYAGER 1 ENCOUNTER. PARAMETERS ARE CALCULATED IN SEVERAL WAYS. TOTAL MOMENT DENSITY AND TEMPERATURE ARE GIVEN. EACH ELECTRON SPECTRUM IS ALSO FIT WITH A THERMAL COMPONENT AND 1-3 HOT COMPONENTS DEPENDING ON HOW MANY MAXWELLIANS ARE NEEDED TO FIT THE ENTIRE DISTRIBUTION. THE MOMENT DENSITY AND TEMPERATURE OF THE HOT COMPONENT IS CALCULATED AFTER THE THERMAL COMPONENT IS SUBTRACTED FROM THE SPECTRUM. THE CHI-SQUARE VALUE FOR EACH FIT IS GIVEN. THE SPACECRAFT CHARGE IS NOT CALCULATED CONSISTENTLY, AND MAY RESULT IN FACTOR OF 2-3 ERRORS IN THE THERMAL ELECTRON DENSITY. DATA IS UNRELIABLE INSIDE 6 RS AND IN THE OCCULTATION REGIONS. A COMPLETE DESCRIPTION OF THIS DATA SET IS IN SITTLERETAL. (1983)
VOYAGER 1 SATURN POSITION RESAMPLED DATA 48.0 SECONDS
This data set includes Voyager 1 Saturn encounter position data that have been generated at a 48.0 second sample rate using the NAIF SPICE kernals. The data set is composed of 4 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) r - this column contains the radial distance from Saturn in Rs = 60330 km, 3) longitude - this column contains the east longitude of the spacecraft in degrees, 4) latitude - this column contains the latitude of the spacecraft in degrees. Position data is given in Minus Saturn Longitude System (kronographic) coordinates.
VOYAGER 1 SATURN MAGNETOMETER RESAMPLED DATA 1.92 SEC
This data set includes Voyager 1 Saturn encounter magnetometer data that have been resampled at a 1.92 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus Saturn Longitude System (-SLS). All of the magnetic field data are calibrated (see the instrument calibration description for more details). The SLS coordinate system is defined in Desch and Kaiser, 1981 and the reference documents for this dataset are: Ness et al, 1982 Acuna,Connerney,and Ness, 1983 Connerney,Acuna,and Ness, 1983 Behannon,Lepping,and Ness, 1983
VOYAGER 1 SATURN EGRESS RADIO OCCULTATION RAW DATA V1.0
This data set consists of raw data collected during the Saturn egress radio occultation of Voyager 1 on 13 November 1980 plus ancillary files that might be useful in analysis of those data. The raw data are sampled voltage outputs from receivers tuned to the Voyager carrier frequencies at both S-band and X-band during the occultation. The data have been reduced to give profiles of temperature and pressure as a function of height in the atmosphere, to infer magnetic field orientations in the upper ionosphere, and to determine the distribution of particles and particle properties in the ring system.
VOYAGER 2 SOLAR WIND MAGNETIC FIELD HGCOORDS HOUR AVGS V1.0
This dataset contains Voyager 2 magnetometer data from the interplanetary cruise averaged to 1 hour samples in Heliographic coordinates.
VOYAGER 2 SATURN MAGNETOMETER RESAMPLED DATA 9.60 SEC
This data set includes Voyager 2 Saturn encounter magnetometer data that have been resampled at a 9.6 second sample rate. The data set is composed of 6 columns: 1) ctime - this column contains the data acquisition time. The time is always output in the ISO standard spacecraft event time format (yyyy-mm-dd-Thh:mm:ss.sss) but is stored internally in Cline time which is measured in seconds after 00:00:00.000 Jan 01, 1966, 2) br - this column contains the radial component of the magnetic field, 3) bphi - this column contains the phi component of the magnetic field, 4) btheta - this column contains the theta component of the magnetic field, 5) bmag - this column contains the magnitude of the magnetic field, 6) flag - a flag value that indicates either software error or spacecraft hardware interference reduced confidence in this record (flag value of 1 is bad , 0 is good or unchecked). All magnetic field observations are measured in nanoTeslas. The coordinate system for this dataset is Minus Saturn Longitude System (-SLS). All of the magnetic field data are calibrated (see the instrument calibration description for more details). The SLS coordinate system is defined in Desch and Kaiser, 1981 and the reference documents for this dataset are: Ness et al, 1982 Acuna,Connerney,and Ness, 1983 Connerney,Acuna,and Ness, 1983 Behannon,Lepping,and Ness, 1983
VOYAGER 1 SATURN PLASMA DERIVED ELECTRON PARAMETERS 96 SEC
THIS DATA SET CONTAINS ELECTRON PARAMETERS IN THE PLS ENERGY RANGE (10-5950 EV) AT SATURN DURING THE VOYAGER 1 ENCOUNTER. PARAMETERS ARE CALCULATED IN SEVERAL WAYS. TOTAL MOMENT DENSITY AND TEMPERATURE ARE GIVEN. EACH ELECTRON SPECTRUM IS ALSO FIT WITH A THERMAL COMPONENT AND 1-3 HOT COMPONENTS DEPENDING ON HOW MANY MAXWELLIANS ARE NEEDED TO FIT THE ENTIRE DISTRIBUTION. THE MOMENT DENSITY AND TEMPERATURE OF THE HOT COMPONENT IS CALCULATED AFTER THE THERMAL COMPONENT IS SUBTRACTED FROM THE SPECTRUM. THE CHI-SQUARE VALUE FOR EACH FIT IS GIVEN. THE SPACECRAFT CHARGE IS NOT TAKEN INTO ACCOUNT, AND MAY RESULT IN FACTOR OF 2-3 ERRORS IN THE THERMAL ELECTRON DENSITY. DATA IS UNRELIABLE INSIDE 6 RS AND IN THE OCCULTATION REGIONS. A COMPLETE DESCRIPTION OF THIS DATA SET IS IN SITTLER ET AL. (1983). DATA FORMAT: THE DATA SET IS IN ASC FORMAT AND CAN BE READ USING THE FOLLOWING FORTRAN STATEMENT:\n
VOYAGER 2 SAT PLASMA WAVE SPECTROMETER RESAMP SPEC 48.0SEC
This data set consists of 48-second calibrated, averaged wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Saturnian magnetosphere. For each 48-second interval, a geometric average field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kilo- Hertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of averages is the beginning of the averating interval. Averages are stored in units of volt/meter. During data gaps where complete 48-second intervals are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Scarf et al. [1982] and a complete instrument description can be found in Scarf and Gurnett [1977].
VOYAGER 1 SOLAR WIND MAGNETIC FIELD HGCOORDS 48SEC AVG V1.0
This dataset contains Voyager 1 magnetometer data from the interplanetary cruise averaged to 48 second samples in Heliographic coordinates.
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