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VOYAGER 2 JUPITER MAGNETOMETER RESAMPLED DATA 1.92 SEC

This data set includes Voyager 2 Jupiter 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 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, 1979A Lepping et al, 1981 Connerney,Acuna,Ness, 1981 Behannon,Burlaga,Ness, 1981

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 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 PWS electric field waveform in CDF files

The Voyager 2 Plasma Wave Subsystem (PWS) electric field waveform data set contains all available uncalibrated full resolution 4-bit measurements for the entire mission. The PWS waveform receiver samples the voltage on the 10 m electric antennas at the rate of 28800 samples per second through a 40 Hz to 12 kHz bandpass filter, utilizing an automatic gain control. However, gain information is not returned in telemetry so absolute calibration cannot be done directly. The waveform may be used to identify features such as dust impacts in the time domain or a power spectrum may be derived to show relative amplitudes of spectral elements in the frequency domain.

VOYAGER 2 JUP 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 Jovian 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 Gurnett et al. [1979] and a complete instrument description can be found in Scarf and Gurnett [1977].

VOYAGER 2 SATURN MAGNETOMETER RESAMPLED DATA 1.92 SEC

This data set includes Voyager 2 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 2 SATURN PLASMA DERIVED ION FITS 96 SEC

THIS DATA SET CONTAINS THE ION PARAMETERS IN THE PLS VOLTAGE RANGE (10-5950 EV/Q) WITH FORMAL 1 SIGMA ERRORS OBTAINED FROM VOYAGER 2 DATA AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS TO OBTAIN PLASMA DENSITIES, TEMPERATURES, AND VELOCITY. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE NITROGEN OUTSIDE OF 14 RS AND OXYGEN ELSEWHERE. OUTSIDE L=10-12 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. THE VALUES FOR POSITION AND MAGNETIC FIELD GIVEN IN THE DATA SET ARE ONLY APPROXIMATE AND SHOULD NOT BE USED FOR PUBLICATION. PARAMETERS WHICH ARE IDENTICALLY 0 AND HAVE UNCERTAINTIES OF 0 WERE NOT FIT DUE TO INSUFFICIENT DATA THESE NUMBERS ARE THUS NOT REAL VALUES. A COMPLETE DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: EACH DATA RECORD CONSISTS OF 5+2N LINES, WHERE N IS THE NUMBER OF IONS FIT. LINE 1: S (A1, INDICATES THE START OF A NEW FIT) TIME OF SPECTRUM SPACECRAFT LOCATION BRHO,BPHI,BZ(3F7.3) MONTHDAYYEAR(I7) ROUTINE USED INCORPORATING THE FULL RESPONSE FUNCTION OF THE INSTRUMENT FOR L MODES DATA): CHI-SQUARE FROM FIT (E7.3) (I2): LINES 2-5 TELL WHICH CHANNELS WERE FIT: CUP IDENTIFIER (A,B,C,D) (A1) AND ENDING CHANNEL OF EACH SET (2-20I3): LINE 6 FOR IONS: F (LINE IDENTIFIER) (A1) (I1)ION MASS, CHARGE (I3,I2) (6E10.3), WHERE THE X* VARIABLES ARE FORMAL 1 SIGMA UNCERTAINTIES: LINE 7 IDENTIFIER), ION SPECIES NUMBER (A1, I1) VZ,XVZ,WPAR,XWPAR,WPER, XWPER (6E10.3). LINES 6 AND 7 REPEAT ONCE FOR EACH ION SPECIES. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. V'S ARE VELOCITIES IN KM/S, W'S THERMAL SPEEDS IN KM/S, AND DEN'S DENSITIESIN CM-3. VALUES OF B AND POSITION INFORMATION MAY BE UNRELIABLE AND SHOULD BE VERIFIED BEFORE USE. 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 RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

