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1) Voyager-1 CRS Cruise Mode daily averages maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/CRS/FLUX/P1D
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:1 day
Stop:2012-08-19 00:00:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
daily averages of selected fluxes

2) Voyager-1 CRS Cruise Mode 15-minute averages maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/CRS/FLUX/PT15M
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:15 minutes
Stop:2012-08-19 00:00:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
15-minute averages of selected fluxes

3) Voyager 1 CRS Cruise Mode 6-hour averages maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/CRS/FLUX/PT6H
Start:1977-09-05 00:00:00 Observatory:Voyager 1 Cadence:6 hours
Stop:2011-10-01 00:00:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
6-hour averages of selected fluxes

4) VG1 JUP CRS DERIVED PROTON/ION/ELECTRON FLUX BROWSE V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/CRS/Jupiter/PT15M
Start:1979-02-28 00:00:00 Observatory:Voyager 1 Cadence:15 minutes
Stop:1979-03-21 23:45:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
Data Set Overview ================= Instrument P.I. : Rochus E. Vogt Data Supplier : National Space Science Data Center Data sampling rate : variable (1 hr for FPHA data, 15 min. for all others) Data Set Start Time : 1979-02-28T00:00:00.000Z Data Set Stop Time : 1979-03-21T23:45:00.000Z (The following description has been adapted from [NSSDCCRS1979]) As its name implies, the Cosmic Ray Subsystem (CRS) was designed for cosmic ray studies [STONEETAL1977B]. It consists of two high Energy Telescopes (HET), four Low Energy Telescopes (LET) and The Electron Telescope (TET). The detectors have large geometric factors (~ 0.48 to 8 cm^2 ster) and long electronic time constants (~ 24 [micro]sec) for low power consumption and good stability. Normally, the data are primarily derived from comprehensive ([Delta]E[1], [Delta]E[2] and E) pulse-height information about individual events. Because of the high particle fluxes encountered at Jupiter and Saturn, greater reliance had to be placed on counting rates in single detectors and various coincidence rates. In inter- planetary space, guard counters are placed in anticoincidence with the primary detectors to reduce the background from high-energy particles penetrating through the sides of the telescopes. These guard counters were turned off in the Jovian magnetosphere when the accidental anticoincidence rate became high enough to block a substantial fraction of the desired counts. Fortunately, under these conditions the spectra were sufficiently soft that the background, due to penetrating particles, was small. The data on proton and ion fluxes at Jupiter were obtained with the LET. The thicknesses of individual solid-state detectors in the LET and their trigger thresholds were chosen such that, even in the Jovian magnetosphere, electrons made, at most, a very minor contribution to the proton counting rates [LUPTON&STONE1972]. Dead time corrections and accidental coincidences were small (< 20%) throughout most of the magnetotail, but were substantial (> 50%) at flux maxima within 40 R[J] Of Jupiter. Data have been included in this package for those periods when the corrections are less than ~ 50% and can be corrected by the user with the dead time appropriate to the detector (2 to 25 [micro]sec). The high counting rates, however, caused some baseline shift which may have raised proton thresholds significantly. In the inner magnetosphere, the L[2] counting rate was still useful because it never rolled over. This rate is due to 1.8- to 13-MeV protons penetrating L[1] (0.43 cm^2 ster) and > 9-MeV protons penetrating the shield (8.4 cm^2 ster). For an E^-2 spectrum, the two groups would make comparable contributions; but in the magnetosphere, for the E^-3 to E^-4 spectrum above 2.5 MeV [MCDONALDETAL1979], the contribution from protons penetrating the shield would be only 3 to 14%. The LET L[1]L[2]L[4] and L[1]L[2]L[3] coincidence- anticoincidence rates give the proton flux between 1.8 and 8 MeV and 3 to 8 MeV with a small alpha particle contribution (~10^-3). Corrections are required for dead time losses in L[1], accidental L[1]L[2] coincidences and anticoincidence losses from L[4]. Data are given only for periods when these corrections are relatively small. In addition to the rates listed in the table, the energy lost in detectors L[1], L[2] and L[3] was measured for individual particles. For protons, this covered the energy range from 0.42 to 8.3 MeV. Protons can be identified positively by the [Delta]E vs. E technique, their spectra obtained and accidental coincidences greatly reduced. Because of telemetry limitations, however, only a small fraction of the events could be transmitted, and statistics become poor unless pulse-height data are averaged over a period of one hour. HET and LET detectors share the same data lines and pulse- height analyzers; thus, the telescopes can interfere with one another during periods of high counting rates. To prevent such an interference and explore different coincidence conditions, the experiment was cycled through four operating modes, each 192 seconds long. Either the HETs or the LETs were turned on at a time. LET-D was cycled through L[1] only and L[1]L[2] coincidence requirements. The TET was cycled through various coincidence conditions, including singles from the front detectors. At the expense of some time resolution, this procedure permitted us to obtain significant data in the outer magnetosphere and excellent data during the long passage through the magnetotail region. Some of the published results from this experiment required extensive corrections for dead time, accidental coincidences and anticoincidences ([VOGTETAL1979A], [VOGTETAL1979B]; [SCHARDTETAL1981]; [GEHRELS1981]). These corrections can be applied only on a case-by-case basis after a careful study of the environment and many self-consistency checks. They cannot be applied on a systematic basis and we have no computer programs to do so; therefore, data from such periods are not included in the Data Center submission. The scientists on the CRS team will, however, be glad to consider special requests if the desired information can be extracted from the data. Description of the Data ----------------------- (1) LD1 RATE gives the nominal > 0.43-MeV proton flux cm^-2 s^-1 sr^-1. This rate includes all particles which pass through a 0.8 mg/cm^2 aluminum foil and deposits more than 220 keV in a 34.6 [micron] Si detector on Voyager 1 (209 keV, 33.9 [microns] on Voyager 2) Therefore, heavy ions, such as oxygen and sulfur are also detected; however, their contribution is believed to be relatively small. Only a small percentage of the pulses in this detector are larger than the maximum energy that can be deposited by a proton. Heavy ions would produce such large pulses, unless their energy spectra were much steeper than the proton spectrum. The true flux, F[t], can be calculated from the data: F F[t] = ---------------- 1 - 1.26x10^-4 F and corrections are small for F < 1000 cm^-2 s^-1. (2) LD2 RATE is not suitable for an absolute flux determination and is given in counters per s. The detector responds to protons and ions that penetrate either (a) 0.8 mg/cm^2 Al plus 8.0 mg/cm^2 Si and lose at least 200 keV in a 35 [micron] Si detector (1.8 to 13 MeV) or (b) pass through > 140 mg/cm^2 Al. For an E^-2 proton spectrum, the contributions from (a) and (b) would be about equal; however, the proton spectrum is substantially softer throughout most of the magnetosphere and the detector should respond primarily to (a). Dead time corrections are given by R R[t] = ---------------- 1 - 2.55x10^-5 R where R is the count rate in counts/s. Thus, correction to the supplied data are small for R < 4000 c/sec, but become 80 large in the middle magnetosphere that the magnitude of even relative intensity changes becomes uncertain. (3) LD L[1].L[2]. L[4]. SL COINCIDENCE RATE gives the total proton flux (cm^-2 s^-1 sr^-1) between ~ 1.8 and ~ 8.1 MeV with a small admixture of alpha particles. Accidental coincidences become subst

5) VG1 SAT CRS RESAMPLED SUMMARY D1 RATE ELEC 192SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/CRS/Saturn/PT192S
Start:1980-11-11 16:01:36 Observatory:Voyager 1 Cadence:192 seconds
Stop:1980-11-14 22:01:36 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
Data Set Overview ==================== This data set describes 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 (see detector description for details). Note that the instrument is saturated near the maximum of counting rate of approximately 50,000 counts/sec. When data are near saturation, the counting rates should be corrected for deadtime according to the formula in the DATA_SET_OR_INST_PARM_DESC: {corrected rate} = {uncorrected rate/(1+deadtime*{uncorrected rate}). Parameters =============== SAMPLING_PARAMETER_RESOLUTION = 192.0 MINIMUM_SAMPLING_PARAMETER = N/A MAXIMUM_SAMPLING_PARAMETER = N/A SAMPLING_PARAMETER_INTERVAL = 192.0 MINIMUM_AVAILABLE_SAMPLING_INT = 192.0 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = D1/D2 RATE NOISE_LEVEL = 0.000 DATA_SET_PARAMETER_UNIT = COUNTS/SECOND

6) VOYAGER 1 DAILY POSITION V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/Ephemeris/Heliosphere/P1D
Start:1977-09-09 00:00:00 Observatory:Voyager 1 Cadence:1 day
Stop:2005-01-24 00:00:00 Instrument:Voyager 1 Positions Resource:NumericalData
Data Set Overview ================= These data were obtained from running the program HELICOOR in the public directory NSSDCA::ANON_DIR:[ACTIVE.HELIO]. These data are based on predicted trajectories calculated with the GTDS code by the NSSDC Satellite Situation Center and converted to solar ecliptic and heliographic coordinates by the HELIOCOOR program. The HELICOOR code was written by R. Parthasarathy. The program GENTRJCON added the HILLON longitude. Note that the solar ecliptic coordinates are given with respect to true equinox and ecliptic of date. The solar ascending node was located at ecliptic longitude +74.367 degrees as of 1 Jan. 1900 at 1200 UT; this longitude increases by 1.4 degrees/century. Data Formats ============ field description ----- ------------------------------ 1. Date YYYY DDD.DD where YY=year and DDD.DD=decimal day 2. Range Heliocentric range in AU 3. SE_Lat Solar Ecliptic latitude in degrees 4. SE_Lon Solar Ecliptic longitude in degrees 5. HG_Lat Heliographic latitude in degrees 6. HG_Lon Heliographic longitude in degrees 7. IHG_Lon Inertial Heliographic longitude in degrees with respect to the ascending node of the solar equator in the ecliptic. Contact Information =================== R. P. (Sardi) Parthasarathy Hughes STX Corporation / Space Physics Data Facility NASA Goddard Space Flight Center Greenbelt, Maryland sardi@nssdca.gsfc.nasa.gov Phone: (301) 286-8105 Acknowledgement =============== Use of these data in publications should be accompanied at minimum by acknowledgements of the National Space Science Data Center and the responsible Principal Investigator defined in the experiment documentation provided here.

