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1) VG2 URA CRS RESAMPLED SUMMARY D2 RATE ELEC 96SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/CRS/Uranus/PT96S
Start:1986-01-24 10:00:00 Observatory:Voyager 2 Cadence:96 seconds
Stop:1986-01-25 00:00:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
Counting rate from the D2 detector in the Cosmic Ray System (CRS) electron telescope (TET) on Voyager 2 during the Uranus encounter. The D2 detector nominally responds to electrons with kinetic energies above approximately 2.5 MeV (see detector description for details). SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 6.0 MINIMUM_SAMPLING_PARAMETER = N/A MAXIMUM_SAMPLING_PARAMETER = N/A SAMPLING_PARAMETER_INTERVAL = 96.0 MINIMUM_AVAILABLE_SAMPLING_INT = 96.0 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = D2 RATE NOISE_LEVEL = 0.000 DATA_SET_PARAMETER_UNIT = COUNTS/SECOND

2) VG2 URA TRAJECTORY DERIVED SUMM U1 COORDS 48SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/Ephemeris/Uranus/PT48S
Start:1986-01-24 06:59:12 Observatory:Voyager 2 Cadence:48 seconds
Stop:1986-01-25 04:00:47 Instrument:Voyager 2 Positions Resource:NumericalData
This dataset contains Voyager 2 spacecraft position vectors relative to Uranus in minus U1 coordinates. The U1 or Uranus West Longitude System coordinate system is a planetocentric system fixed to Uranus which is rotating with a 17.24 hour period. The prime meridian of the this system is defined such that at 1986-01-24T18:00:00.000 the Voyager 2 spacecraft was at 302 degrees west longitude (58 degrees east longitude). For the PDS archive dataset, the original data archive has been converted to an east longitude (righthanded) coordinate system minus U1 (-U1). This is achieved by subtracting the U1 longitude from 360.0 degrees. The data are provided in units of Uranian radii which was taken to be 25,600km by the Voyager project. Angles are given in degrees. Both cartesian and spherical coordinates are provided. The Cartesian coordinate system is defined as follows: - X lies in the equatorial plane of Uranus, positive away from the planet, and through the prime meridian at the reference epoch. - Z is parallel to the Uranus spin axis, positive in the southern hemisphere in ecliptic (orbital) coordinates, and, - Y is Z x X (righthanded) The Cartesian coordinate system does not rotate with the planet. SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 96.0 MINIMUM_SAMPLING_PARAMETER = N/A MAXIMUM_SAMPLING_PARAMETER = N/A SAMPLING_PARAMETER_INTERVAL = 48.0 MINIMUM_AVAILABLE_SAMPLING_INT = 48.0 SAMPLING_PARAMETER_UNIT = SECONDS DATA_SET_PARAMETER_NAME = POSITION VECTOR NOISE_LEVEL = N/A DATA_SET_PARAMETER_UNIT = URANUS RADII (25,600km) OR DEGREES

3) VG2 LECP 0.4S HIGH RESOLUTION URANUS FAR ENCOUNTER DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Uranus/PT0.400S
Start:1986-01-24 00:00:00 Observatory:Voyager 2 Cadence:0.400 seconds
Stop:1986-01-26 23:59:57 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 2 while the spacecraft was within the vicinity of Uranus. This instrument measures the intensities of in-situ charged particles ( >13 keV electrons and >24 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 Uranus 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 2 LECP CH CH LOW HIGH MEAN GEOMETRIC CH Num NAME (MeV/N) (MeV/N) (Mev/N) FACTOR LOGIC cm**2 sr DEFINITIN -------------------------------------------------------- 1 EB01 0.013 0.035 0.020 0.00200 2 EBD1 0.013 0.035 0.020 0.00200 3 EB02 0.035 0.061 0.045 0.00200 4 EBD2 0.035 0.061 0.045 0.00200 5 EB03 0.061 0.112 0.090 0.00200 6 EBD3 0.061 0.112 0.090 0.00200 7 EB04 0.112 0.183 0.120 0.00200 8 EBD4 0.112 0.183 0.120 0.00200 9 EB05 0.183 0.500 0.200 0.00200 10 EBD5 0.183 0.500 0.200 0.00200 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 2.000 100.000 2.000 1.31000 17 E37 6.000 100.000 6.000 1.31000 18 PL01 0.024 0.048 0.025 0.12000 19 PL02 0.048 0.080 0.050 0.12000 20 PL03 0.080 0.137 0.100 0.12000 21 PL04 0.137 0.215 0.150 0.12000 22 PL05 0.215 0.540 0.250 0.12000 23 PL06 0.540 0.990 0.600 0.12000 24 PL07 0.990 2.140 1.000 0.12000 25 PL08 2.140 3.500 2.500 0.12000 26 P32 0.330 0.610 0.350 0.09750 E0E2(E3) 27 P1 0.520 1.450 0.600 0.44100 E1E2(E3) 28 P10 4.400 11.400 5.000 0.53900 E2E3(E4) 29 P11 11.400 20.000 12.000 0.53900 E2E3(E4) 30 P16 3.040 17.000 5.000 1.50000 E5E4(E3) 31 P23 22.000 30.000 25.000 1.31000 E5E4E3(E2) 32 P27 37.000 89.000 50.000 1.20000 E5E4E3E2 33 P31 213.000 1000.000 250.000 1.31000 E4E3 34 A39 0.091 0.233 0.100 0.09750 E0(E2) 35 A33 0.230 0.480 0.350 0.09750 