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1) Cassini RPWS Key Parameter 60S maxmize
Resource ID:spase://VWO/NumericalData/Cassini/RPWS/KP_PT60S
Start:1997-10-25 00:00:00 Observatory:Cassini Cadence:60 seconds
Stop:2014-02-24 01:03:42 Instrument:Cassini RPWS Resource:NumericalData
The Cassini Radio and Plasma Wave Science (RPWS) calibrated summary key parameter data set includes reduced temporal and spectral resolution spectral information calibrated in units of spectral density for the entire Cassini mission. This data set includes calibrated values binned and averaged within 1 minute by 0.1 decade spectral channels for all times during the mission including the two Venus flybys, the Earth flyby, the Jupiter flyby, interplanetary cruise, and the entire Saturn tour. Data for this data set are acquired by the RPWS Low Frequency Receiver (LFR), Medium Frequency Receiver (MFR), and High Frequency Receiver (HFR). Data are presented in a set of fixed-record-length tables. This data set is intended to provide numerical summary data which can be used in conjunction with other Cassini fields and particles key parameter data sets to establish trends, select events, or simply as a browse data set for the Cassini RPWS archive. This data set should be among the first used by a user of any of the RPWS archive as it will lead one to information required to search for more detailed or highly specialized products.

2) Cassini RPWS Low Rate Full Resolution maxmize
Resource ID:spase://VWO/NumericalData/Cassini/RPWS/LRFULL_PT32S
Start:1997-10-25 00:00:00 Observatory:Cassini Cadence:32 seconds
Stop:2014-02-24 01:03:42 Instrument:Cassini RPWS Resource:NumericalData
The Cassini Radio and Plasma Wave Science (RPWS) Low Rate Full Resolution Calibrated (RPWS_LOW_RATE_FULL) is a data set including all spectral density measurements acquired by the RPWS in units of electric or magnetic field spectral density. This data set includes calibrated values for each frequency channel for each sensor for all times during the mission including the two Venus flybys, the Earth flyby, the Jupiter flyby, interplanetary cruise, and the entire Saturn tour. Data for this data set are acquired from the RPWS Low Frequency Receiver (LFR), Medium Frequency Receiver (MFR), Medium Frequency Digital Receiver (MFDR) (which can be used to replace MFR band 2 data) and High Frequency Receiver (HFR). Data are presented in a set of tables organized so as to have fixed-length records for ease in data handling. This data set is intended to be the most comprehensive and complete data set included in the Cassini RPWS archive. A browse data set is included with these data which provides for a graphical search of the data using a series of thumbnail and full-sized spectrograms which lead the user to the particular data file(s) of interest. This data set should be among the first used by a user of any of the RPWS archive as it will lead one to information required to search for more detailed or highly specialized products.