7) VG1 JUP EPHEMERIS SYSTEM III (1965) COORDS BROWSE V1.1 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/Ephemeris/Jupiter/PT96S
Start:1979-03-03 00:00:35 Observatory:Voyager 1 Cadence:96 seconds
Stop:1979-03-16 23:59:56 Instrument:Voyager 1 Positions Resource:NumericalData
Data Set Overview ================= Version 1.1 ----------- The SEDR based data provided as part of this data set were originally reviewed and archived with the NSSDC and PDS as version 1.0 (DATA_SET_ID = VG1-J-POS-4-48.0SEC). Version 1.1 includes additional columns not present in the previous version, 96 second rather than 48 second time samples, times converted to 'PDS Style' or ISO standard, and upgrading of PDS labels and templates to version 3.2. The SPICE based data that are also part of this data set were not previously archived with the PDS. This version 1.1 data set replaces previously archived versions. Data Set Description -------------------- This data set consists of Voyager 1 Jupiter encounter ephemeris data in System III (1965) left handed coordinates covering the period 1979-03-03 to 1979-03-16. Two versions, both covering the same time period, but containing slightly different data, are provided. One version was generated by the Voyager MAG team from Voyager 1 SEDR, the other by the PDS/PPI node using the VG1_JUP.BSP and PCK00003.TCP SPICE kernels. Two versions of the spacecraft ephemeris data are provided as an attempt to correct some of the problems in the Voyager SEDR while preserving the ability to reproduce early results. The original SEDR data has a variety of problems which may affect the knowledge of the spacecraft position, or conversely, the timing associated with certain events such as ring plane crossings. The SPICE SPK kernel provided on this disk includes corrections to some, but not all, of the problems associated with the Voyager SEDR. The Navigation and Ancillary Information Facility (NAIF) at JPL may issue a new Voyager SPK kernel in the future that will further improve the knowledge of the spacecraft location in inertial space. There are other differences in the in the two versions of ephemeris data that are the result of improvements in the knowledge of some of the physical constants associated with Jupiter and its moons. Since the Voyager era, there have been updates to the orientation of the jovian spin axis right ascension and declination, the radius of Jupiter, as well as the orbital characteristic and other physical parameters of many of the moons of Jupiter. These changes affect the stated position of the spacecraft in jovigraphic coordinate systems like System III without changing the position of the spacecraft in inertial space. The spin rate of Jupiter is not changed from the System III (1965) rate of 9h 55m 29.71sec (870.536 deg/day). The SPICE planetary constants kernel (PCK) contains both the current IAU definitions of the physical constants for the bodies within in the jovian system (as data) as well as the older IAU definitions (as comments). This is an ASCII text file (PCK00003.TCP) and users of the ephemeris data are encouraged to review it. SEDR generated ephemeris ------------------------ Instrument P.I. : N/A Data Supplier : NSSDC (Voyager MAG Team) Data sampling rate : 96 seconds Data Set Start Time : 1979-03-03T00:00:35.978Z Data Set Stop Time : 1979-03-16T23:59:08.185Z SPICE generated ephemeris ------------------------- Instrument P.I. : N/A Data Supplier : S. Joy Data sampling rate : 48 seconds Data Set Start Time : 1979-03-03T00:00:35.978Z Data Set Stop Time : 1979-03-16T23:59:56.185Z Parameters ========== SEDR generated ephemeris ------------------------ PARAMETER RESOLUTION/ DESCRIPTION NAME UNITS time 96.0 Sec time of the sample (UT) in the format yyyy-mm-ddThh:mm:ss.sssZ m65536 counts spacecraft clock counts mod60 counts fds_line counts sc_x R[J] jovicentric (System III) cartesian sc_y R[J] cartesian position vectors: X, Y, and sc_z R[J] Z vel_x km/s jovicentric X, Y, and Z spacecraft vel_y km/s velocity components vel_z km/s

8) VG1 JUP EPHEMERIS HELIOGRAPHIC COORDS BROWSE V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/Ephemeris/Jupiter/PT97S
Start:1979-02-26 00:00:35 Observatory:Voyager 1 Cadence:97 seconds
Stop:1979-03-24 22:49:32 Instrument:Voyager 1 Positions Resource:NumericalData
Data Set Overview ================= This data set consists of Voyager 1 Jupiter encounter ephemeris data in Heliographic coordinates covering the period 1979-02-26 to 1979-03-24. Two versions, both covering the same time period, but containing slightly different data, are provided. One version was generated by the Voyager MAG team from Voyager 1 SEDR, the other by the PDS/PPI node using the VG1_JUP.BSP and PCK00003.TPC SPICE kernels. Two versions of the spacecraft ephemeris data are provided as an attempt to correct some of the problems in the Voyager SEDR while preserving the ability to reproduce early results. The original SEDR data has a variety of problems which may affect the knowledge of the spacecraft position, or conversely, the timing associated with certain events such as ring plane crossings. The SPICE SPK kernel provided on this disk includes corrections to some, but not all, of the problems associated with the Voyager SEDR. The Navigation and Ancillary Information Facility (NAIF) at JPL may issue a new Voyager SPK kernel in the future that will further improve the knowledge of the spacecraft location in inertial space. There are other differences in the in the two versions of ephemeris data that are the result of improvements in the knowledge of some of the physical constants associated with Jupiter and its moons. Since the Voyager era, there have been updates to the orientation of the jovian spin axis right ascension and declination, the radius of Jupiter, as well as the orbital characteristic and other physical parameters of many of the moons of Jupiter. These changes affect the stated position of the spacecraft in jovigraphic coordinate systems like System III without changing the position of the spacecraft in inertial space. The spin rate of Jupiter is not changed from the System III (1965) rate of 9h 55m 29.71sec (870.536 deg/day). The SPICE planetary constants kernel (PCK) contains both the current IAU definitions of the physical constants for the bodies within in the jovian system (as data) as well as the older IAU definitions (as comments). This is an ASCII text file (PCK00003.TCP) and users of the ephemeris data are encouraged to review it. SEDR generated ephemeris ------------------------ Data Supplier : NSSDC Data sampling rate : 96 seconds Data Set Start Time : 1979-02-26T00:00:35.897Z Data Set Stop Time : 1979-03-24T22:47:56.304Z SPICE generated ephemeris ------------------------- Data Supplier : S. Joy Data sampling rate : 48 seconds Data Set Start Time : 1979-02-26T00:00:35.897Z Data Set Stop Time : 1979-03-24T22:49:32.304Z Parameters ========== SEDR generated ephemeris ------------------------ PARAMETER RESOLUTION/ DESCRIPTION NAME UNITS time 96.0 Sec. time of the sample (UT) in the format yyyy-mm-ddThh:mm:ss.sssZ m65536 counts spacecraft clock counts mod60 fds_line sc_x AU heliographic cartesian coordinates sc_y position vectors: X, Y, and Z sc_z vel_x km/s heliocentric X, Y, and Z spacecraft vel_y velocity components vel_z sc_r AU heliographic spherical coordinates sc_lat degrees position vectors: range, latitude, and sc_lon degrees longitude SolEquatorial_to_HG solar equatorial to heliographic coordinates rotation matrix containing 9 1pe15.8 elements HG_to_EarthOrbTrue heliographic to earth orbit true coordinates rotation matrix containing 9 1pe15.8 elements Spacecraft_to_HG payload (spacecraft) to heliographic coordinates rotation matrix containing 9 1pe15.8 elements SPICE generated ephemeris ------------------------- PARAMET

9) VG1 SAT EPHEMERIS KRONOGRAPHIC (L1) COORDS BROWSE V1.1 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/Ephemeris/Saturn/PT96S
Start:1980-11-10 00:00:34 Observatory:Voyager 1 Cadence:96 seconds
Stop:1980-11-18 22:54:59 Instrument:Voyager 1 Positions Resource:NumericalData
Data Set Overview ================= Data Set Description -------------------- This data set consists of Voyager 1 Saturn encounter ephemeris data in Kronographic (L1) coordinates covering the period 1980-11-10 to 1980-11-18. Two versions, both covering the same time period, but containing slightly different data, are provided. One version was generated by the Voyager MAG team from Voyager SEDR, the other by the PDS/PPI node using the VG1_SAT.TSP and PCK00006.TPC SPICE kernels. Due to inaccuracies in Voyager SEDR, as well as changes in the values of some key parameters (e.g. Saturnian radius) the timing is improved for the SPICE generated data. However, since much of the original analysis was based upon the SEDR generated ephemeris, this data has been included as well. SEDR generated ephemeris ------------------------ Instrument P.I. : N/A Data Supplier : NSSDC Data sampling rate : 96 seconds Data Set Start Time : 1980-11-10T00:00:34.923Z Data Set Stop Time : 1980-11-18T22:54:59.149Z SPICE generated ephemeris ------------------------- Instrument P.I. : N/A Data Supplier : S. Joy Data sampling rate : 96 seconds Data Set Start Time : 1980-11-10T00:00:00.000Z Data Set Stop Time : 1980-11-18T23:58:24.000Z Parameters ========== SEDR generated ephemeris ------------------------ PARAMETER RESOLUTION/ DESCRIPTION NAME UNITS time 96.0 Sec time of the sample (UT) in the format yyyy-mm-ddThh:mm:ss.sssZ m65536 counts spacecraft clock counts mod60 counts fds_line counts sc_x R[J] kronocentric (L1) cartesian sc_y R[J] cartesian position vectors: X, Y, and sc_z R[J] Z vel_x km/s kronocentric (L1) X, Y, and Z spacecraft vel_y km/s velocity components vel_z km/s sc_r R[J] kronocentric (L1) spherical sc_lat degrees coordinates position vectors: range, sc_lon degrees latitude, and longitude CartSys3_to_SphSys3 cartesian L1 coordinates to spherical L1 coordinates rotation matrix containing 9 1pe15.8 elements SC_to_CartSys3 payload (spacecraft) to cartesian L1 coordinates rotation matrix containing 9 1pe15.8 elements SC_to_SphSys3 payload (spacecraft) to spherical L1 coordinates rotation matrix containing 9 1pe15.8 elements SPICE generated ephemeris ------------------------- PARAMETER RESOLUTION/ DESCRIPTION NAME UNITS time 96.0 Sec time of the sample (UT) in the format yyyy-mm-ddThh:mm:ss.sssZ R AU kronocentric (L1) spherical coordinates LAT degrees range, latitude, and longitude position LON degrees LocTime hours angular separation between the meridian containing the sun and the one containing the spacecraft converted to a time. The sun meridian is defined to be noon (12.000), with midnight (0.000) opposite it. Dawn (6.000) and dusk (18.000) are where the sun rises and sets according to the planet's rotation Coordinate System ================= The Kronographic (L1) coordinates is a Saturn centered spherical system, based on the Saturn Longitude System (Voyager Measurements of the Rotation Period of Saturn's Magnetic Field, Desch and Kai

10) Voyager1 LECP H Fluxbox Fluxes in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/H-FLUX-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Calibrated, Cadence PT5D

11) Voyager1 LECP H Fluxbox Fluxes in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/H-FLUX-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Calibrated, Cadence P5D

12) Voyager1 LECP H Fluxbox Rates in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/H-RATE-P26D/
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Uncalibrated, Cadence PT5D

13) Voyager1 LECP H Fluxbox Rates in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/H-RATE-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Uncalibrated, Cadence P5D

14) Voyager1 LECP He Fluxbox Fluxes in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/HE-FLUX-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Calibrated, Cadence PT5D

15) Voyager1 LECP He Fluxbox Fluxes in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/HE-FLUX-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Calibrated, Cadence P5D

16) Voyager1 LECP He Fluxbox Rates in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/HE-RATE-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Uncalibrated, Cadence PT5D

17) Voyager1 LECP He Fluxbox Rates in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/HE-RATE-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Uncalibrated, Cadence P5D

18) Voyager1 LECP O Fluxbox Fluxes in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/O-FLUX-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Calibrated, Cadence PT5D

19) Voyager1 LECP O Fluxbox Fluxes in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/O-FLUX-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Calibrated, Cadence P5D

20) Voyager1 LECP O Fluxbox Rates in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/O-RATE-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Uncalibrated, Cadence PT5D

21) Voyager1 LECP O Fluxbox Rates in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/FLUXBOX/O-RATE-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager1, LECP, Uncalibrated, Cadence P5D

22) Voyager 1 LECP Cosmic Ray Proton Rates in ASCII Format daily maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/Flux.Cosmic.Ray.P1D
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:24 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager1, LECP, Filtered, Channel, Calibrated, CadencePT24H

23) Voyager 1 LECP Cosmic Ray Proton Rates in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/Flux.Cosmic.Ray.P26D
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:26 days
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager1, LECP, Filtered, Channel, Calibrated, CadenceP26D

24) Voyager 1 LECP Ion Channel Intensities in ASCII Format daily maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/Flux.Ion.P1D
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:24 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager1, LECP, Filtered, Channel, Calibrated, CadencePT24H Each file in this directory contains one year's worth of data from the LECP instrument on the Voyager 1 spacecraft. Each record in a file contains 1-day (24-hour) averages of fluxes and flux uncertainties of ions (Z>=1) in eight contiguous energy channels, from 0.040-4.00 Mev/ion. Each file contains a 2-line header that identifies the spacecraft, data type and time resolution, and labels each column of data. Statistical uncertainties represent one standard deviation. Differential (in energy) flux units are: Ions/(cm^2 sec ster MeV).