E0E2(E3) 36 A46 0.147 2.000 0.600 0.44100 'D1F1,CA' 37 A3 0.420 1.700 0.600 0.44100 E1E2(E3) 38 A4 1.800 4.000 2.500 0.44100 E1E2(E3L12) 39 A12 4.200 7.800 5.000 0.53900 E2E3(E4L23) 40 A13 7.800 20.000 15.000 0.53900 E2E3(E4L23) 41 A17 3.000 58.000 5.000 1.50000 E5E4(E3L54) 42 A24 22.000 30.000 25.000 1.31000 E5E4E3(E2) 43 A28 31.000 56.000 50.000 1.20000 E5E4E3E2 44 AL01 1.040 1.850 1.000 0.12000 CALC. 45 AL02 1.850 3.700 2.500 0.12000 CALC. 46 M34 0.230 0.440 0.200 0.09750 E0E2 47 L5 0.710 5.600 1.500 0.44100 E1E2(E3L12) 48 L14 5.800 28.000 6.000 0.53900 E2E3(E4L23) 49 L18 3.900 20.000 5.000 1.50000 E5E4(E3L54) 50 M38 0.060 0.200 0.100 0.09750 E0(E2) 51 M35 0.200 0.340 0.250 0.09750 E0E2(E3) 52 M47 0.124 14.300 0.250 0.44100 D1F2 53 M6 0.470 5.200 0.500 0.44100 E1E2(E3L12) 54 M7 5.200 8.200 6.000 0.44100 E1E2(E3L12) 55 M15 8.600 40.000 15.000 0.53900 E2E3(E4L23) 56 M19 6.000 9.200 6.000 1.50000 E5E4(E3L54) 57 M20 9.600 42.000 15.000 1.50000 E5E4(E3L54) 58 M25 44.000 61.000 50.000 1.31000 E5E4E3(E2) 59 M29 69.000 270.000 70.000 1.20000 E5E4E3E2 60 H36 0.099 0.140 0.100 0.09750 E0(E2) 61 H8 0.280 1.900 0.350 0.44100 E1E2(E3) 62 H9 2.000 12.000 2.000 0.44100 E1E2(E3) 63 H43 11.800 74.000 15.000 0.53900 E2E3(E4) 64 H21 8.200 17.000 10.000 1.50000 E5E4(E3L54) 65 H22 18.000 82.000 25.000 1.50000 E5E4(E3L54) 66 H26 86.000 120.000 100.000 1.31000 E5E4E3 67 H30 127.000 1000.000 150.000 1.20000 E5E4E3E2 68 AR SINGLES 69 E0 SINGLES 70 E1 SINGLES 71 E2

4) VG2 URA LECP RESAMPLED RDR STEPPING SECTOR 12.8MIN V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Uranus/PT12M48S
Start:1986-01-24 00:00:00 Observatory:Voyager 2 Cadence:12 minutes; 48 seconds
Stop:1986-01-27 00:00:00 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
This data consists of resampled data from the Low Energy Charged Particle (LECP) Experiment on the Voyager 2 Spacecraft for the period when Voyager 2 was in the vicinity of the planet Uranus. The period covered is 1989/day 24/0000 SCET to 1989/day 27/0000 SCET. This data gives scan plane angle distributions for those periods when the LECP instrument was mechanically scanning. There are periods when the instrument was not scanning, and the corresponding data does not appear here with this Step data. Another data set that is available, the so called Scan data, contains data for these not stepping periods as well as angle averaged data for the stepping periods. The instrument samples 8 directional sectors during a single scan, and thus this Step data contains 8 particle intensity numbers for each channel of data utilized (a ninth sector corresponds to accumulations for which the sector is unknown). Two scanning situations occurred during the time of this data. They are: 1) continuous 48 sec stepping (48 seconds for each of 8 look directions for a total of 6.4 minutes per scan; note that sector 8 is shielded with 2 mm Al), and 2) a special Uranus scan cyclic with the following sequence: 7, scan, scan, 7, scan, scan, repeat; where the 7 represents a 10.4 minute period when the instrument is fixed in sector 7, and where the word scan represents a period of scanning (6 sec stepping for a total scan time of 48 sec). For this Uranus Scan data the two adjacent scans within the Uranus scan cyclic (Mode 2 above) have been averaged together into a single, 96 sec record. The records of the 48 sec stepping mode (mode 1 above) are for 6.4 minutes. The schedule of mode changes is as follows: prior to day 24/ 0420 SCET: Mode (1) 24/0420 to 25/1357: Mode (2) after 25/1357: Mode (1) Please note that the change-over between modes is not instantaneous, and that for a few minutes the state of the scanning is not regular. Note also that there were brief interruptions to, and changes in time phase in, the mode (2) scan cyclic during the transitions into and out of the movable block period that bracketed the close approach position (not shown above). Obviously these stepping mode changes, and the angle sample switching that occurs during stepping mode (2), gives the data a disjointed appearance. The LECP channels utilized with this data set are: EB01: electrons, 22 to 35 keV EB02: electrons, 35 to 61 keV EB03: electrons, 61 to 112 keV EB04: electrons, 112 to 183 keV EG06-EG07: electrons, 252 to 480 keV EG07-EG08: electrons, 480 to 853 keV EG08-EG09: electrons, 853 to 1200 keV PL01: ions, 28 to 43 keV PL02: ions, 43 to 80 keV PL03: ions, 80 to 137 keV PL04: ions, 137 to 215 keV PL05: ions, 215 to 540 keV PL06: ions, 540 to 990 keV PL07: ions, 990 to 2140 keV PL08: ions, 2140 to 3500 keV Please note that 3 of the electron channels are derived from 4 of the instrumental channels by taking differences between adjacent (in energy) channels. The channel data is given in units of intensity: counts/(cm^2.sec.str.keV). For the ions, it has been assumed that they consist only of protons. Intensity is derived from the raw count rates via the relation: I = CR/(eG.