VOYAGER 1 JUPITER PLASMA DERIVED ION MOMENTS 96 SEC

THIS DATA SET CONTAINS THE BEST ESTIMATES OF THE TOTAL ION DENSITY AT JUPITER DURING THE VOYAGER 1 ENCOUNTER IN THE PLS VOLTAGE RANGE (10-5950 EV/Q). IT IS CALCULATED USING THE METHOD OF MCNUTT ET AL. (1981) WHICH TO FIRST ORDER CONSISTS OF TAKING THE TOTAL MEASURED CURRENT AND DIVIDING BY THE COLLECTOR AREA AND PLASMA BULK VELOCITY. THIS METHOD IS ONLY ACCURATE FOR HIGH MACH NUMBER FLOWS DIRECTLY INTO THE DETECTOR, AND MAY RESULT IN UNDERESTIMATES OF THE TOTAL DENSITY OF A FACTOR OF 2 IN THE OUTER MAGNETOSPHERE. THUS ABSOLUTE DENSITIES SHOULD BE TREATED WITH CAUTION, BUT DENSITY VARIATIONS IN THE DATA SET CAN BE TRUSTED. THE LOW RESOLUTION MODE DENSITY IS USED BEFORE 1979 63 1300, AFTER THIS THE LARGER OF THE HIGH AND LOW RESOLUTION MODE DENSITIES IN A 96 SEC PERIOD IS USED SINCE THE L-MODE SPECTRA OFTEN ARE SATURATED. COROTATION IS ASSUMED INSIDE L=17.5, AND A CONSTANT VELOCITY COMPONENT OF 200 KM/S INTO THE D CUP IS USED OUTSIDE OF THIS. THESE ARE THE DENSITIES GIVEN IN THE MCNUTT ET AL. (1981) PAPER CORRECTED BY A FACTOR OF 1.209 (.9617) FOR DENSITIES OBTAINED FROM THE SIDE (MAIN) SENSOR. THIS CORRECTION IS DUE TO A BETTER CALCULATION OF THE EFFECTIVE AREA OF THE SENSORS. DATA FORMAT: COLUMNS 1-6 ARE TIME (YEAR, DAY, HOUR, MIN, SEC, MSEC) COLUMN 7 IS THE MOMENT DENSITY IN CM-3. EACH ROW HAS FORMAT (6I4, E12.3). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. 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 MCNUTT ET AL. (1981) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

Voyager 1 hourly merged magnetic field and plasma data

This is an hourly resolution, merged magnetic field and plasma data set created at NSSDC for COHOWeb. Magnetic field vectors and plasma flow direction angles are given in RTN coordinates. Spacecraft position data are given in Heliographic inertial (HGI coordinates).

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Voyager 1 PWS electric field waveform in CDF files

The Voyager 1 Plasma Wave Subsystem (PWS) electric field waveform data set contains all available uncalibrated full resolution 4-bit measurements for the entire mission. The PWS waveform receiver samples the voltage on the 10 m electric antennas at the rate of 28800 samples per second through a 40 Hz to 12 kHz bandpass filter, utilizing an automatic gain control. However, gain information is not returned in telemetry so absolute calibration cannot be done directly. The waveform may be used to identify features such as dust impacts in the time domain or a power spectrum may be derived to show relative amplitudes of spectral elements in the frequency domain.

VOYAGER 1&2 SATURN IRIS DERIVED NORTH/SOUTH PARAMETERS V1.0

The data set contains Saturn atmospheric parameters derived from spectra obtained with the Voyager infrared interferometer spectrometer (IRIS). The data set is ordered by time as measured by the Flight Data System Count (FDSC). This represents the data frame number modulo 60. Also included in the data set are information on pointing and associated geometry of the measurements and brightness temperatures obtained from measured radiances at selected wavenumbers.