25) Voyager 1 LECP Ion Channel Intensities in ASCII Format hourly maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/Flux.Ion.PT1H
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:1 hour
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager1, LECP, Filtered, Channel, Calibrated, CadencePT1H

26) Voyager 1 LECP Ion Channel Intensities By Sector in ASCII Format 3-hour maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/Flux.Ion.Sectored.PT3H
Start:1991-01-01 00:00:00 Observatory:Voyager 1 Cadence:3 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, For All Sectors, Voyager1, LECP, Filtered, Channel, Calibrated, CadencePT3H

27) Voyager 1 LECP Proton Intensities in ASCII Format daily maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/Flux.Proton.P1D
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:24 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager1, LECP, Filtered, Channel, Calibrated, CadencePT24H Each file in this directory contains one year's worth of data from the LECP instrument on the Voyager 1 spacecraft. Each record in a file contains 1-day (24-hour) averages of fluxes and flux uncertainties of ions (Z>=1) in eight contiguous energy channels, from 0.040-4.00 Mev/ion. Each file contains a 2-line header that identifies the spacecraft, data type and time resolution, and labels each column of data. Statistical uncertainties represent one standard deviation. Differential (in energy) flux units are: Ions/(cm^2 sec ster MeV).

28) Voyager 1 LECP Proton Intensities in ASCII Format hourly maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/Flux.Proton.PT1H
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:1 hour
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager1, LECP, Filtered, Channel, Calibrated, CadencePT1H

29) VG1 LECP 0.4 SEC HIGH RESOLUTION JUPITER NEAR ENCOUNTER DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/LECP/Jupiter/PT0.400S
Start:1979-03-04 19:41:36 Observatory:Voyager 1 Cadence:0.400 seconds
Stop:1979-03-06 08:18:15 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Data Set Overview ================= Data Set Description -------------------- This near encounter data set consists of electron and ion counting rate data from the Low Energy Charged Particle (LECP) experiment on Voyager 1 while the spacecraft was within the very close vicinity of Jupiter. This instrument measures the intensities of in-situ charged particles ( >15 keV electrons and >30 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. During Jupiter near encounter, the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystem was turned on for data collection. Particles include low energy electrons, protons, alpha particles, medium energy protons and ions, high energy and intensity protons, electrons, alpha particles, and Z >= nuclei. The near encounter data are 0.4 second rate measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into 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 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of '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, which gives 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. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. Near Encounter Channel Definitions for Voyager 1 LECP CH CH LOW HIGH MEAN GEOMETRIC CH Num NAME (MeV/N) (MeV/N) (Mev/N) FACTOR LOGIC cm**2 sr DEFINITIN -------------------------------------------------------- 1 EB01 0.015 0.037 0.020 0.00600 2 EBD1 0.015 0.500 0.020 0.00012 3 EB02 0.037 0.061 0.045 0.00600 4 EBD2 0.037 0.500 0.045 0.00012 5 EB03 0.070 0.112 0.090 0.00600 6 EBD3 0.070 0.500 0.090 0.00012 7 EB04 0.130 0.183 0.120 0.00600 8 EBD4 0.130 0.500 0.120 0.00012 9 EB05 0.200 0.500 0.200 0.00600 10 EBD5 0.200 0.500 0.200 0.00012 11 EG06 0.252 2.000 0.250 0.00200 12 EG07 0.480 2.000 0.500 0.00200 13 EG08 0.853 2.000 0.900 0.00200 14 EG09 2.100 5.000 2.000 0.00200 15 E44 0.350 1.500 0.500 1.31000 16 E45 2.500 100.000 2.000 1.31000 17 E37 6.000 100.000 6.000 1.31000 18 PL01 0.030 0.053 0.025 0.04020 19 PL02 0.053 0.085 0.050 0.04020 20 PL03 0.085 0.139 0.100 0.04020 21 PL04 0.139 0.200 0.150 0.04020 22 PL05 0.200 0.550 0.250 0.04020 23 PL06 0.540 1.050 0.600 0.04020 24 PL07 1.050 2.030 1.000 0.04020 25 PL08 2.030 4.010 2.500 0.04020 44 AL01 0.980 1.770 1.000 0.04020 45 AL02 1.770 4.220 2.500 0.04020 77 ESA0 2.500 99.999 2.500 0.49350 A-B COINC. 78 ESB0 8.500 99.999 8.500 0.94620 B 4 PI SR 79 AB10 8.500 99.999 8.500 0.05040 A-B COINC. 80 DP09 0.285 5.020 0.250 0.00084 DELTA' 81 DP10 0.480 2.580 0.600 0.00084 DELTA' 82 DP11 0.725 1.640 1.000 0.00084 DELTA' 83 PD09 0.285 5.250 0.250 0.00260 DELTA 84 PD10 0.480 2.720 0.600 0.00260 DELTA 85 PD11 0.725 1.580 1.000 0.00260 DELTA 86 AB12 54.000 87.300 50.000 0.05040 A-B COINC. 87 AB13 87.300 152.000 100.000 0.05040 A-B COINC. 88 PSA1 15.800 158.000 15.000 0.49350 A 2 PI SR 89 PSA2 15.800 49.000 25.000 0.49350 A 2 PI SR 90 PSA3 16.300 26.200 25.000 0.49350 A 2 PI SR 91 PSB1 54.000 174.000 50.000 0.94620 B 4 PI SR 92 PSB2 54.000 87.300 50.000 0.94620 B 4 PI SR 93 PSB3 54.000 59.000 50.000 0.94620 B 4 PI SR 94 DA03 0.480 2.450 0.600 0.00084 DELTA' 95 DA04 0.780 1.410 1.000 0.00084 DELTA' 96 DZ01 0.405 18.800 0.600 0.00084 DELTA' 97 AD03 0.480 2.580 0.600 0.00260 DELTA 98 AD04 0.780 1.480 1.000 0.00260 DELTA 99 ZD01 0.400 19.800 0.600 0.00260 DELTA -------------------------------------------------------- Near encounter data are stored in files for channels from different rate groups indicated by the file names, e.g. V1YYDOY{A,B,...,H}NG0{1,2, ..., 9}.CSV ------- --------- -------------- | | | | | | | | | rate group number | | | | | | | starting time A: 00:00:00 | | | B: 03:00:00 | | | C: 06:00:00 | | | D: 09:00:00 | | | E: 12:00:00 | | | F: 15:00:00 | | | G: 18:00:00 | | | H: 21:00:00 | | | | | 3-digit day of year | | | 2-digit year | Voyager 1 Rate group definitions are listed as below: ------------------------------------------------------- rate channel names group in # the rate group ------------------------------------------------------- 1 PL01 PL02 PL03 EB04 EBP04 2 EB01 EBP01 EB02 EBP02 EB03 EBP03 EG06 3 PD09 DP09 PD10 DP10 PD11 DP11 AD03 DA03 4 EG07 EG08 EG09 EB05 EBP05 5 PSA3 PSB3

30) VG1 JUP LECP CALIBRATED RESAMPLED SECTORED 15MIN V1.1 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/LECP/Jupiter/PT15M
Start:1979-02-28 00:00:11 Observatory:Voyager 1 Cadence:15 minutes
Stop:1979-03-22 23:44:44 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
DATA SET OVERVIEW ================= Version 1.1 ----------- This version 1.1 data set replaces the version 1.0 data set (DATA_SET_ID = VG1-J-LECP-4-15MIN) previously archived with the PDS. Data records from the version 1.0 data set provided data for each of 8 sectors, plus the average for all sectors in a separate record for each channel. This resulted in 9 repeated times per channel. Data records for the version 1.1 data set provide all data for a given channel and time period (8 sectors, plus the average for all sectors) in a single record. Other changes to this version include upgrading of the associated labels and templates to PDS version 3.2 compliance, modification of the time formats and flag values. Data Set Description -------------------- 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 instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles that it measures. The cycle time for the rotation is 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 and passes for other 'Z' values are not all known, but some are given in the literature (e.g. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity with the units: counts/(cm^2 str sec keV). This figure represents the structure of a single data record. Note that the 'SECTOR_STRUCTURE' (SECTOR1, SECTOR2, etc.) are not columns, but rather a grouping of the DATA_VALUE and STANDARD_DEVIATION columns. SECTOR1 SECTOR2 AVERAGE __________________ __________________ __________________ ____ | _____ _________ || _____ _________ | | _____ _________ | | |||DATA ||STANDARD ||||DATA ||STANDARD || ||DATA ||STANDARD || |TIME|||VALUE||DEVIATION||||VALUE||DEVIATION|| ... ||VALUE||DEVIATION|| |____|||_____||_________||||_____||_________|| ||_____||_________|| |__________________||__________________| |__________________| Parameters ========== Electron Rate ------------- Sampling Parameter Name : TIME Data Set Parameter Name : ELECTRON RATE Sampling Parameter Resolution : 15.000000 Sampling Parameter Interval : 15.000000 Data Set Parameter Unit : COUNTS/SECOND Noise Level : 0.000000 Sampling Parameter Unit : MINUTE A measured parameter equaling the number of electrons hitting a particle detector per specified accumulation interval. The counted electrons may or may not be discriminated as to their energies (e.g. greater than E1, or between E1 and E2).