(E2-E1), where eG is geometric factor times detector efficiency, and (E2-E1) is the band pass of the channel in energy. The proton values of these parameters were used in deriving the intensities for this data set. To obtain the Intensities under the assumption that some other mass species dominates, one must convert back to count rate (CR) utilizing the proton parameters, and then convert to intensity using the parameters corresponding to the mass species in question. The parameters can be found in Table 1 of Krimigis et al. (Journal of Geophysical Research, V. 86, page 8227, 1981). The corresponding parameters for electrons can be found in Mauk et al. (Journal of Geophysical Research, V. 92, page 15283, 1987). Prior to the conversion to intensity, the count rates have been corrected for: (1) Background, (2) electron contamination of the lower energy ion channels, and (3) solar UV contamination of the lowest energy ion channel. The uncertainty parameters given with the data associated with each channel (expressed as a percent) is the largest of the two quantities: (i) one standard deviation Poisson statistical error, and (ii) a percentage assigned by the data supplier based on the amount of contamination correction that has been performed on each data channel. Also supplied with each record of this data set is the fraction of the data accumulations that correspond to each of the 8 angle sectors. A sector 9 has also been defined corresponding to those accumulations with no known sector assignment. Additionally supplied for each data channel is a one bit code that tells whether that channel had any accumulations at all associated with it (1 = yes; 0 = no). This code must be used to distinguish between accumulations that yielded no counts and situations where the channel simply had no accumulations (results in Intensity = 0.0). Processing Level Id : 4 Software Flag : N Processing Start Time : 1991-07-24 Processing Stop Time : 1991-07-25 Parameters ========== Data Set Parameter 'PARTICLE FLUX INTENSITY' -------------------------------------------- The channel data is given in units of intensity: counts/(cm^2.sec.str.keV). For the ions, it has been assumed that they consist only of protons. Intensity is derived from the raw count rates via the relation: I = CR/(eG.(E2-E1), where eG is geometric factor times detector efficiency, and (E2-E1) is the band pass of the channel in energy. The proton values of these parameters were used in deriving the intensities for this data set. To obtain the Intensities under the assumption that some other mass species dominates, one must convert back to count rate (CR) utilizing the proton parameters, and then convert to intensity using the parameters corresponding to the mass species in question. The parameters can be found in Table 1 of Krimigis et al. (Journal of Geophysical Research, V. 86, page 8227, 1981). The corresponding parameters for electrons can be found in Mauk et al. (Journal of Geophysical Research, V. 92, page 15283, 1987). Prior to the conversion to intensity, the count rates have been corrected for: (1) Background, (2) electron contamination of the lower energy ion channels, and (3) solar UV contamination of the lowest energy ion channel. Sampling Parameter Name : TIME Data Set Parameter Name : PARTICLE FLUX INTENSITY Sampling Parameter Resolution : 768.000000 Sampling Parameter Interval : 768.000000 Minimum Available Sampling Int : 6.000000 Data Set Parameter Unit : COUNTS/(CM**2*SECOND*STERRADIAN*KEV) Sampling Parameter Unit : SECOND S Source Instrument Parameters ============================ Instrument Host ID : VG2 Data Set Parameter Name : PARTICLE FLUX INTENSITY Instrument Parameter Name : PARTICLE MULTIPLE PARAMETERS Important Instrument Parameters : 1 Processing ========== Processing History ----------------

5) VG2 URA LECP RESAMPLED SUMMARY SCAN AVERAGED 15MIN V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Uranus/PT15M
Start:1986-01-24 00:00:00 Observatory:Voyager 2 Cadence:15 minutes
Stop:1986-01-30 00:00:00 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