Voyager 2 Plasma Spectrometer (PLS) Faraday Cups A-D High Energy Resolution Current Ion Spectra, M Mode, for Proton Energies from 10 eV to 5950 eV, 96 s Data

These Ion Current Spectra in the Jovian Magnetosphere are from the Plasma Spectrometer (PLS) Instrument on Voyager 2 during July 1979 Flyby of Jupiter. The Instrument has four Faraday Cups A, B, C, and D, the Electron Data come only from Faraday Cup D. The Data are specified in Terms of Current per Faraday Cup in femto-amperes (10^-15 A equals 1 fA) versus Channel Number and Energy (eV). This Data Set is for the PLS M Mode covering Proton (H+ Ion) Energies from 10 eV to 5950 eV at High Energy Resolution in 128 logarithmic Energy Channels. The PLS Instrument samples only one Mode of Electron (E1, E2) or Ion (L, M) Spectra in each Time Interval, so the M Mode Data are not continuous but consecutive with the other Modes in Time. Reference: Bridge, H.S., Belcher, J.W., Butler, R.J., Lazarus, A.J., Mavretic, A.M., Sullivan, J.D., Siscoe, G.L., and V.M. Vasyliunas, The Plasma Experiment on the 1977 Voyager Mission, Space Sci. Rev., 21, 259-287, 1977.

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Voyager 2 Plasma Wave Subsystem (PWS), 16-Channel Spectrum Analyzer Data

This data set contains Voyager 2 Plasma Wave Subsystem (PWS) electric field 16-channel Spectrum Analyzer (SA) data for the entire mission in calibrated CDF files. As of the release date new data are accumulating.

VOYAGER 2 SATURN POSITION RESAMPLED DATA 48.0 SECONDS

This data set includes Voyager 2 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 2 48-s Triaxial Fluxgate Magnetometer (MAG) Magnetic Field Data Near and Beyond Termination Shock in CDF Format

The main science objectives for the Voyager Interplanetary Mission, VIM, are as follows: - investigate the structure of the solar wind magnetic fields and plasma in the inner and outer heliosphere; - conduct long term study of heliospheric evolution during different phases of the 22-year solar magnetic cycle and the 11-year solar activity cycle; - study the long term solar modulation and determine the elemental and isotopic abundances of galactic cosmic ray particles in the heliosphere; - measure radial gradients, spectra, and nuclear abundances of the anomalous component of cosmic rays from acceleration at the solar wind termination shock; - investigate local particle acceleration in the interplanetary medium from solar flare shocks and corotating interaction regions; - study propagation of solar energetic particles in the heliosphere. The average magnetic field strength produced by the spacecraft at the location of the outboard magnetometer of the dual magnetometers system on Voyager 1 and Voyager 2 is about 0.1-0.2 nT, comparable to the most probable magnetic field strength in the inner heliosheath and significantly larger than the most probable magnetic field strength in the distant supersonic solar wind. The spacecraft magnetic field is a complex, time-dependent signal that must be removed from the measured magnetic field signal in order to derive the ambient magnetic fields of the solar wind and heliosheath. Corrections must also be made for spurious magnetic signals and noise associated with the telemetry system, ground tracking systems, and other factors. Extracting the signal describing the solar wind and heliosheath from the many sources of uncertainty is a complex and partly subjective process that requires understanding of the instrument and judgement based on experience in dealing with the ever-changing extraneous signals. We estimate that for the Voyager magnetic field data the 1-sigma the uncertainty of the 48-s averages for each of the components of the magnetic field BR, BT, and BN is typically +/- 0.02 nT; the uncertainty in magnitude F1 is typically +/- 0.03 nT. F1, BR, BT, and BN can differ from one another and they may vary with time, but there is no practical way to determine these uncertainties more precisely at present. References: D.B. Berdichevsky, Voyager Mission, Detailed processing of weak magnetic fields; I - Constraints to the uncertainties of the calibrated magnetic field signal in the Voyager missions, 2009; https://vgrmag.gsfc.nasa.gov/Berdichevsky-VOY_sensor_opu090518.pdf Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994. Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002. Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., Spacecraft studies of the interplanetary magnetic field, 76, 3564, 1971.

VOYAGER 2 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 2 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 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 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 JUP 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 JUPITER. 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 U HAVE BEEN APPLIED ONLY TO THE URANUS DATA SET.