31) VG1 LECP 3.2 MINUTE JUPITER FAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/LECP/Jupiter/PT3M
Start:1979-02-22 00:00:11 Observatory:Voyager 1 Cadence:3 minutes
Stop:1979-03-20 23:59:38 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Data Set Overview ================= Data Set Description -------------------- This far encounter step data set consists of the counting rate and flux data for electrons and ions from the Low Energy Charged Particle (LECP) experiment on Voyager 1 while the spacecraft was within the vicinity of Jupiter. This instrument measures the intensities of in-situ charged particles ( >15 keV electrons and >30 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. During Jupiter far encounter, the entire LEPT (Low Energy Particle Telescope) and part of the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystems were turned on for data collection. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 3.2 minute rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into 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 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of '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, which gives 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. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. Far Encounter Channel Definitions for Voyager 1 LECP CH CH LOW HIGH MEAN GEOMETRIC CH Num NAME (MeV/N) (MeV/N) (Mev/N) FACTOR LOGIC cm**2 sr DEFINITIN -------------------------------------------------------- 1 EB01 0.015 0.037 0.020 0.00600 2 EBD1 0.015 0.500 0.020 0.00012 3 EB02 0.037 0.061 0.045 0.00600 4 EBD2 0.037 0.500 0.045 0.00012 5 EB03 0.070 0.112 0.090 0.00600 6 EBD3 0.070 0.500 0.090 0.00012 7 EB04 0.130 0.183 0.120 0.00600 8 EBD4 0.130 0.500 0.120 0.00012 9 EB05 0.200 0.500 0.200 0.00600 10 EBD5 0.200 0.500 0.200 0.00012 11 EG06 0.252 2.000 0.250 0.00200 12 EG07 0.480 2.000 0.500 0.00200 13 EG08 0.853 2.000 0.900 0.00200 14 EG09 2.100 5.000 2.000 0.00200 15 E44 0.350 1.500 0.500 1.31000 16 E45 2.500 100.000 2.000 1.31000 17 E37 6.000 100.000 6.000 1.31000 18 PL01 0.030 0.053 0.025 0.04020 19 PL02 0.053 0.085 0.050 0.04020 20 PL03 0.085 0.139 0.100 0.04020 21 PL04 0.139 0.200 0.150 0.04020 22 PL05 0.200 0.550 0.250 0.04020 23 PL06 0.540 1.050 0.600 0.04020 24 PL07 1.050 2.030 1.000 0.04020 25 PL08 2.030 4.010 2.500 0.04020 26 P32 0.310 0.610 0.350 0.09750 E0E2(E3) 27 P1 0.570 0.890 0.600 0.44100 E1E2(E3) 28 P10 4.400 9.200 5.000 0.53900 E2E3(E4) 29 P11 9.200 21.000 12.000 0.53900 E2E3(E4) 30 P16 3.400 18.000 5.000 1.50000 E5E4(E3) 31 P23 22.000 31.000 25.000 1.31000 E5E4E3(E2) 32 P27 34.000 72.000 50.000 1.20000 E5E4E3E2 33 P31 211.000 1000.000 250.000 1.31000 E4E3 34 A39 0.100 0.203 0.100 0.09750 E0(E2) 35 A33 0.200 0.510 0.350 0.09750 E0E2(E3) 36 A46 0.147 2.000 0.600 0.44100 'D1F1,CA' 37 A3 0.460 1.800 0.600 0.44100 E1E2(E3) 38 A4 1.900 4.000 2.500 0.44100 E1E2(E3L12) 39 A12 4.200 7.800 5.000 0.53900 E2E3(E4L23) 40 A13 7.800 21.000 15.000 0.53900 E2E3(E4L23) 41 A17 3.300 69.000 5.000 1.50000 E5E4(E3L54 42 A24 22.000 31.000 25.000 1.31000 E5E4E3(E2) 43 A28 33.000 62.000 50.000 1.20000 E5E4E3E2 44 AL01 0.980 1.770 1.000 0.04020 45 AL02 1.770 4.220 2.500 0.04020 46 M34 0.150 0.180 0.200 0.09750 E0E2 47 L5 0.470 5.600 1.500 0.44100 E1E2(E3L12) 48 L14 5.800 28.000 6.000 0.53900 E2E3(E4L23) 49 L18 6.800 28.000 5.000 1.50000 E5E4(E3L54 50 M38 0.072 0.150 0.100 0.09750 E0(E2) 51 M35 0.180 0.280 0.250 0.09750 E0E2(E3) 52 M47 0.124 14.300 0.250 0.44100 D1F2 53 M6 0.530 5.600 0.500 0.44100 E1E2(E3L12) 54 M7 6.170 8.600 6.000 0.44100 E1E2(E3L12) 55 M15 9.500 46.000 15.000 0.53900 E2E3(E4L23) 56 M19 6.800 10.400 6.000 1.50000 E5E4(E3L54) 57 M20 10.400 40.000 15.000 1.50000 E5E4(E3L54) 58 M25 48.000 64.000 50.000 1.31000 E5E4E3(E2) 59 M29 68.000 270.000 70.000 1.20000 E5E4E3E2 60 H36 0.099 0.140 0.100 0.09750 E0(E2) 61 H8 0.310 2.200 0.350 0.44100 E1E2(E3) 62 H9 2.300 12.000 2.000 0.44100 E1E2(E3) 63 H43 13.000 82.000 15.000 0.53900 E2E3(E4) 64 H21 9.500 18.000 10.000 1.50000 E5E4(E3L54) 65 H22 19.000 78.000 25.000 1.50000 E5E4(E3L54) 66 H26 82.000 120.000 100.000 1.31000 E5E4E3 67 H30 127.000 850.000 150.000 1.20000 E5E4E3E2 68 AR SINGLES 69 E0 SINGLES 70 E1 SINGLES

32) VG1 LECP 48.0 SECOND JUPITER NEAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/LECP/Jupiter/PT48S
Start:1979-03-05 00:00:36 Observatory:Voyager 1 Cadence:48 seconds
Stop:1979-03-06 23:59:48 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Data Set Overview ================= Data Set Description -------------------- This near encounter step data set consists of the counting rate and flux data for electrons and ions from the Low Energy Charged Particle (LECP) experiment on Voyager 1 while the spacecraft was within the very close vicinity of Jupiter. This instrument measures the intensities of in-situ charged particles ( >15 keV electrons and >30 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. During Jupiter near encounter, the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystem was turned on for data collection. Particles include low energy electrons, protons, alpha particles, medium energy protons and ions, high energy and intensity protons, electrons, alpha particles, and Z >= nuclei. The near encounter data are 48.0 second rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into 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 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of '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, which gives 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. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. Near Encounter Channel Definitions for Voyager 1 LECP CH CH LOW HIGH MEAN GEOMETRIC CH Num NAME (MeV/N) (MeV/N) (Mev/N) FACTOR LOGIC cm**2 sr DEFINITIN -------------------------------------------------------- 1 EB01 0.015 0.037 0.020 0.00600 2 EBD1 0.015 0.500 0.020 0.00012 3 EB02 0.037 0.061 0.045 0.00600 4 EBD2 0.037 0.500 0.045 0.00012 5 EB03 0.070 0.112 0.090 0.00600 6 EBD3 0.070 0.500 0.090 0.00012 7 EB04 0.130 0.183 0.120 0.00600 8 EBD4 0.130 0.500 0.120 0.00012 9 EB05 0.200 0.500 0.200 0.00600 10 EBD5 0.200 0.500 0.200 0.00012 11 EG06 0.252 2.000 0.250 0.00200 12 EG07 0.480 2.000 0.500 0.00200 13 EG08 0.853 2.000 0.900 0.00200 14 EG09 2.100 5.000 2.000 0.00200 15 E44 0.350 1.500 0.500 1.31000 16 E45 2.500 100.000 2.000 1.31000 17 E37 6.000 100.000 6.000 1.31000 18 PL01 0.030 0.053 0.025 0.04020 19 PL02 0.053 0.085 0.050 0.04020 20 PL03 0.085 0.139 0.100 0.04020 21 PL04 0.139 0.200 0.150 0.04020 22 PL05 0.200 0.550 0.250 0.04020 23 PL06 0.540 1.050 0.600 0.04020 24 PL07 1.050 2.030 1.000 0.04020 25 PL08 2.030 4.010 2.500 0.04020 44 AL01 0.980 1.770 1.000 0.04020 45 AL02 1.770 4.220 2.500 0.04020 77 ESA0 2.500 99.999 2.500 0.49350 A-B COINC. 78 ESB0 8.500 99.999 8.500 0.94620 B 4 PI SR 79 AB10 8.500 99.999 8.500 0.05040 A-B COINC. 80 DP09 0.285 5.020 0.250 0.00084 DELTA' 81 DP10 0.480 2.580 0.600 0.00084 DELTA' 82 DP11 0.725 1.640 1.000 0.00084 DELTA' 83 PD09 0.285 5.250 0.250 0.00260 DELTA 84 PD10 0.480 2.720 0.600 0.00260 DELTA 85 PD11 0.725 1.580 1.000 0.00260 DELTA 86 AB12 54.000 87.300 50.000 0.05040 A-B COINC. 87 AB13 87.300 152.000 100.000 0.05040 A-B COINC. 88 PSA1 15.800 158.000 15.000 0.49350 A 2 PI SR 89 PSA2 15.800 49.000 25.000 0.49350 A 2 PI SR 90 PSA3 16.300 26.200 25.000 0.49350 A 2 PI SR 91 PSB1 54.000 174.000 50.000 0.94620 B 4 PI SR 92 PSB2 54.000 87.300 50.000 0.94620 B 4 PI SR 93 PSB3 54.000 59.000 50.000 0.94620 B 4 PI SR 94 DA03 0.480 2.450 0.600 0.00084 DELTA' 95 DA04 0.780 1.410 1.000 0.00084 DELTA' 96 DZ01 0.405 18.800 0.600 0.00084 DELTA' 97 AD03 0.480 2.580 0.600 0.00260 DELTA 98 AD04 0.780 1.480 1.000 0.00260 DELTA 99 ZD01 0.400 19.800 0.600 0.00260 DELTA -------------------------------------------------------- Near encounter data are stored in files for channels from different rate groups indicated by the file names, e.g. V1YYDOYS{Rate_Group_Number}.CSV ------- ----------------- | | | | | | | rate group # for near encounter | | | 1-5, 17-21, 23-26, 36-40 | | | | | 3-digit day of year | | | 2-digit year | Voyager 1 Rate group definitions are listed as below: -------------------------------------------------------------------- Rate Group CH# CH# CH# CH# CH# CH# Descriptions # -------------------------------------------------------------------- 1 18 19 20 21 22 PL01,2,3,4,5 Rates 2 23 24 25 44 45 PL06,7,8,AL01,2 Rates 3 1 3 5 7 9 EB01,2,3,4,5 Rates 4 2 4 6 8 10 EB'01,2,3,4,5 Rates 5 11 12 13 14 EG06,7,8,9 Rates 6 34 50 36 52 E0 (E1) , D1F1, D1F2 Rates 7 26 35 46 51 60 E0 E2 (E3) Rates 8 27 28 29 53 54 Protons, Mediums Rates 9 37 38 47 61 62 Alphas, L Nuclei, H Nuclei Rates

33) Voyager 1 LECP PHA Events in ASCII maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/PHA
Start:1993-01-01 00:00:00 Observatory:Voyager 1 Cadence:
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
PHA Events, Voyager1, LECP, Uncalibrated

34) Voyager 1 LECP Average Filtered Rate Data in ASCII Format daily maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/Rates.P1D
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:24 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, All Sectors, Voyager1, LECP, Filtered, Channel, CadencePT24H

35) Voyager 1 LECP Average Filtered Rate Data in ASCII Format hourly maxmize
Resource ID:spase://VEPO/NumericalData/Voyager1/LECP/Rates.PT1H
Start:1977-09-07 00:00:00 Observatory:Voyager 1 Cadence:1 hour
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, All Sectors, Voyager1, LECP, Filtered, Channel, CadencePT1H