This browse data consists of resampled data from the Low Energy Charged Particle (LECP) experiment on Voyager 2 while the spacecraft was in the vicinity of Uranus. 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. For this browse data set only scan average data is given (no angular information). The data is in the form of 'rate' data which has not been converted to the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'rate' to 'intensity' for a particular channel one performs the following tasks: 1) decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 has a 2 MM al shield covering it). 2) divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. The geometric factor is found in entry 'CHANNEL_GEOMETRIC_FACTOR' as associated with each channel 'CHANNEL_ID'. To determine the energy bandpass, one must judge the mass species of the of the detected particles (for ions but not for electrons). The energy band passes are given in entries 'MINIMUM_INSTRUMENT_PARAMETER' and 'MAXIMUM_INSTRUMENT_PARAMETER' in table 'FPLECPENERGY', and are given in the form 'ENERGY/NUCLEON'. For channels that begin their names with the designations 'CH' these bandpasses can be used on mass species that are accepted into that channel (see entries 'MINIMUM_INSTRUMENT_PARAMETER' and 'MAXIMUM_INSTRUMENT_ PARAMETER' in table 'FPLECPCHANZ', which give the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The bandpasses for other 'Z' values are not all known, but some are given in the literature (e.g. Krimigis et al., 1979). The final product of these instructions will be the particle intensity with the units: counts/(cm**2.str.sec.keV). Some channels are subject to serious contaminations, and many of these contaminations cannot be removed except with a region-by-region analysis, which has not been done for this data. Thus, to use this data it is absolutely vital that the contamination types ('CONTAMINATION_ID' , 'CONTAMINATION_DESC') and the levels of contamination ('DATA_QUALITY_ID' corresponding to the definitions 'DATA_QUALITY_DESC') be carefully examined for all regions of study. A dead time correction procedure has been applied in an attempt to correct the linear effects of detector overdrive (Pulse-Pileup). This procedure does not fix severely overdriven detectors. A procedure is available for correcting Voyager 2 LECP electron contamination of low energy ion channels, but its effectiveness has been evaluated only for the Uranus data set. Thus, corrections have been applied only to the Uranus data set. Processing Level Id : 4 Software Flag : Y Processing Start Time : 1987-02-01 Parameters ========== Data Set Parameter 'ELECTRON RATE' ---------------------------------- 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). 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 Data Set Parameter 'ION RATE' ----------------------------- 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). Data Set Parameter Name : ION RATE Data Set Parameter Unit : COUNTS/SECOND Sam

6) VG2 URA LECP RESAMPLED SUMMARY SCAN AVERAGED 24SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Uranus/PT24S
Start:1989-01-24 00:00:00 Observatory:Voyager 2 Cadence:24 seconds
Stop:1989-01-27 00:00:00 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
This data consists of resampled data from the Low Energy Charged Particle (LECP) Experiment on the Voyager 2 Spacecraft for the period when Voyager 2 was in the vicinity of the planet Uranus. The period covered is 1986/day 24/0000 SCET to 1986/day 27/0000 SCET. This data approximates a time series of charged particle fluxes from a selection of channels available from the instrument. The word approximates is used because the angle scanning modes of the instrument complicates the nature of the data. At times the instrument mechanically scans, and at times it is fixed to look at a specific direction. With the type of data given here, the fluxes are angle averaged for those time periods when the instrument is scanning, and are time averaged over an arbitrary period (24 seconds) for the periods when the detectors are stationary. The angle averaged records represent periods of time equal to 96 or 384 sec (see below). This kind of data presentation has been called the LECP Scan data. Another form that is also available is the LECP Step data that gives the angle distributions sampled during the scanning periods. Two scanning situations occurred during the time of this data. They are: 1) continuous 48 sec stepping (48 seconds for each of 8 look directions for a total of 6.4 minutes per scan; note that sector 8 is shielded with 2 mm Al), and 2) a special Uranus scan cyclic with the following sequence: 7, scan, scan, 7, scan, scan, repeat; where the 7 represents a 10.4 