3) 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

4) 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

5) 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

6) 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

7) 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

8) 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

9) 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

10) 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

11) 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 ====

12) VG1 SAT PLS DERIVED ION SOLAR WIND BROWSE 96SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/PLS/Saturn/PT96S
Start:1980-11-11 00:06:19 Observatory:Voyager 1 Cadence:96 seconds
Stop:1980-11-21 04:44:51 Instrument:Plasma Spectrometer (PLS) Resource:NumericalData
Data Set Overview ================= Instrument P.I. : John D. Richardson Data Supplier : John D. Richardson Data sampling rate : 96 seconds Data Set Start Time : 1981-08-19T00:00:09.229Z Data Set Stop Time : 1981-09-04T02:51:21.885Z This data set contains solar wind plasma browse data near the Voyager 1 Saturn encounter. Moment parameters are given. Since only the first 72 or last 72 energy/charge channels are telemetered to Earth from each M-mode spectra, derived parameters change significantly only every other set of spectra so the effective time resolution is 96 second. Parameters ========== Data Set Parameter 'ION DENSITY' -------------------------------- Data Set Parameter Name : ION DENSITY Data Set Parameter Unit : CM**-3 Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND Minimum Sampling Parameter : UNK Maximum Sampling Parameter : UNK Sampling Parameter Interval : UNK Minimum Available Sampling Int : UNK Noise Level : UNK A derived parameter equaling the number of ions per unit volume over a specified range of ion energy, energy/charge, or energy/nucleon. Discrimination with regard to mass and or charge state is necessary to obtain this quantity, however, mass and charge state are often assumed due to instrument limitations. Many different forms of ion density are derived. Some are distinguished by their composition (N+, proton, ion, etc.) or their method of derivation (Maxwellian fit, method of moments). In some cases, more than one type of density will be provided in a single data set. In general, if more than one ion species is analyzed, either by moment or fit, a total density will be provided which is the sum of the ion densities. If a plasma component does not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, in which case the density of each Maxwellian is given. Data Set Parameter 'ION TEMPERATURE' ------------------------------------ Data Set Parameter Name : ION TEMPERATURE Data Set Parameter Unit : EV Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND Minimum Sampling Parameter : UNK Maximum Sampling Parameter : UNK Sampling Parameter Interval : UNK Minimum Available Sampling Int : UNK Noise Level : UNK A derived parameter giving an indication of the mean energy/ion, assuming the shape of the ion energy spectrum to be Maxwellian. Given that the ion energy spectrum is not exactly Maxwellian, the ion temperature can be defined integrally (whereby the mean energy obtained by integrating under the actual ion energy spectrum is set equal to the integral under a Maxwellian, where the temperature is a free parameter for which to solve), or differentially (whereby the slopes of the actually ion energy spectrum at various energies are matched to the slopes of a corresponding Maxwellian). The temperature parameter is often qualified with a range of applicable energies. Temperatures can be angularly anisotropic. If the ions do not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, each with a separate temperature. Data Set Parameter 'ION THERMAL SPEED' -------------------------------------- Data Set Parameter Name : ION THERMAL SPEED Data Set Parameter Unit : KM/S Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND Minimum Sampling Parameter : UNK Maximum Sampling Parameter : UNK Sampling Parameter Interval : UNK Minimum Available Sampling Int : UNK Noise Level : UNK A measure of the velocity associated with the temperature of the ions. It is formally defined as the Ion Thermal Speed squared equals two times K (Boltzmann's constant) times T (temperature of ion) divided by M (ion mass). Each component of a plasma has a thermal speed associated with it. Data Set Parameter 'ION VELOCITY' --------------------------------- Data Set Parameter Name : ION VELOCITY Data Set Parameter Unit : KM/S Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND

13) VG1 SAT PRA CALIBRATED HI-RES LOW FREQ. REC. BAND DATA V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/PRA/Saturn/PT6S
Start:1980-11-11 22:09:23 Observatory:Voyager 1 Cadence:6 seconds
Stop:1980-11-16 23:59:47 Instrument:Voyager 1 Planetary Radio Astronomy (PRA) experiment Resource:NumericalData
Data Set Overview ================= This data set (VG1-S-PRA-3-RDR-LOWBAND-6SEC-V1.0) contains data acquired by the Voyager-1 Planetary Radio Astronomy (PRA) instrument during the Saturn encounter. Since the PRA instrument is able to observe planetary phenomenon at much larger ranges than other fields and particles experiments, thus the PRA data cover a variable and longer encounter period. PRA lowband data provided here cover the entire Saturn Encounter Phase (1981-06-05 to 1981-09-28). VG1-S-PRA-3-RDR-LOWBAND-6SEC-V1.0 contains data at the highest time resolution possible during normal operations. The normal mode of PRA operations during the planetary encounters was to sweep through the two radio receiver bands, high band (40.5 to 1.5 MHz in 128 channels spaced 0.3072 MHz apart) and low band (1326.0 to 1.2 kHz in 70 channels spaced 19.2 kHz apart) in a period of 6 seconds. The receivers measured, on alternate samples, the left hand circular and right hand circular (radio definition) power. Measured Parameters =================== The data here are from the low frequency receiver band and are 'packaged' into spacecraft major frame records. Each major frame is 48 seconds long or eight sweeps through the PRA receiver. The data are calibrated and are given in units of 'millibels' which is 1000 times the log of the received power. Zero millbels corresponds to approximately 1.4 x 10^-21 W m^-2 Hz^-1, however, this value is never seen in practice. The minimum values detected, which includes receiver internal and spacecraft generated noise, are about 2300 to 2400 millibels, or about 3.5 x 10^-19 W m^-2 Hz^-1; even higher values are seen at the very lowest frequencies. The data format is ASCII and consists of a time indicator followed by an array containing the eight low band sweeps. Time is spacecraft event time (SCET) which is basically universal time at the spacecraft. Specifically, time is in the form of YYMMDD and seconds into YYMMDD. Both are written as I6. Example: July 1, 1979 at 12 hours SCET would be 790701, 43200. The seconds corresponds, to the nearest second, to the start of the sweep (which occurs in PRA high band). The first value in low band (1326.0 kHz) occurs some 3.9 seconds after this time and samples at successively lower frequencies are space 0.03 seconds apart. Only one time is given for the entire major frame, thus the start of each sweep is the time given plus 6 times the sweep number minus 1 (i.e., 0 through 7). The data array is dimensioned as 71 X 8 and written as I4 format (i.e. 568I4). The '8' corresponds to the eight PRA sweeps. The lowest 68 of the 70 low band channels (1287.6 to 1.2 kHz) are in positions 2-69. Positions 70-71 should be ignored. Missing or bad data values are set to zero. In position 1 of each sweep is a status word where the 12 least significant bits have used, although not all 12 have meaning for PRA low band. Numbering those bits 0 for least significant to 11 for most significant, the bits that have meaning are as follows: bit 0: 15 dB attenuator in use when equal to 1 1: 30 dB attenuator in use when equal to 1 2: 45 dB attenuator in use when equal to 1 9,10 (together): polarization of first channel sampled (1326.0 kHz) according to the scheme: value bit 10 = 0 1 value bit 9 = 0 R L 1 L R Polarization at successively lower frequencies is opposite to the frequency above it, i.e. either a LRLR or an RLRL pattern. Successive 6-second sweeps start on the opposite polarization as the previous sweep as indicated in the status bits. Note that this polarization is the received polarization, not necessarily the emitted polarization. Correct interpretation of the received polarization depends on the antenna plane orientation relative to the radio source. A good description of this concept can be found in [LEBLANCETAL1987]. Missing or bad data values are set to zero. If the status word is zero, any data in that receiver sweep should be discarded.

14) VG1 SAT PWS EDITED SPECTRUM ANALYZER 4.0SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/PWS/Saturn/PT4.0S
Start:1981-08-24 00:00:47 Observatory:Voyager 1 Cadence:4.0 seconds
Stop:1981-08-31 23:56:46 Instrument:Plasma Wave System (PWS) Resource:NumericalData
Data Set Overview ================= Data Set Description -------------------- This data set consists of 4-second edited, wave electric field intensities from the Voyager 1 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Jovian magnetosphere. For each 4-second interval, a field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kiloHertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of intensities (16 channels) is the time of the beginning of the scan. During data gaps where complete 4-second spectra are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. When one or more channels are missing within a scan, the missing measurements are zero-filled. Data are edited but not calibrated. The data numbers in this data set can be plotted in raw form for event searches and simple trend analysis since they are roughly proportional to the log of the electric field strength. Calibration procedures and tables are provided for use with this data set; the use of these is described below. Use of Voyager PWS Calibration Tables The Voyager PWS calibration table is given in an ASCII text file named SA_CL.TAB (for Voyager-1). This provides information to convert the uncalibrated 'data number' output of the PWS 16-channel spectrum analyzer to calibrated antenna voltages for each frequency channel. Following is a brief description of these files and a tutorial in their application. Descriptive headers have been removed from the calibration table file. The columns included are IDN, ICHAN01, ICHAN02, ICHAN03, ICHAN04, ICHAN05, ICHAN06, ... ICHAN16. The first column lists an uncalibrated data number followed by the corresponding value in calibrated volts for each of the 16 frequency channels of the PWS spectrum analyzer. Each line contains calibrations for successive data number values ranging from 0 through 255. (Data number 0 actually represents the lack of data since the baseline noise values for each channel are all above that.) A data analysis program may load the appropriate table into a data structure and thus provide a simple look-up scheme to obtain the appropriate voltage for a given data number and frequency channel. For example, the following VAX FORTRAN code may be used to load a calibration array for Voyager 1 PWS: real*4 cal (16,0:255) open ( unit=10, file='SA_CL.TAB', status='old' ) do i=0,255 read (10,*) idn, (cal(ichan,i),ichan=1,16) end do close (10) Then, given an uncalibrated data value idn for the frequency channel ichan, the corresponding calibrated antenna voltage would be given by the following array reference: volts = cal (ichan, idn) This may be converted to a wave electric field amplitude by dividing by the effective antenna length in meters, 7.07 m. That is: efield = cal(ichan, idn) / 7.07 Spectral density units may be obtained by dividing the square of the electric field value by the nominal frequency bandwidth of the corresponding spectrum analyzer channel. specdens = (cal(ichan,idn)/7.07)**2 / bandwidth(ichan) Finally, power flux may be obtained by dividing the spectral density by the impedance of free space in ohms: pwrflux = ((cal(ichan,idn)/7.07)**2/bandwidth(ichan))/376.73 Of course, for a particular application, it may be more efficient to apply the above conversions to the calibration table directly. The center frequencies and bandwidths of each PWS spectrum analyzer channel for the Voyager 1 PWS are given below: VOYAGER 1 PWS SPECTRUM ANALYZER Voyager-1 Channel Center Frequency Bandwidth 1 10.0 Hz 2.16 Hz 2 17.8 Hz 3.58 Hz 3 31.1 Hz 4.50 Hz 4 56.2 Hz 10.7 Hz