36) VG1 LECP 0.4S HIGH RESOLUTION SATURN FAR ENCOUNTER DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/LECP/Saturn/PT0.400S
Start:1979-02-28 09:00:11 Observatory:Voyager 1 Cadence:0.400 seconds
Stop:1979-03-11 13:00:17 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Data Set Overview ================= Data Set Description -------------------- This far encounter data set consists of electron and ion counting rate data from the Low Energy Charged Particle (LECP) experiment on Voyager 1 while the spacecraft was within the vicinity of Saturn. This instrument measures the intensities of in-situ charged particles ( >15 keV electrons and >30 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. During Saturn far encounter, the entire LEPT (Low Energy Particle Telescope) and part of the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystems were turned on for data collection. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 0.4 second rate measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into 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 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of '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, which gives 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. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. Far Encounter Channel Definitions for Voyager 1 LECP CH CH LOW HIGH MEAN GEOMETRIC CH Num NAME (MeV/N) (MeV/N) (Mev/N) FACTOR LOGIC cm**2 sr DEFINITIN -------------------------------------------------------- 1 EB01 0.015 0.037 0.020 0.00600 2 EBD1 0.015 0.500 0.020 0.00012 3 EB02 0.037 0.061 0.045 0.00600 4 EBD2 0.037 0.500 0.045 0.00012 5 EB03 0.070 0.112 0.090 0.00600 6 EBD3 0.070 0.500 0.090 0.00012 7 EB04 0.130 0.183 0.120 0.00600 8 EBD4 0.130 0.500 0.120 0.00012 9 EB05 0.200 0.500 0.200 0.00600 10 EBD5 0.200 0.500 0.200 0.00012 11 EG06 0.252 2.000 0.250 0.00200 12 EG07 0.480 2.000 0.500 0.00200 13 EG08 0.853 2.000 0.900 0.00200 14 EG09 2.100 5.000 2.000 0.00200 15 E44 0.350 1.500 0.500 1.31000 16 E45 2.500 100.000 2.000 1.31000 17 E37 6.000 100.000 6.000 1.31000 18 PL01 0.030 0.053 0.025 0.04020 19 PL02 0.053 0.085 0.050 0.04020 20 PL03 0.085 0.139 0.100 0.04020 21 PL04 0.139 0.200 0.150 0.04020 22 PL05 0.200 0.550 0.250 0.04020 23 PL06 0.540 1.050 0.600 0.04020 24 PL07 1.050 2.030 1.000 0.04020 25 PL08 2.030 4.010 2.500 0.04020 26 P32 0.310 0.610 0.350 0.09750 E0E2(E3) 27 P1 0.570 0.890 0.600 0.44100 E1E2(E3) 28 P10 4.400 9.200 5.000 0.53900 E2E3(E4) 29 P11 9.200 21.000 12.000 0.53900 E2E3(E4) 30 P16 3.400 18.000 5.000 1.50000 E5E4(E3) 31 P23 22.000 31.000 25.000 1.31000 E5E4E3(E2) 32 P27 34.000 72.000 50.000 1.20000 E5E4E3E2 33 P31 211.000 1000.000 250.000 1.31000 E4E3 34 A39 0.100 0.203 0.100 0.09750 E0(E2) 35 A33 0.200 0.510 0.350 0.09750 E0E2(E3) 36 A46 0.147 2.000 0.600 0.44100 'D1F1,CA' 37 A3 0.460 1.800 0.600 0.44100 E1E2(E3) 38 A4 1.900 4.000 2.500 0.44100 E1E2(E3L12) 39 A12 4.200 7.800 5.000 0.53900 E2E3(E4L23) 40 A13 7.800 21.000 15.000 0.53900 E2E3(E4L23) 41 A17 3.300 69.000 5.000 1.50000 E5E4(E3L54 42 A24 22.000 31.000 25.000 1.31000 E5E4E3(E2) 43 A28 33.000 62.000 50.000 1.20000 E5E4E3E2 44 AL01 0.980 1.770 1.000 0.04020 45 AL02 1.770 4.220 2.500 0.04020 46 M34 0.150 0.180 0.200 0.09750 E0E2 47 L5 0.470 5.600 1.500 0.44100 E1E2(E3L12) 48 L14 5.800 28.000 6.000 0.53900 E2E3(E4L23) 49 L18 6.800 28.000 5.000 1.50000 E5E4(E3L54 50 M38 0.072 0.150 0.100 0.09750 E0(E2) 51 M35 0.180 0.280 0.250 0.09750 E0E2(E3) 52 M47 0.124 14.300 0.250 0.44100 D1F2 53 M6 0.530 5.600 0.500 0.44100 E1E2(E3L12) 54 M7 6.170 8.600 6.000 0.44100 E1E2(E3L12) 55 M15 9.500 46.000 15.000 0.53900 E2E3(E4L23) 56 M19 6.800 10.400 6.000 1.50000 E5E4(E3L54) 57 M20 10.400 40.000 15.000 1.50000 E5E4(E3L54) 58 M25 48.000 64.000 50.000 1.31000 E5E4E3(E2) 59 M29 68.000 270.000 70.000 1.20000 E5E4E3E2 60 H36 0.099 0.140 0.100 0.09750 E0(E2) 61 H8 0.310 2.200 0.350 0.44100 E1E2(E3) 62 H9 2.300 12.000 2.000 0.44100 E1E2(E3) 63 H43 13.000 82.000 15.000 0.53900 E2E3(E4) 64 H21 9.500 18.000 10.000 1.50000 E5E4(E3L54) 65 H22 19.000 78.000 25.000 1.50000 E5E4(E3L54) 66 H26 82.000 120.000 100.000 1.31000 E5E4E3 67 H30 127.000 850.000 150.000 1.20000 E5E4E3E2 68 AR SINGLES 69 E0 SINGLES 70 E1 SINGLES 71 E2

37) VG1 SAT LECP CALIBRATED RESAMPLED SECTORED 15MIN V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/LECP/Saturn/PT15M
Start:1980-11-11 00:00:00 Observatory:Voyager 1 Cadence:15 minutes
Stop:1980-11-16 23:30:00 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Data Set Description ==================== Data Set Description -------------------- 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 instrument 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 and passes for other 'Z' values are not all known, but some are given in the literature (e.g. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity with the units: counts/(cm^2 str sec keV). Parameters ========== Electron Rate ------------- Sampling Parameter Name : TIME Data Set Parameter Name : ELECTRON RATE Sampling Parameter Resolution : 15.000000 Sampling Parameter Interval : 15.000000 Data Set Parameter Unit : COUNTS/SECOND Noise Level : 0.000000 Sampling Parameter Unit : MINUTE A measured parameter equaling the number of electrons hitting a particle detector per specified accumulation interval. The counted electrons may or may not be discriminated as to their energies (e.g. greater than E1, or between E1 and E2). Ion Rate -------- Sampling Parameter Name : TIME Data Set Parameter Name : ION RATE Sampling Parameter Resolution : 15.000000 Sampling Parameter Interval : 15.000000 Data Set Parameter Unit : COUNTS/SECOND Noise Level : 0.000000 Sampling Parameter Unit : MINUTE A measured parameter equaling the number of ions striking a particle detector per specified accumulation interval. The counted ions may or may not be discriminated as to their energies (e.g. energy/nucleon or energy/charge between E1 and E2 or greater than E1) and/or as to their ion composition (atomic number Z or mass number greater than Z1 or M1, or between Z1 and z2 or M1 and M2). Source Instrument Parameters ============================ Instrument Host ID : VG1 Data Set Parameter Name : ION RATE Instrument Parameter Name : ION RATE Important Instrument Parameters : 1 Instrument Host ID : VG1 Data Set Parameter Name : ELECTRON RATE

38) VG1 LECP 6.4 MINUTE SATURN FAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/LECP/Saturn/PT6M
Start:1980-11-10 10:29:22 Observatory:Voyager 1 Cadence:6 minutes
Stop:1980-12-30 23:56:56 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Data Set Overview ================= Data Set Description -------------------- This far encounter step data set consists of the counting rate and flux data for electrons and ions from the Low Energy Charged Particle (LECP) experiment on Voyager 1 while the spacecraft was within the vicinity of Saturn. This instrument measures the intensities of in-situ charged particles ( >15 keV electrons and >30 keV ions) with various levels of discrimination based on energy range and mass species. A subset of almost 100 LECP channels are included in this data set. The LECP data are globally calibrated to the extent possible. During Saturn far encounter, the entire LEPT (Low Energy Particle Telescope) and part of the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystems were turned on for data collection. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 6.4 minute rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into 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 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of '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, which gives 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. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. Far Encounter Channel Definitions for Voyager 1 LECP CH CH LOW HIGH MEAN GEOMETRIC CH Num NAME (MeV/N) (MeV/N) (Mev/N) FACTOR LOGIC cm**2 sr DEFINITIN -------------------------------------------------------- 1 EB01 0.015 0.037 0.020 0.00600 2 EBD1 0.015 0.500 0.020 0.00012 3 EB02 0.037 0.061 0.045 0.00600 4 EBD2 0.037 0.500 0.045 0.00012 5 EB03 0.070 0.112 0.090 0.00600 6 EBD3 0.070 0.500 0.090 0.00012 7 EB04 0.130 0.183 0.120 0.00600 8 EBD4 0.130 0.500 0.120 0.00012 9 EB05 0.200 0.500 0.200 0.00600 10 EBD5 0.200 0.500 0.200 0.00012 11 EG06 0.252 2.000 0.250 0.00200 12 EG07 0.480 2.000 0.500 0.00200 13 EG08 0.853 2.000 0.900 0.00200 14 EG09 2.100 5.000 2.000 0.00200 15 E44 0.350 1.500 0.500 1.31000 16 E45 2.500 100.000 2.000 1.31000 17 E37 6.000 100.000 6.000 1.31000 18 PL01 0.030 0.053 0.025 0.04020 19 PL02 0.053 0.085 0.050 0.04020 20 PL03 0.085 0.139 0.100 0.04020 21 PL04 0.139 0.200 0.150 0.04020 22 PL05 0.200 0.550 0.250 0.04020 23 PL06 0.540 1.050 0.600 0.04020 24 PL07 1.050 2.030 1.000 0.04020 25 PL08 2.030 4.010 2.500 0.04020 26 P32 0.310 0.610 0.350 0.09750 E0E2(E3) 27 P1 0.570 0.890 0.600 0.44100 E1E2(E3) 28 P10 4.400 9.200 5.000 0.53900 E2E3(E4) 29 P11 9.200 21.000 12.000 0.53900 E2E3(E4) 30 P16 3.400 18.000 5.000 1.50000 E5E4(E3) 31 P23 22.000 31.000 25.000 1.31000 E5E4E3(E2) 32 P27 34.000 72.000 50.000 1.20000 E5E4E3E2 33 P31 211.000 1000.000 250.000 1.31000 E4E3 34 A39 0.100 0.203 0.100 0.09750 E0(E2) 35 A33 0.200 0.510 0.350 0.09750 E0E2(E3) 36 A46 0.147 2.000 0.600 0.44100 'D1F1,CA' 37 A3 0.460 1.800 0.600 0.44100 E1E2(E3) 38 A4 1.900 4.000 2.500 0.44100 E1E2(E3L12) 39 A12 4.200 7.800 5.000 0.53900 E2E3(E4L23) 40 A13 7.800 21.000 15.000 0.53900 E2E3(E4L23) 41 A17 3.300 69.000 5.000 1.50000 E5E4(E3L54 42 A24 22.000 31.000 25.000 1.31000 E5E4E3(E2) 43 A28 33.000 62.000 50.000 1.20000 E5E4E3E2 44 AL01 0.980 1.770 1.000 0.04020 45 AL02 1.770 4.220 2.500 0.04020 46 M34 0.150 0.180 0.200 0.09750 E0E2 47 L5 0.470 5.600 1.500 0.44100 E1E2(E3L12) 48 L14 5.800 28.000 6.000 0.53900 E2E3(E4L23) 49 L18 6.800 28.000 5.000 1.50000 E5E4(E3L54 50 M38 0.072 0.150 0.100 0.09750 E0(E2) 51 M35 0.180 0.280 0.250 0.09750 E0E2(E3) 52 M47 0.124 14.300 0.250 0.44100 D1F2 53 M6 0.530 5.600 0.500 0.44100 E1E2(E3L12) 54 M7 6.170 8.600 6.000 0.44100 E1E2(E3L12) 55 M15 9.500 46.000 15.000 0.53900 E2E3(E4L23) 56 M19 6.800 10.400 6.000 1.50000 E5E4(E3L54) 57 M20 10.400 40.000 15.000 1.50000 E5E4(E3L54) 58 M25 48.000 64.000 50.000 1.31000 E5E4E3(E2) 59 M29 68.000 270.000 70.000 1.20000 E5E4E3E2 60 H36 0.099 0.140 0.100 0.09750 E0(E2) 61 H8 0.310 2.200 0.350 0.44100 E1E2(E3) 62 H9 2.300 12.000 2.000 0.44100 E1E2(E3) 63 H43 13.000 82.000 15.000 0.53900 E2E3(E4) 64 H21 9.500 18.000 10.000 1.50000 E5E4(E3L54) 65 H22 19.000 78.000 25.000 1.50000 E5E4(E3L54) 66 H26 82.000 120.000 100.000 1.31000 E5E4E3 67 H30 127.000 850.000 150.000 1.20000 E5E4E3E2 68 AR SINGLES 69 E0 SINGLES 70 E1 SINGLES 71