minute period when the instrument is fixed in sector 7, and where the word scan represents a period of scanning (6 sec stepping for a total scan time of 48 sec). For this Uranus Scan data the two adjacent scans within the Uranus scan cyclic have been averaged together into a single, 96 sec record. The records of the 48 sec stepping mode (Mode 1 above) are for 6.4 minutes. As stated in the first paragraph, the records for the periods of no stepping during the Uranus scan cyclic (mode 2 above) are for 24 sec periods. The schedule of mode changes is as follows: prior to day 24/0420: Mode (1) 24/0420 to 25/ 1357: Mode (2) after day 25/1357: Mode (1) Please note that the change-over between modes is not instantaneous, and that for a few minutes the state of the scanning is not regular. Not also that there were brief interruptions to, and changes in time phase in, the Mode (2) scan cyclic during the transitions into and out of the movable block periods that bracketed the close approach position (not shown above). Obviously these stepping mode changes, and the angle sample switching that occurs during stepping mode (2), gives the data a disjointed appearance. The LECP channels utilized with this data set are: EB01: electrons, 22 to 35 keV EB02: electrons, 35 to 61 keV EB03: electrons, 61 to 112 keV EB04: electrons, 112 to 183 keV EG06-EG07: electrons, 252 to 480 keV EG07-EG08: electrons, 480 to 853 keV EG08-EG09: electrons, 853 to 1200 keV PL01: ions, 28 to 43 keV PL02: ions, 43 to 80 keV PL03: ions, 80 to 137 keV PL04: ions, 137 to 215 keV PL05: ions, 215 to 540 keV PL06: ions, 540 to 990 keV PL07: ions, 990 to 2140 keV PL08: ions, 2140 to 3500 keV Please note that 3 of the electron channels are derived from 4 of the instrumental channels by taking differences between adjacent (in energy) channels. The channel data is given in units of intensity: counts/(cm^2.sec.str.keV). For the ions, it has been assumed that they consist only of protons. Intensity is derived from the raw count rates via the relation: I = CR/(eG.(E2-E1), where eG is geometric factor times detector efficiency, and (E2-E1) is the band pass of the channel in energy. The proton values of these parameters were used in deriving the intensities for this data set. To obtain the Intensities under the assumption that some other mass species dominates, one must convert back to count rate (CR) utilizing the proton parameters, and then convert to intensity using the parameters corresponding to the mass species in question. The parameters can be found in Table 1 of Krimigis et al. (Journal of Geophysical Research, V. 86, page 8227, 1981). The corresponding parameters for electrons can be found in Mauk et al. (Journal of Geophysical Research, V. 92, page 15283, 1987). Prior to the conversion to intensity, the count rates have been corrected for: (1) Background, (2) electron contamination of the lower energy ion channels, and (3) solar UV contamination of the lowest energy ion channel. The uncertainty parameters given with the data associated with each channel (expressed as a percent) is the largest of the two quantities

7) VG2 LECP 6.4 MINUTE URANUS FAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Uranus/PT6M24S
Start:1986-01-19 01:36:24 Observatory:Voyager 2 Cadence:6 minutes; 24 seconds
Stop:1986-02-07 05:55:17 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 2 while the spacecraft was within the vicinity of Uranus. This instrument measures the intensities of in-situ charged particles ( >13 keV electrons and >24 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 Uranus 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 2 LECP CH CH LOW HIGH MEAN GEOMETRIC CH Num NAME (MeV/N) (MeV/N) (Mev/N) FACTOR LOGIC cm**2 sr DEFINITIN -------------------------------------------------------- 1 EB01 0.013 0.035 0.020 0.00200 2 EBD1 0.013 0.035 0.020 0.00200 3 EB02 0.035 0.061 0.045 0.00200 4 EBD2 0.035 0.061 0.045 0.00200 5 EB03 0.061 0.112 0.090 0.00200 6 EBD3 0.061 0.112 0.090 0.00200 7 EB04 0.112 0.183 0.120 0.00200 8 EBD4 0.112 0.183 0.120 0.00200 9 EB05 0.183 0.500 0.200 0.00200 10 EBD5 0.183 0.500 0.200 0.00200 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 2.000 100.000 2.000 1.31000 17 E37 6.000 100.000 6.000 1.31000 18 PL01 0.024 0.048 0.025 0.12000 19 PL02 0.048 0.080 0.050 0.12000 20 PL03 0.080 0.137 0.100 0.12000 21 PL04 0.137 0.215 0.150 0.12000 22 PL05 0.215 0.540 0.250 0.12000 23 PL06 0.540 0.990 0.600 0.12000 24 PL07 0.990 2.140 1.000 0.12000 25 PL08 2.140 3.500 2.500 0.12000 26 P32 0.330 0.610 0.350 0.09750 E0E2(E3) 27 P1 0.520 1.450 