15) VG1 SAT PWS RESAMPLED SPECTRAL ANALYZER 48SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/PWS/Saturn/PT48S
Start:1980-11-11 00:00:00 Observatory:Voyager 1 Cadence:48 seconds
Stop:1980-11-11 23:59:12 Instrument:Plasma Wave System (PWS) Resource:NumericalData
Data Set Overview ================= Instrument P.I. : Donald A. Gurnett Data Supplier : William S. Kurth Data sampling rate : 48 seconds Data Set Start Time : 1981-08-24T00:00:00.000Z Data Set Stop Time : 1981-08-31T23:59:12.000Z Data Set Description -------------------- This data set consists of 48-second calibrated, averaged wave electric field intensities from the Voyager 1 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Jovian magnetosphere. For each 48-second interval, a geometric average field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kiloHertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of averages is the beginning of the averaging interval. Averages are stored in units of volt/meter. During data gaps where complete 48-second intervals are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. Additional information about this data set and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in [GURNETTETAL1979] and a complete instrument description can be found in [SCARF&GURNETT1977]. Processing Level Id : 4 Software Flag : Y Processing Start Time : 1988-02-01 Parameters ========== Sampling Parameter Name : TIME Data Set Parameter Name : PLASMA WAVE SPECTRUM Sampling Parameter Resolution : 48.000000 Minimum Sampling Parameter : 197708201553.000000 Sampling Parameter Interval : 48.000000 Minimum Available Sampling Int : 4.000000 Data Set Parameter Unit : VOLT/METER Noise Level : 0.000005 Sampling Parameter Unit : SECOND A set of derived parameters consisting of wave electric field intensities or electric field spectral densities at various contiguous frequencies over a range of frequencies. The MKS units are: Volts/Meter or Volts**2/(Hertz Meter**2), respectively. Source Instrument Parameters ============================ Instrument Host ID : VG1 Data Set Parameter Name : PLASMA WAVE SPECTRUM Instrument Parameter Names : ELECTRIC FIELD WAVEFORM ELECTRIC FIELD COMPONENT MAGNETIC FIELD COMPONENT WAVE ELECTRIC FIELD INTENSITY WAVE MAGNETIC FIELD INTENSITY Important Instrument Parameters : 1 (for all parameters)