39) VOYAGER 1 SOLAR WIND MAGNETIC FIELD HGCOORDS HOUR AVGS V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/MAG/Heliosphere.Outer/PT1H
Start:1977-09-05 00:00:00 Observatory:Voyager 1 Cadence:1 hour
Stop:2004-12-31 01:00:00 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Data Set Overview ================= This data set contains hour averages of the interplanetary magnetic field (IMF) measurements obtained by the triaxial fluxgate magnetometer experiment on Voyager 1. Identical instruments on Voyager 1 and 2 were designed to measure the IMF between Earth and Saturn (10 AU) during the primary Voyager mission. The design and performance yielded absolute accuracies to better than < 0.1 nT. In general, each component of the hourly average has an uncertainty of up to (+/- 0.05 nT) in the region beyond 10 AU. More accurate measurements can be obtained by special processing of the data, but it was not feasible to do this for the entire data set included here. The magnetic field magnitude in nT is provided along with angles of the field vector in the spacecraft- centered Heliographic (HG) coordinate system, also known as RTN. Coordinate System ================= Interplanetary magnetic field studies make use of two important coordinate systems, the Inertial Heliographic (IHG) coordinate system and the Heliographic (HG) coordinate system. The IHG coordinate system is use to define the spacecraft's position. The IHG system is defined with its origin at the Sun. There are three orthogonal axes, X(IHG), Y(IHG), and Z(IHG). The Z(IHG) axis points northward along the Sun's spin axis. The X(IHG) - Y(IHG) 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(IHG) axis. The X(IHG) axis drifts slowly with time, approximately one degree per 72 years. Magnetic field orientation is defined in relation to the spacecraft. Drawing a line from the Sun's center (IHG 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(IHG)-Y(IHG) plane too. The Z(HG) axis is chosen to complete the orthonormal triad. An excellent reference guide with diagrams explaining the IHG and HG systems may be found in Space and Science Reviews, Volume 39 (1984), pages 255-316, MHD Processes in the Outer Heliosphere, L. F. Burlaga [BURLAGA1984]. Data Formats ============ field description (data before 1990) ----- ------------------------------ 1. s/c id (1 = Voyager-1, 2 = Voyager-2) 2. UTC YY DDD HH where YY=year, DDD=day, and HH=hour 3. X X IHG position component (A.U. - IHG coordinates) 4. Y Y IHG position component (A.U. - IHG coordinates) 5. Z Z IHG position component (A.U. - IHG coordinates) 6. Range Heliocentric range = sqrt(X*X+Y*Y+Z*Z) 7. F1 Field magnitude (nT) ( avg(F2(48sec)) ) 8. F2 Field modulus (nT) ( norm (B1,B2,B3) ) 9. delta Latitudinal angle (degrees - HG coordinates) 10. lambda Longitudinal angle (degrees - HG coordinates) field descriptor (data after 1990) ----- ---------------------------- 1. s/c identification (FLT1=Voyager 1) (FLT2=Voyager 2) 2. Time (UTC) decimal year format (90.00000 is day 1 of 1990) 3. The magnetic field strength, F1, computed from high-resolution observations. 4. The elevation angle (degrees) in heliographic coordinates. 5. The azimuthal angle (degrees) in heliographic coordinates. 6. The magnetic field strength, F2, computed from hour averages of the components. The components of B can be computed from F2 and the two angles. MAG field components may be recovered using F2, delta and lambda. BR = F2*COS(lambda)*COS(delta) Fortran users need to convert BT = F2*SIN(lambda)*COS(delta) degrees to radians before BN = F2*SIN(delta) using trig functions. Contact Information =================== Principal Investigator: Prof. Norman F. Ness Bartol Research Institute Univerity of Delaware Newark, Delaware 19716-4793 Phone: (302) 831-8116 Fax: (302) 831-1843 Email: norman.ness@mus.udel.edu Data Contact: Dr. Len Burlaga Code 612.2 NASA Goddard Space Flight Center Greenbelt, MD 20771 Tel.: 301-286-5956 Fax: 301-286-1433

40) VOYAGER 1 SOLAR WIND MAGNETIC FIELD HGCOORDS 48SEC AVG V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/MAG/Heliosphere.Outer/PT48S
Start:1977-09-05 14:19:47 Observatory:Voyager 1 Cadence:48 seconds
Stop:1989-12-31 22:08:33 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Data Set Overview ================= This dataset contains Voyager 1 magnetometer data from the interplanetary cruise averaged to 48 second samples in Heliographic coordinates. Data Processing =============== The high resolution data submitted to the NSSDC has its origins in the original MVS 'Summary' data sets formally produced on the NSSC IBM MVS mainframe system. The original data sets contain a mix of engineering, electron, magnetic field and plasma data. The Voyager magnetometer (MAG) experiment now resides on a dedicated workstation where only MAG data are processed. All Voyager MAG data submitted to the NSSDC consists wholly of high resolution LFM averages. These files consist of a set of averages applied across all of the mission's differing telemetry modes. In the case of the Magnetometer Experiment, the records contain both 1.92 second, 9.6 second and 48 second averages. 1.92 second averages are created from the detail detail data, 9.6 second averages are created from 1.92 second averages and 48 second averages are created from the 9.6 second averages. All data in this NSSDC data set are interplanetary and in heliographic coordinates (see below). An ASCII formated data set containing key components of the 48 second magnetic field data and ephemeris data has been created allowing more convenient access to high resolution Voyager magnetometer data. Coordinate System ================= Interplanetary magnetic field studies make use of two important coordinate systems, the Inertial Heliographic (IHG) coordinate system and the Heliographic (HG) coordinate system. The IHG coordinate system is use to define the spacecraft's position. The IHG system is defined with its origin at the Sun. There are three orthogonal axes, X(IHG), Y(IHG), and Z(IHG). The Z(IHG) axis points northward along the Sun's spin axis. The X(IHG) - Y(IHG) 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(IHG) axis. The X(IHG) axis drifts slowly with time, approximately one degree per 72 years. Magnetic field orientation is defined in relation to the spacecraft. Drawing a line from the Sun's center (IHG 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(IHG)-Y(IHG) plane too. The Z(HG) axis is chosen to complete the orthonormal triad. An excellent reference guide with diagrams explaining the IHG and HG systems may be found in Space and Science Reviews, Volume 39 (1984), pages 255-316, MHD Processes in the Outer Heliosphere, L. F. Burlaga [BURLAGA1984]. Data Format =========== field descriptor ----- ---------- 1. s/c identification (FLT1=Voyager 1) (FLT2=Voyager 2) 2. coordinate system (HG=heliographic)used for this data set 3. Time (UTC) format YY DDD HH MM SS MSS YY = year DDD = day of year HH = hour MM = minute SS = second MSS = millisecond 4. field magnitude (nT) 5. field component 1 (nT) - HG 6. field component 2 (nT) - HG 7. field component 3 (nT) - HG 8. spacecraft radial distance (AU) 9. spacecraft x position (AU) - IHG 10. spacecraft y position (AU) - IHG 11. spacecraft z position (AU) - IHG Contact Information =================== Principal Investigator: Prof. Norman F. Ness Bartol Research Institute Univerity of Delaware Newark, Delaware 19716-4793 Phone: (302) 831-8116 Fax: (302) 831-1843 Email: norman.ness@mus.udel.edu Acknowledgement

41) VG1 JUP MAG RESAMPLED SYSTEM III (1965) COORDS 1.92SEC V1.1 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/MAG/Jupiter/PT1.92S
Start:1979-03-03 00:00:35 Observatory:Voyager 1 Cadence:1.92 seconds
Stop:1979-03-17 00:00:42 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Version 1.1 ----------- This version 1.1 data set replaces the version 1.0 data set (DATA_SET_ID = VG1-J-MAG-4-1.92SEC) previously archived with PDS. Changes to this version include the addition of data columns not included in version 1.0, the modification of time format and flag values, and upgrade of associated labels and catalog templates to PDS version 3.2. Data Set Overview ================= This data set includes calibrated magnetic field data acquired by the Voyager 1 Low Field Magnetometer (LFM) during the Jupiter encounter. Coverage begins in the solar wind inbound to Jupiter and continues past the last outbound bowshock crossing. The data are in System III (1965) (SYS3) coordinates and have been averaged from the 60 ms instrument sample rate to a 1.92 second sample rate. All magnetic field measurements are given in nanoTesla (nT). The magnetic field data are calibrated (see the calibration description included in the Voyager 1 Magnetometer instrument catalog file for details). Parameters ========== The full LFM instrument sample rate is 1 sample per 0.06 seconds. Full telemetry resolution 'detail' data must be obtained from the instrument team. These data have been resampled at 1.92 seconds from the detail data. The LFM has eight dynamic ranges. The instrument is designed switch between dynamic ranges automatically depending upon the observed magnetic field magnitude and fluctuations. Instrument digitization uncertainty depends upon dynamic range as indicated in the following table (from [BEHANNONETAL1977]). ----------------------------------------------- LFM Dynamic ranges and quantization uncertainty ----------------------------------------------- Range (nT) Quantization (nT) ----------------------------------------------- 1. +/- 8.8 +/- .0022 2. +/- 26 +/- .0063 3. +/- 79 +/- .019 4. +/- 240 +/- .059 5. +/- 710 +/- .173 6. +/- 2100 +/- .513 7. +/- 6400 +/- 1.56 8. +/- 50,000 +/- 12.2 Processing ========== Voyager EDR's undergo the following processing in order to produce these 1.92 second averaged summary data: * Read EDR * Unpack header block (rec. id, s/c id, tel. mode, FDS counts, data flags) * Convert selected time tags to integer time (yy/ddd/hh:mm:ss.fff) * Unpack sub-header block (MAG status words, plasma data) * Unpack science block (MAG counts) * Convert counts to gammas * Apply sensor and boom alignment matrices * Rotate (optional) 1.92 second averages while averaging detail gammas to create 1.92 second averages * Write Summary record Counts are measured onboard using 12 bit words that may represent values ranging from 0-4096. Integer counts are converted to magnetic field units (gammas) by subtracting a zero offset, from the measured MAG value and multiplying this difference by the sensitivity of the instrument. Data ==== The data files are given in ASCII, fixed field width, comma delimited tables. The record structure is described in the following table: -------------------------------------------------------------------- 1.92 Second System III (1965) Coordinates ------------------------------------------------------------------- Column Type Description ------------------------------------------------------------------- time a23 spacecraft event time (UT) of the sample in the format: yyyy-mm-ddThh:mm:ss.sss sclk a12 spacecraft clock in the format: MOD65536:MOD60:FDS-LINE mag_id i1 magnetometer ID (1 = LFM, 2 = HFM) Br f9.3 average of detail magnetic field R component in nT Btheta f9.3 average of detail magnetic field Theta component in nT Bphi f9.3 average of detail magnetic field Phi component in nT Bmag f

42) VG1 JUP MAG RESAMPLED SYSTEM III (1965) COORDS 48.0SEC V1.1 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/MAG/Jupiter/PT48.0S
Start:1979-03-03 00:00:35 Observatory:Voyager 1 Cadence:48.0 seconds
Stop:1979-03-16 23:59:56 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Version 1.1 ----------- This version 1.1 data set replaces the version 1.0 data set (DATA_SET_ID = VG1-J-MAG-4-48.0SEC) previously archived with PDS. Changes to this version include the addition of data columns not included in version 1.0, the modification of time format and flag values, and upgrade of associated labels and catalog templates to PDS version 3.2. Data Set Overview ================= This data set includes calibrated magnetic field data acquired by the Voyager 1 Low Field Magnetometer (LFM) during the Jupiter encounter. Coverage begins in the solar wind inbound to Jupiter and continues past the last outbound bowshock crossing. The data are in System III (1965) (SYS3) coordinates and have been averaged from the 9.6 second summary data to a 48 second sample rate. All magnetic field measurements are given in nanoTesla (nT). The magnetic field data are calibrated (see the calibration description included in the Voyager 1 Magnetometer instrument catalog file for details). Ephemeris data, provided in 96 second sampled System III (1965) coordinates, have been merged into the data files for this data set. The ephemeris data, generated from Voyager 1 SEDR and provided by the Voyager MAG Team, are part of the data set VG1-J-POS-6-SUMM-S3COORDS-V1.1. The position vectors for times at which ephemeris is not provided have been flagged. Parameters ========== The full LFM instrument sample rate is 1 sample per 0.06 seconds. Full telemetry resolution 'detail' data must be obtained from the instrument team. For this data set, the data have been resampled to 48 seconds from 9.6 second averages. The 9.6 second data were resampled from 1.92 second averages which were in turn resampled from the detail data. The LFM has eight dynamic ranges. The instrument is designed switch between dynamic ranges automatically depending upon the observed magnetic field magnitude and fluctuations. Instrument digitization uncertainty depends upon dynamic range as indicated in the following table (from [BEHANNONETAL1977]). ----------------------------------------------- LFM Dynamic ranges and quantization uncertainty ----------------------------------------------- Range (nT) Quantization (nT) ----------------------------------------------- 1. +/- 8.8 +/- .0022 2. +/- 26 +/- .0063 3. +/- 79 +/- .019 4. +/- 240 +/- .059 5. +/- 710 +/- .173 6. +/- 2100 +/- .513 7. +/- 6400 +/- 1.56 8. +/- 50,000 +/- 12.2 Processing ========== Voyager EDR's undergo the following processing in order to produce these 48 second averaged summary data: * Read EDR * Unpack header block (rec. id, s/c id, tel. mode, FDS counts, data flags) * Convert selected time tags to integer time (yy/ddd/hh:mm:ss.fff) * Unpack sub-header block (MAG status words, plasma data) * Unpack science block (MAG counts) * Convert counts to gammas * Apply sensor and boom alignment matrices * Rotate (optional) 1.92 second averages while averaging detail gammas to create 1.92 second averages * Average 1.92 second data to 9.6 seconds, then 9.6 second data to 48 seconds * Write Summary record Counts are measured onboard using 12 bit words that may represent values ranging from 0-4096. Integer counts are converted to magnetic field units (gammas) by subtracting a zero offset, from the measured MAG value and multiplying this difference by the sensitivity of the instrument. Data ==== The data files are given in ASCII, fixed field width, comma delimited tables. The record structure is described in the following table: -------------------------------------------------------------------- 48 Second System III (1965) Coordinates -------------------------------------------------------------------- Column Type Description -------------------------------------------------------------------- time a