0.600 0.44100 E1E2(E3) 28 P10 4.400 11.400 5.000 0.53900 E2E3(E4) 29 P11 11.400 20.000 12.000 0.53900 E2E3(E4) 30 P16 3.040 17.000 5.000 1.50000 E5E4(E3) 31 P23 22.000 30.000 25.000 1.31000 E5E4E3(E2) 32 P27 37.000 89.000 50.000 1.20000 E5E4E3E2 33 P31 213.000 1000.000 250.000 1.31000 E4E3 34 A39 0.091 0.233 0.100 0.09750 E0(E2) 35 A33 0.230 0.480 0.350 0.09750 E0E2(E3) 36 A46 0.147 2.000 0.600 0.44100 'D1F1,CA' 37 A3 0.420 1.700 0.600 0.44100 E1E2(E3) 38 A4 1.800 4.000 2.500 0.44100 E1E2(E3L12) 39 A12 4.200 7.800 5.000 0.53900 E2E3(E4L23) 40 A13 7.800 20.000 15.000 0.53900 E2E3(E4L23) 41 A17 3.000 58.000 5.000 1.50000 E5E4(E3L54) 42 A24 22.000 30.000 25.000 1.31000 E5E4E3(E2) 43 A28 31.000 56.000 50.000 1.20000 E5E4E3E2 44 AL01 1.040 1.850 1.000 0.12000 CALC. 45 AL02 1.850 3.700 2.500 0.12000 CALC. 46 M34 0.230 0.440 0.200 0.09750 E0E2 47 L5 0.710 5.600 1.500 0.44100 E1E2(E3L12) 48 L14 5.800 28.000 6.000 0.53900 E2E3(E4L23) 49 L18 3.900 20.000 5.000 1.50000 E5E4(E3L54) 50 M38 0.060 0.200 0.100 0.09750 E0(E2) 51 M35 0.200 0.340 0.250 0.09750 E0E2(E3) 52 M47 0.124 14.300 0.250 0.44100 D1F2 53 M6 0.470 5.200 0.500 0.44100 E1E2(E3L12) 54 M7 5.200 8.200 6.000 0.44100 E1E2(E3L12) 55 M15 8.600 40.000 15.000 0.53900 E2E3(E4L23) 56 M19 6.000 9.200 6.000 1.50000 E5E4(E3L54) 57 M20 9.600 42.000 15.000 1.50000 E5E4(E3L54) 58 M25 44.000 61.000 50.000 1.31000 E5E4E3(E2) 59 M29 69.000 270.000 70.000 1.20000 E5E4E3E2 60 H36 0.099 0.140 0.100 0.09750 E0(E2) 61 H8 0.280 1.900 0.350 0.44100 E1E2(E3) 62 H9 2.000 12.000 2.000 0.44100 E1E2(E3)

8) VG2 URA MAG RESAMPLED RDR U1 COORDINATES 1.92SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/MAG/Uranus/PT1.92S
Start:1986-01-24 07:00:00 Observatory:Voyager 2 Cadence:1.92 seconds
Stop:1986-01-25 03:59:58 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
This data set includes data from the Low Field Magnetometer (LFM) in the solar wind during the Uranus encounter. The encounter data (1986-01-24T07:00:00 -> 1986-01-25T04:00:00) have been averaged from the 60ms instrument sample rate to a 1.92 second resampled rate and are provided in the Uranus Longitude (U1) coordinate system. Magnetometer data in the solar wind are given in Heliographic coordinates and are also available in a separate dataset. The dataset consists of the following columns: 1) ctime (decimal seconds since 1966-01-01T00:00:00.000), 2) pdstime (ISO standard time format), 3-5) spacecraft clock (m65536,m60,fds-line), 6) magnetometer id (1 = LFM, 2 = HFM), 7) Br (radial component), 8) Bphi (longitudinal component), 9) Btheta (colatitudinal component), 10) Bmag (magnitude of the average components), 11) avg_Bmag (average of the magnitude of the raw components), 12) Lambda (longitude = tan^-1(Bt/Br)), 13) Delta (latitude = sin^-1(Bn/avg_Bmag) ), 14-16) rms vector (Pythagorean root mean square deviation of the component averages), 17) npts (number of points in average), 18) flag a character string which indicates software or s/c hardware intervention which reduces confidence in the data (NULL flags represent 'good' data). The U1 coordinate system is a non-inertial spherical coordinate system that rotates with Uranus with a period of 17.24 hours. The system components are: R - Radial along the Uranus-S/C line, positive away from Uranus, Phi - east longitudinal component, Theta - colatitudinal component. An ancillary data file containing the derived spacecraft magnetic field is provided with this data at a 48 second sample rate. These data provide zero level offsets used in the data processing. S/C field data is provided in spacecraft coordinates. SAMPLING_PARAMETER_NAME = TIME 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 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = MAGNETIC FIELD VECTOR NOISE_LEVEL = 0.006000 DATA_SET_PARAMETER_UNIT = NANOTESLA

9) VG2 URA MAG RESAMPLED SUMMARY U1 COORDINATES 48SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/MAG/Uranus/PT48S
Start:1986-01-24 07:00:00 Observatory:Voyager 2 Cadence:48 seconds
Stop:1986-01-25 03:59:58 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