Voyager 1 1.92-s Averaged Triaxial Fluxgate Magnetometer (MAG) Interplanetary Magnetic Field in CDF Format

This data set includes the Voyager spacecraft number (1 or 2), the date-time in decimal year (90.00000 is day 1 of 1990), the magnetic field strength, F1, computed from high-resolution magnitudes, the elevation and azimuth angles in heliographic (RTN) coordinates, and the magnetic field strength, F2, computed from 1-hr averages of the components. The vector components of B can be computed from F2 and the two angles. The elevation angle is the latitude angle above or below the solar equatorial plane, and the azimuth angle is in the direction orbital motion around the Sun from the projection of the Sun-to-spacecraft axis into the solar equatorial plane. The Voyager MAG experiment and coordinates are further described in the following publication: Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Sci. Rev., 21 (3), 235-257, 1977. At the time of experiment proposal, it was expected that the required accuracy of the measurements would be 0.1 nT, determined by the combined noise of the sensors and the spacecraft field. The spacecraft magnetic field at the outboard magnetic field sensor, referred to as the primary unit, was expected to be 0.2 nT and highly variable, consistent with current estimates. Hence, the dual magnetometer design (Ness et al., 1971, 1973; Behannon et al., 1977). At distances > 40 AU, the heliospheric magnetic fields are generally much weaker than 0.4 nT; the average magnetic field strength near 40 AU and 85 AU is about 0.15 nT and 0.05 nT, respectively. The use of roll calibrations lasting about 6 hours permits determination of the effective zero levels for the two independent magnetic axes that are perpendicular to the roll axis, which is nearly parallel to the radius vector to the Sun, at intervals of about 3 months. There is no roll calibration for the third magnetic axis. Comparison of the two derived magnetic vectors from the two magnetometers permits validation of the primary magnetometer data with an accuracy of 0.02 to 0.05 nT. A discussion of the uncertainties that must be considered when using these data is given in the Appendix of Burlaga et al. (1994) and in Appendix A of Burlaga et al. (2002). References: Behannon, K.W., M.H. Acuna, L.F. Burlaga, R.P. Lepping, N.F. Ness, and F.M. Neubauer, Magnetic-Field Experiment for Voyager-1 and Voyager-2, Space Science Reviews, 21 (3), 235-257, 1977. Burlaga, L.F., Merged interaction regions and large-scale magnetic field fluctuations during 1991 - Voyager-2 observations, J. Geophys. Res., 99 (A10), 19341-19350, 1994. Burlaga, L.F., N.F. Ness, Y.-M. Wang, and N.R. Sheeley, Jr., Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23, J. Geophys. Res., 107 (A11), 1410, 2002. Ness, N., K.W. Behannon, R. Lepping, and K.H. Schatten, J. Geophys. Res., 76, 3564, 1971. Ness et al., 1973. Coordinate Systems: Interplanetary magnetic field studies make use of two important coordinate systems, the Heliographic Inertial (HGI) coordinate system and the Heliographic (HG) coordinate system. The HGI coordinate system is used to define the spacecraft's position. The HGI system is defined with its origin at the Sun. There are three orthogonal axes, X(HGI), Y(HGI), and Z(HGI). The Z(HGI) axis points northward along the Sun's spin axis. The X(HGI)-Y(HGI) plane lays in the solar equatorial plane. The intersection of the solar equatorial plane with the ecliptic plane defines a line, the longitude of the ascending node, which is taken to be the X(HGI) axis. The X(HGI) axis drifts slowly with time, approximately one degree per 72 years. The magnetic field orientation is defined in relation to the spacecraft. Drawing a line from the Sun's center (HGI origin) to the spacecraft defines the X axis of the HG coordinate system. The HG coordinate system is defined with its origin centered at the spacecraft. Three orthogonal axes are defined, X(HG), Y(HG), and Z(HG). The X(HG) axis points radially away from the Sun and the Y(HG) axis is parallel to the solar equatorial plane and therefore parallel to the X(HGI)-Y(HGI) plane as well. The Z(HG) axis is chosen to complete the orthonormal triad. An excellent reference guide with diagrams explaining the HGI and HG systems may be found in L.F. Burlaga, MHD Processes in the Outer Heliosphere, Space Sci. Rev., 39, 255-316, 1984.

VOYAGER 1 JUP 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 JUPITER. 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 s