43) VG1 JUP MAG RESAMPLED SYSTEM III (1965) COORDS 9.60SEC V1.1 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/MAG/Jupiter/PT9.60S
Start:1979-03-03 00:00:35 Observatory:Voyager 1 Cadence:9.60 seconds
Stop:1979-03-17 00:00:34 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Version 1.1 ----------- This version 1.1 data set replaces the version 1.0 data set (DATA_SET_ID = VG1-J-MAG-4-9.60SEC) previously archived with PDS. Changes to this version include the addition of data columns not included in version 1.0, the modification of time format and flag values, and upgrade of associated labels and catalog templates to PDS version 3.2. Data Set Overview ================= This data set includes calibrated magnetic field data acquired by the Voyager 1 Low Field Magnetometer (LFM) during the Jupiter encounter. Coverage begins in the solar wind inbound to Jupiter and continues past the last outbound bowshock crossing. The data are in System III (1965) (SYS3) coordinates and have been averaged from the 1.92 second summary data to a 9.6 second sample rate. All magnetic field measurements are given in nanoTesla (nT). The magnetic field data are calibrated (see the calibration description included in the Voyager 1 Magnetometer instrument catalog file for details). Parameters ========== The full LFM instrument sample rate is 1 sample per 0.06 seconds. Full telemetry resolution 'detail' data must be obtained from the instrument team. For this data set, the data have been resampled to 9.6 seconds from 1.92 second summary data. The 1.92 second data were in turn resampled from the detail data. The LFM has eight dynamic ranges. The instrument is designed switch between dynamic ranges automatically depending upon the observed magnetic field magnitude and fluctuations. Instrument digitization uncertainty depends upon dynamic range as indicated in the following table (from [BEHANNONETAL1977]). ----------------------------------------------- LFM Dynamic ranges and quantization uncertainty ----------------------------------------------- Range (nT) Quantization (nT) ----------------------------------------------- 1. +/- 8.8 +/- .0022 2. +/- 26 +/- .0063 3. +/- 79 +/- .019 4. +/- 240 +/- .059 5. +/- 710 +/- .173 6. +/- 2100 +/- .513 7. +/- 6400 +/- 1.56 8. +/- 50,000 +/- 12.2 Processing ========== Voyager EDR's undergo the following processing in order to produce these 9.6 second averaged summary data: * Read EDR * Unpack header block (rec. id, s/c id, tel. mode, FDS counts, data flags) * Convert selected time tags to integer time (yy/ddd/hh:mm:ss.fff) * Unpack sub-header block (MAG status words, plasma data) * Unpack science block (MAG counts) * Convert counts to gammas * Apply sensor and boom alignment matrices * Rotate (optional) 1.92 second averages while averaging detail gammas to create 1.92 second averages * Average 1.92 second data to 9.6 seconds * Write Summary record Counts are measured onboard using 12 bit words that may represent values ranging from 0-4096. Integer counts are converted to magnetic field units (gammas) by subtracting a zero offset, from the measured MAG value and multiplying this difference by the sensitivity of the instrument. Data ==== The data files are given in ASCII, fixed field width, comma delimited tables. The record structure is described in the following table: -------------------------------------------------------------------- 9.6 Second System III (1965) Coordinates -------------------------------------------------------------------- Column Type Description -------------------------------------------------------------------- time a23 spacecraft event time (UT) of the sample in the format: yyyy-mm-ddThh:mm:ss.sss sclk a12 spacecraft clock in the format: MOD65536:MOD60:FDS-LINE mag_id i1 magnetometer ID (1 = LFM, 2 = HFM) Br f9.3 average of detail magnetic field R component in nT Btheta f9.3 average of detail magnetic field Theta component in nT Bphi f9.3 average of detail magnetic field Phi component in

44) Voyager 1 MAG 2-day plots at MAG team site maxmize
Resource ID:spase://VHO/DisplayData/Voyager1/MAG/PT96S
Start:1977-09-05 00:00:00 Observatory:Voyager 1 Cadence:96 seconds
Stop:1991-12-26 00:00:00 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Voyager 1 magnetic field data plots at the Voyager MAG team site. Plots show magnetic field magnitude, direction angles, and Cartesian components in RTN coordinates. Plots typically cover 2 days.

45) VG1 SAT MAG RESAMPLED KRONOGRAPHIC (L1) COORDS 1.92SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/MAG/Saturn/PT1.92S
Start:1980-11-10 00:00:34 Observatory:Voyager 1 Cadence:1.92 seconds
Stop:1980-11-18 22:57:21 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Data Set Overview ================= This data set includes calibrated magnetic field data acquired by the Voyager 1 Low Field Magnetometer (LFM) during the Saturn encounter. Coverage begins in the solar wind inbound to Saturn and continues past the last outbound bowshock crossing. The data are in Kronographic (L1) coordinates and have been averaged from the 60 ms instrument sample rate to a 1.92 second sample rate. All magnetic field measurements are given in nanoTesla (nT). The magnetic field data are calibrated (see the calibration description included in the Voyager 1 Magnetometer instrument catalog file for details). Parameters ========== The full LFM instrument sample rate is 1 sample per 0.06 seconds. Full telemetry resolution 'detail' data must be obtained from the instrument team. These data have been resampled at 1.92 seconds from the detail data. Sampling Parameter Name : TIME Data Set Parameter Name : MAGNETIC FIELD VECTOR Sampling Parameter Resolution : 1.920000 Minimum Sampling Parameter : 19770820120000.000000 Maximum Sampling Parameter : UNK Sampling Parameter Interval : 1.920000 Minimum Available Sampling Int : 0.060000 Data Set Parameter Unit : NANOTESLA Noise Level : 0.006000 Sampling Parameter Unit : SECOND The LFM has eight dynamic ranges. The instrument is designed switch between dynamic ranges automatically depending upon the observed magnetic field magnitude and fluctuations. Instrument digitization uncertainty depends upon dynamic range as indicated in the following table (from [BEHANNONETAL1977]). ----------------------------------------------- LFM Dynamic ranges and quantization uncertainty ----------------------------------------------- Range (nT) Quantization (nT) ----------------------------------------------- 1. +/- 8.8 +/- .0022 2. +/- 26 +/- .0063 3. +/- 79 +/- .019 4. +/- 240 +/- .059 5. +/- 710 +/- .173 6. +/- 2100 +/- .513 7. +/- 6400 +/- 1.56 8. +/- 50,000 +/- 12.2 Instrument Host ID : VG1 Data Set Parameter Name : MAGNETIC FIELD VECTOR Instrument Parameter Name : MAGNETIC FIELD COMPONENT Important Instrument Parameters : 1 Instrument Host ID : VG1 Data Set Parameter Name : MAGNETIC FIELD VECTOR Instrument Parameter Name : WAVE MAGNETIC FIELD INTENSITY Important Instrument Parameters : 1 Processing ========== Voyager EDR's undergo the following processing in order to produce these 1.92 second averaged summary data: * Read EDR * Unpack header block (rec. id, s/c id, tel. mode, FDS counts, data flags) * Convert selected time tags to integer time (yy/ddd/hh:mm:ss.fff) * Unpack sub-header block (MAG status words, plasma data) * Unpack science block (MAG counts) * Convert counts to gammas * Apply sensor and boom alignment matrices * Rotate (optional) 1.92 second averages while averaging detail gammas to create 1.92 second averages * Write Summary record Counts are measured onboard using 12 bit words that may represent values ranging from 0-4096. Integer counts are converted to magnetic field units (gammas) by subtracting a zero offset, from the measured MAG value and multiplying this difference by the sensitivity of the instrument. Processing Level Id : 4 Software Flag : Y Processing Start Time : 1988-09-21 Source Data Set ID : N/A Software : UNK Product Data Set ID : VG1-S-MAG-4-1.92SEC Data ==== The data files are given in ASCII, fixed field width, comma

46) VG1 SAT MAG RESAMPLED HELIOGRAPHIC (RTN) COORDS 48.0SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/MAG/Saturn/PT48.0S
Start:1980-11-10 00:00:34 Observatory:Voyager 1 Cadence:48.0 seconds
Stop:1980-11-20 23:59:47 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Data Set Overview ================= This data set includes calibrated magnetic field data acquired by the Voyager 1 Low Field Magnetometer (LFM) during the Saturn encounter. Coverage begins in the solar wind inbound to Saturn and continues past the last outbound bowshock crossing. The data are in Heliographic (RTN) coordinates and have been averaged from the 9.6 second summary rate to a 48 second sample rate. All magnetic field measurements are given in nanoTesla (nT). The magnetic field data are calibrated (see the calibration description included in the Voyager 1 Magnetometer instrument catalog file for details). Parameters ========== The full LFM instrument sample rate is 1 sample per 0.06 seconds. Full telemetry resolution 'detail' data must be obtained from the instrument team. For this data set, the data have been resampled to 48 seconds from 9.6 second averages. The 9.6 second data were resampled from 1.92 second averages which were in turn resampled from the detail data. The LFM has eight dynamic ranges. The instrument is designed switch between dynamic ranges automatically depending upon the observed magnetic field magnitude and fluctuations. Instrument digitization uncertainty depends upon dynamic range as indicated in the following table (from [BEHANNONETAL1977]). ----------------------------------------------- LFM Dynamic ranges and quantization uncertainty ----------------------------------------------- Range (nT) Quantization (nT) ----------------------------------------------- 1. +/- 8.8 +/- .0022 2. +/- 26 +/- .0063 3. +/- 79 +/- .019 4. +/- 240 +/- .059 5. +/- 710 +/- .173 6. +/- 2100 +/- .513 7. +/- 6400 +/- 1.56 8. +/- 50,000 +/- 12.2 Processing ========== Voyager EDR's undergo the following processing in order to produce these 48 second averaged summary data: * Read EDR * Unpack header block (rec. id, s/c id, tel. mode, FDS counts, data flags) * Convert selected time tags to integer time (yy/ddd/hh:mm:ss.fff) * Unpack sub-header block (MAG status words, plasma data) * Unpack science block (MAG counts) * Convert counts to gammas * Apply sensor and boom alignment matrices * Rotate (optional) 1.92 second averages while averaging detail gammas to create 1.92 second averages * Average 1.92 second data to 9.6 seconds, then 9.6 second data to 48 seconds * Write Summary record Counts are measured onboard using 12 bit words that may represent values ranging from 0-4096. Integer counts are converted to magnetic field units (gammas) by subtracting a zero offset, from the measured MAG value and multiplying this difference by the sensitivity of the instrument. Data ==== The data files are given in ASCII, fixed field width, comma delimited tables. The record structure is described in the following table: -------------------------------------------------------------------- 48 Second Heliographic (RTN) Coordinates -------------------------------------------------------------------- Column Type Description -------------------------------------------------------------------- time a23 spacecraft event time (UT) of the sample in the format: yyyy-mm-ddThh:mm:ss.sss sclk a12 spacecraft clock in the format: MOD65536:MOD60:FDS-LINE mag_id i1 magnetometer ID (1 = LFM, 2 = HFM) Br f9.3 average of detail magnetic field R component in nT Bt f9.3 average of detail magnetic field T component in nT Bn f9.3 average of detail magnetic field N component in nT Bmag f9.3 magnitude of the averaged magnetic field components in nT avg_Bmag f9.3 average of the magnetic field magnitude over the averaging interval in nT Delta f7.3 spacecraft centered heliographic magnetic field latitude in degrees: Delta = asin(Bn/Bmag) Lambda f7.3 spacecraft centered heliographic magnetic field longitude in degrees: Lambda = atan(Bt/Br) rms_Br f8.3 root-mean-square deviation of Br over the averagi