16) VOYAGER 1 TITAN RADIO OCCULTATION RAW DATA V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager1/RSS/Saturn/PT0.00001S
Start:1980-11-12 00:00:00 Observatory: Cadence:0.00001 seconds
Stop:1980-11-12 23:59:59 Instrument: Resource:NumericalData
Data Set Overview ================= This data set consists of raw data collected during the Titan radio occultation of Voyager 1 in November 1980 plus ancillary files that might be useful in analysis of those data. The raw data are sampled voltage outputs from receivers tuned to the Voyager carrier frequencies at both S-band and X-band during the occultations. The data have been reduced to give profiles of atmospheric temperature and pressure as a function of height above the surface on both the ingress and egress sides of Titan [LINDALETAL1983] and to make a marginal detection of an ionosphere [BIRDETAL1997]. During the Titan occultation, the Voyager 1 spacecraft provided a coherent, dual-frequency microwave radio signal source. The signal frequency was derived from a precision, onboard Ultra-Stable Oscillator (USO). The spacecraft high-gain antenna (HGA) beamed that signal through the atmosphere of Titan. As the spacecraft moved on its trajectory, the radio signal probed different levels in the atmosphere. An hour later the signals were received by antennas of the NASA Deep Space Network (DSN) on Earth. Because the density of Titan's atmosphere was so poorly known prior to the Voyager encounter, experiment planners did not know how much refractive bending to expect during the observations. Models predicted a range of behaviors from very little bending to so much that the narrow beam from the spacecraft high-gain antenna (HGA) would be deflected away from Earth and the surface occultation would not be seen. Timing uncertainties in the motion of the spacecraft with respect to Titan only complicated the problem. The experiment was implemented with a very small (0.11 deg) fixed HGA offset during the ingress occultation and a large (2.36 deg) offset during egress. These choices, in retrospect, were very good given the atmosphere that was found. Parameters ========== The output of the S-band receiver was a sinusoidal carrier signal embedded in noise -- a voltage with bandwidth approximately 50 kHz and sampled at 300000 samples per second. The X-band receiver output was similar; but, because of greater potential for Doppler drift and prediction uncertainty, its bandwidth was 150 kHz and sampling rate was 300000 samples per second. Voltages typically were in the range +/- 10 volts; but the absolute levels were not calibrated. In fact, they are generally not needed since it is the frequency (or phase) of the signal (rather than amplitude) that is most useful in inferring properties of a neutral atmosphere or ionosphere. The frequency of the USO was known from monitoring during the Jupiter-Saturn cruise (and from post-Saturn observations). Doppler contributions from motions of the spacecraft, Earth, Titan, and other bodies of the solar system were determined jointly with the Voyager Navigation Team. Relativistic Doppler contributions could be estimated from proximity to large masses. Receiver tuning was recorded in POCA (Programmable Oscillator Control Assembly) files, which are included with this archive. Processing ========== No processing per se has been carried out on these data. However, because of the high sampling rate, the 8-bit samples were recorded originally on wide-bandwidth analog video tape. The analog tapes were then replayed later at slower speeds and the digital data were extracted and separated onto computer compatible tapes (CCTs) with S-band and X-band data on different sets of tapes. Because the S-band data had been oversampled originally (300 ksps for a 50 kHz bandwidth), only one of every three samples was saved during the transfer of S-band data to CCTs. This process, known as 'decimation', meant that 300 seconds of data could be stored on an S-band CCT whereas only 100 seconds of X-band data would fit. Because analog recording technology was required to save the high data rate digital samples, there are occasional dropouts in the sample stream. These can be detected by paying special attention to counter fields in data record headers. Two analog recorders (A and B) were available at each DSN complex. Because a single recorder could not capture the entire set of Titan occultation activities, the two were run in parallel with staggered start/stop times. Most data were collected using Recorder A; but Recorder B was used to capture the samples while Recorder A was being reloaded. Data ==== Primary data were delivered to Voyager Radio Science Team members in the form of 30 megabyte (MB) CCTs covering 300 s (S-band) or 100 s (X-band). Each tape had 6000 records of 5056 bytes (56 bytes of header information and 5000 8-bit samples of receiver output voltage). Tapes were numbered sequentially as CCTs were generated from the high density video originals. Tapes with Titan data from Recorder A were numbered VJ6281 through VJ6360; tapes from Recorder B were numbered VJ6361 through VJ6380. Test and calibration data after the Titan encounter were collected on Recorder A and have numbers VJ6589 through VJ6594. The original tape numbering has been preserved in the current file names, which have the form VJnnnnCC.ODR. On tapes where one or more records could not be read, the original has been separated into two or more files. The character 'C' indicates the ordering of these file fragments with 'A' being first (and the default with no tape reading errors), 'B' next, etc. Each Original D

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