This data set includes data from the Low Field Magnetometer (LFM) in the during the Uranus encounter. The encounter data (1986-01-24T07:00:00 -> 1986-01-25T04:00:00) have been averaged from the 9.6 second averages to a 48 second resampled rate and are provided in the Uranus Longitude (U1) coordinate system. Magnetometer data in the solar wind are given in Heliographic coordinates and are also available in a separate dataset. The dataset consists of the following columns: 1) ctime (decimal seconds since 1966-01-01T00:00:00.000), 2) pdstime (ISO standard time format), 3-5) spacecraft clock (m65536,m60,fds-line), 6) magnetometer id (1 = LFM, 2 = HFM), 7) Br (radial component), 8) Bphi (longitudinal component), 9) Btheta (colatitudinal component), 10) Bmag (magnitude of the average components), 11) avg_Bmag (average of the magnitude of the raw components), 12) Lambda (longitude = tan^-1(Bt/Br)), 13) Delta (latitude = sin^-1(Bn/avg_Bmag) ), 14-16) rms vector (Pythagorean root mean square deviation of the component averages), 17) npts (number of points in average), 18) flag a character string which indicates software or s/c hardware intervention which reduces confidence in the data (NULL flags represent 'good' data). The U1 coordinate system is a non-inertial spherical coordinate system that rotates with Uranus with a period of 17.24 hours. The system components are: R - Radial along the Uranus-S/C line, positive away from Uranus, Phi - east longitudinal component, Theta - colatitudinal component. An ancillary data file containing the derived spacecraft magnetic field is provided with this data at a 48 second sample rate. These data provide zero level offsets used in the data processing. S/C field data is provided in spacecraft coordinates. SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 48.0 MINIMUM_SAMPLING_PARAMETER = 19770820120000.000000 MAXIMUM_SAMPLING_PARAMETER = UNK SAMPLING_PARAMETER_INTERVAL = 48.0 MINIMUM_AVAILABLE_SAMPLING_INT = 0.060000 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = MAGNETIC FIELD VECTOR NOISE_LEVEL = 0.006000 DATA_SET_PARAMETER_UNIT = NANOTESLA

10) VG2 URA MAG RESAMPLED RDR U1 COORDINATES 9.6SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/MAG/Uranus/PT9.6S
Start:1986-01-24 07:00:00 Observatory:Voyager 2 Cadence:9.6 seconds
Stop:1986-01-25 03:59:58 Instrument:Triaxial Fluxgate Magnetometer (MAG) Resource:NumericalData
This data set includes data from the Low Field Magnetometer (LFM) in the solar wind during the Uranus encounter. The encounter data (1986-01-24T07:00:00 -> 1986-01-25T04:00:00) have been averaged from the 1.92 second averaged data to a 9.6 second resampled rate and are provided in the Uranus Longitude (U1) coordinate system. Magnetometer data in the solar wind are given in Heliographic coordinates and are also available in a separate dataset. The dataset consists of the following columns: 1) ctime (decimal seconds since 1966-01-01T00:00:00.000), 2) pdstime (ISO standard time format), 3-5) spacecraft clock (m65536,m60,fds-line), 6) magnetometer id (1 = LFM, 2 = HFM), 7) Br (radial component), 8) Bphi (longitudinal component), 9) Btheta (colatitudinal component), 10) Bmag (magnitude of the average components), 11) avg_Bmag (average of the magnitude of the raw components), 12) Lambda (longitude = tan^-1(Bt/Br)), 13) Delta (latitude = sin^-1(Bn/avg_Bmag) ), 14-16) rms vector (Pythagorean root mean square deviation of the component averages), 17) npts (number of points in average), 18) flag a character string which indicates software or s/c hardware intervention which reduces confidence in the data (NULL flags represent 'good' data). The U1 coordinate system is a non-inertial spherical coordinate system that rotates with Uranus with a period of 17.24 hours. The system components are: R - Radial along the Uranus-S/C line, positive away from Uranus, Phi - east longitudinal component, Theta - colatitudinal component. An ancillary data file containing the derived spacecraft magnetic field is provided with this data at a 48 second sample rate. These data provide zero level offsets used in the data processing. S/C field data is provided in spacecraft coordinates. SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 9.6 MINIMUM_SAMPLING_PARAMETER = 19770820120000.000000 MAXIMUM_SAMPLING_PARAMETER = UNK SAMPLING_PARAMETER_INTERVAL = 9.6 MINIMUM_AVAILABLE_SAMPLING_INT = 0.060000 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = MAGNETIC FIELD VECTOR NOISE_LEVEL = 0.006000 DATA_SET_PARAMETER_UNIT = NANOTESLA

11) VG2 URA PLS DERIVED SUMMARY ION FIT 48SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/PLS/Uranus/PT48S
Start:1986-01-24 15:01:48 Observatory:Voyager 2 Cadence:48 seconds
Stop:1986-01-24 19:55:24 Instrument:Plasma Spectrometer (PLS) Resource:NumericalData