47) VG1 SAT MAG RESAMPLED KRONOGRAPHIC (L1) COORDS 48.0SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/MAG/Saturn/PT48S
Start:1980-11-10 00:00:34 Observatory:Voyager 1 Cadence:48 seconds
Stop:1980-11-18 22:56:35 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Data Set Overview ================= This data set includes calibrated magnetic field data acquired by the Voyager 1 Low Field Magnetometer (LFM) during the Saturn encounter. Coverage begins in the solar wind inbound to Saturn and continues past the last outbound bowshock crossing. The data are in Kronographic (L1) coordinates and have been averaged from the 9.6 second summary rate to a 48 second sample rate. All magnetic field measurements are given in nanoTesla (nT). The magnetic field data are calibrated (see the calibration description included in the Voyager 1 Magnetometer instrument catalog file for details). This data set supersedes VG1-S-MAG-4-48.0SEC Parameters ========== The full LFM instrument sample rate is 1 sample per 0.06 seconds. Full telemetry resolution 'detail' data must be obtained from the instrument team. For this data set, the data have been resampled to 48 seconds from 9.6 second averages. The 9.6 second data were resampled from 1.92 second averages which were in turn resampled from the detail data. Sampling Parameter Name : TIME Data Set Parameter Name : MAGNETIC FIELD VECTOR Sampling Parameter Resolution : 48.000000 Minimum Sampling Parameter : 19770820120000.000000 Maximum Sampling Parameter : UNK Sampling Parameter Interval : 48.000000 Minimum Available Sampling Int : 0.060000 Data Set Parameter Unit : NANOTESLA Noise Level : 0.006000 Sampling Parameter Unit : SECOND The LFM has eight dynamic ranges. The instrument is designed switch between dynamic ranges automatically depending upon the observed magnetic field magnitude and fluctuations. Instrument digitization uncertainty depends upon dynamic range as indicated in the following table (from [BEHANNONETAL1977]). ----------------------------------------------- LFM Dynamic ranges and quantization uncertainty ----------------------------------------------- Range (nT) Quantization (nT) ----------------------------------------------- 1. +/- 8.8 +/- .0022 2. +/- 26 +/- .0063 3. +/- 79 +/- .019 4. +/- 240 +/- .059 5. +/- 710 +/- .173 6. +/- 2100 +/- .513 7. +/- 6400 +/- 1.56 8. +/- 50,000 +/- 12.2 Instrument Host ID : VG1 Data Set Parameter Name : MAGNETIC FIELD VECTOR Instrument Parameter Name : MAGNETIC FIELD COMPONENT Important Instrument Parameters : 1 Instrument Host ID : VG1 Data Set Parameter Name : MAGNETIC FIELD VECTOR Instrument Parameter Name : WAVE MAGNETIC FIELD INTENSITY Important Instrument Parameters : 1 Processing ========== Voyager EDR's undergo the following processing in order to produce these 48 second averaged summary data: * Read EDR * Unpack header block (rec. id, s/c id, tel. mode, FDS counts, data flags) * Convert selected time tags to integer time (yy/ddd/hh:mm:ss.fff) * Unpack sub-header block (MAG status words, plasma data) * Unpack science block (MAG counts) * Convert counts to gammas * Apply sensor and boom alignment matrices * Rotate (optional) 1.92 second averages while averaging detail gammas to create 1.92 second averages * Average 1.92 second data to 9.6 seconds, then 9.6 second data to 48 seconds * Write Summary record Counts are measured onboard using 12 bit words that may represent values ranging from 0-4096. Integer counts are converted to magnetic field units (gammas) by subtracting a zero offset, from the measured MAG value and multiplying this difference by the sensitivity of the instrument. Processing Level Id : 4 Software Flag : Y Processing Start Time : 1988-09-21 Source Data Set ID : N/A Software : UNK Product Data Set ID : VG1-S-MAG-4-48.0SEC

48) VG1 SAT MAG RESAMPLED KRONOGRAPHIC (L1) COORDS 9.6SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/MAG/Saturn/PT9.60S
Start:1980-11-10 00:00:34 Observatory:Voyager 1 Cadence:9.60 seconds
Stop:1980-11-18 22:57:13 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
Data Set Overview ================= This data set includes calibrated magnetic field data acquired by the Voyager 1 Low Field Magnetometer (LFM) during the Saturn encounter. Coverage begins in the solar wind inbound to Saturn and continues past the last outbound bowshock crossing. The data are in Kronographic (L1) coordinates and have been averaged from the 1.92 second summary rate to a 9.6 second sample rate. All magnetic field measurements are given in nanoTesla (nT). The magnetic field data are calibrated (see the calibration description included in the Voyager 1 Magnetometer instrument catalog file for details). Parameters ========== The full LFM instrument sample rate is 1 sample per 0.06 seconds. Full telemetry resolution 'detail' data must be obtained from the instrument team. For this data set, the data have been resampled to 9.6 seconds from 1.92 second summary data. The 1.92 second data were in turn resampled from the detail data. Sampling Parameter Name : TIME Data Set Parameter Name : MAGNETIC FIELD VECTOR Sampling Parameter Resolution : 9.600000 Minimum Sampling Parameter : 19770820120000.000000 Maximum Sampling Parameter : UNK Sampling Parameter Interval : 9.600000 Minimum Available Sampling Int : 0.060000 Data Set Parameter Unit : NANOTESLA Noise Level : 0.006000 Sampling Parameter Unit : SECOND The LFM has eight dynamic ranges. The instrument is designed switch between dynamic ranges automatically depending upon the observed magnetic field magnitude and fluctuations. Instrument digitization uncertainty depends upon dynamic range as indicated in the following table (from [BEHANNONETAL1977]). ----------------------------------------------- LFM Dynamic ranges and quantization uncertainty ----------------------------------------------- Range (nT) Quantization (nT) ----------------------------------------------- 1. +/- 8.8 +/- .0022 2. +/- 26 +/- .0063 3. +/- 79 +/- .019 4. +/- 240 +/- .059 5. +/- 710 +/- .173 6. +/- 2100 +/- .513 7. +/- 6400 +/- 1.56 8. +/- 50,000 +/- 12.2 Instrument Host ID : VG1 Data Set Parameter Name : MAGNETIC FIELD VECTOR Instrument Parameter Name : MAGNETIC FIELD COMPONENT Important Instrument Parameters : 1 Instrument Host ID : VG1 Data Set Parameter Name : MAGNETIC FIELD VECTOR Instrument Parameter Name : WAVE MAGNETIC FIELD INTENSITY Important Instrument Parameters : 1 Processing ========== Voyager EDR's undergo the following processing in order to produce these 9.6 second averaged summary data: * Read EDR * Unpack header block (rec. id, s/c id, tel. mode, FDS counts, data flags) * Convert selected time tags to integer time (yy/ddd/hh:mm:ss.fff) * Unpack sub-header block (MAG status words, plasma data) * Unpack science block (MAG counts) * Convert counts to gammas * Apply sensor and boom alignment matrices * Rotate (optional) 1.92 second averages while averaging detail gammas to create 1.92 second averages * Average 1.92 second data to 9.6 seconds * Write Summary record Counts are measured onboard using 12 bit words that may represent values ranging from 0-4096. Integer counts are converted to magnetic field units (gammas) by subtracting a zero offset, from the measured MAG value and multiplying this difference by the sensitivity of the instrument. Processing Level Id : 4 Software Flag : Y Processing Start Time : 1988-09-21 Source Data Set ID : N/A Software : UNK Product Data Set ID : VG1-S-MAG-4-9.60SEC Data ====

49) VOYAGER 1 SOLAR WIND PLS 1 HOUR AVERAGES V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/PLS/Heliosphere/PT1H
Start:1977-09-07 09:00:00 Observatory:Voyager 1 Cadence:1 hour
Stop:1980-12-31 17:00:00 Instrument:Plasma Spectrometer (PLS) Resource:NumericalData
Voyager 1 plasma data of the solar wind, 1 hour averages. The files in this directory contain the Voyager hourly average plasma data. The plasma parameters are obtained by finding the best fit of a convected isotropic Maxwellian distribution to the data. One sigma errors are typically less than 0.5% in the speed and VR, less than 5% for the density and thermal speed, and vary greatly for VT and VN. Sampling times range from 12 to 192 sec., with sampling generally more frequent early in the mission. The columns are: 1) Year 2) day of year (day 1 is Jan. 1) 3) hour 4) proton speed in km/s (magnitude of V) 5) proton density in cm-3 6) proton thermal speed in km/s (proton temperature in eV = .0052 times the square of the thermal speed) 7) VR 8) VT (WARNING: this parameter is often NOT reliable after 1989) 9) VN (WARNING: this parameter is often NOT reliable after 1989) The velocity components are given in the RTN coordinate system, where R is radially outward, T is in a plane parallel to the solar equatorial plane and positive in the direction of solar rotation, and N completes a right-handed system. Please consult with us, or at least send preprints, when you use this data to prevent grievous errors or misconceptions. (John Richardson, jdr@space.mit.edu)

50) VOYAGER 1 SOLAR WIND PLS FINE RES V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/PLS/Heliosphere/PT96S
Start:1977-09-07 09:21:00 Observatory:Voyager 1 Cadence:96 seconds
Stop:1980-12-31 17:56:00 Instrument:Plasma Spectrometer (PLS) Resource:NumericalData
Voyager 1 plasma data of the solar wind, fine resolution data. The files in this directory contain the Voyager fine resolution plasma data. The plasma parameters are obtained by finding the best fit of a convected isotropic Maxwellian distribution to the data. One sigma errors are typically less than 0.5 percent in the speed and VR, less than 5 percent for the density and thermal speed, and vary greatly for VT and VN. Sampling times range from 12 to 192 sec., with sampling generally more frequent early in the mission. The columns are: 1) Year 2) day of year (day 1 is Jan. 1) 3) decimal hour 4) proton speed in km/s (magnitude of V) 5) proton density in cm-3 6) proton thermal speed in km/s (proton temperature in eV = .0052 times the square of the thermal speed) 7) VR 8) VT (WARNING: this parameter is often NOT reliable after 1989) 9) VN (WARNING: this parameter is often NOT reliable after 1989) The velocity components are given in the RTN coordinate system, where R is radially outward, T is in a plane parallel to the solar equatorial plane and positive in the direction of solar rotation, and N completes a right-handed system. Please consult with us, or at least send preprints, when you use this data to prevent grievous errors or misconceptions. (John Richardson, jdr@space.mit.edu)

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