This data set contains the total ion density obtained from Voyager 2 PLS data (voltage range 10-5950 eV/Q) at Uranus by fitting the measured spectra with isotropic Maxwellian distributions. It is a subset of the data set VG2-U-PLS-5-RDR-IONFIT-48SEC. Up to three isotropic proton components (warm, hot and intermediate) were used to match the observations. These were then summed to give total ion density. This determination does not include possible plasma outside the PLS energy range; limits on a cold component can be derived in the charging region from 1939-2158 on day 24. It is found that if a cold component exists it will increase the total ion density by at most a factor of two. uncertainties in plasma parameters are a factor of 2 in the charging region, less than 20% elsewhere. A complete description of this data set is given in McNutt et al. (1987) and Selesnick and McNutt (1987). Data format: first six columns are time tags (6I4), last column is total ion density in CM-3 (E11.3). Values of 1.E32 indicate that the parameter could not be obtained from the data using the standard analysis technique. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in McNutt et al. (1987) and Selesnick and McNutt (1987) and a complete instrument description can be found in Bridge (1977). SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = N/A MAXIMUM_SAMPLING_PARAMETER = N/A SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 24.000000 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = ION DENSITY NOISE_LEVEL = N/A DATA_SET_PARAMETER_UNIT = CM-3 SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = N/A MAXIMUM_SAMPLING_PARAMETER = N/A SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 24.000000 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = ION THERMAL SPEED NOISE_LEVEL = N/A DATA_SET_PARAMETER_UNIT = KM/S

12) VG2 URA PRA EDITED RDR HIGH RATE 60MS V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/PRA/Uranus/PT0.60S
Start:1985-10-24 23:23:12 Observatory:Voyager 2 Cadence:0.60 seconds
Stop:1988-07-14 07:43:09 Instrument:Voyager 2 Planetary Radio Astronomy (PRA) experiment Resource:NumericalData
This data set (VG2-U-PRA-2-RDR-HIGHRATE-60MS-V1.0) contains data acquired by the Voyager-2 Planetary Radio Astronomy (PRA) instrument during the Uranus 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 Uranus Encounter Phase (1985-10-24 to 1988-07-14). Each file within the dataset represents a single PRA high rate frame, of duration 48 seconds. Each file contains a 28 octet header, followed by 1280000 octets of data. The header format is described as below: -------------------------------------------------------------------- Length (bytes) Name Contents -------------------------------------------------------------------- 2 Year Year A.D. 2 Day Day of year (1 Jan == 1) 1 Hour Hour of day (midnight == 0) 1 Minute Minute of hour (o'clock = 0) 1 Second Second of Minute (exact minute == 0) 1 Spacecraft 1 == V1, 2 == V2 2 Integral FDS Integer part of FDS count 1 Fractional FDS Fractional part of FDS count 4 Freq. 1 Frequency of 1st channel (Hz) 4 Freq. 2 Frequency of 2nd channel (Hz) 4 Freq. 3 Frequency of 3rd channel (Hz) 4 Freq. 4 Frequency of 4th channel (Hz) 1 Bandwidth Bandwidth (kHz) -------------------------------------------------------------------- where all values are unsigned, and multi-octet values are presented with the most significant byte first. The data are 16 bit numbers, most significant byte first, with 0 indicating unavailable data. The data are presented as a single stream of 16 bit numbers. The frame is logically divided into lines (although there is no indication of the lines within the file). This terminology comes from the fact that in this high rate mode, the PRA data are treated exactly as if they were imaging data, and a 48 second image comprises 800 horizontal scan lines. Similarly, there are 800 logical lines within a PRA frame. Each line comprises 800 values, representing 400 data pairs. In the high rate mode, the PRA measures the flux at two frequencies _simultaneously_ and returns these two data sequentially. A sample pair is acquired every (actually every 138.88... microseconds), through an RC filter with a 100 microsecond time constant. A single line comprises 60 milliseconds of data. Lines are NOT contiguous in time. There is a 4444.44... microsecond gap between the ending of one line and the start of the succeeding line. The PRA samples a frequency pair in this manner for 24 seconds. It then has the option of switching to a second pair for the final 24 seconds. These frequencies are designated Freq. 1 through Freq. 4 in the header. The data are presented such that the higher of the relevant frequency pair is presented first. SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = N/A MINIMUM_SAMPLING_PARAMETER = N/A MAXIMUM_SAMPLING_PARAMETER = N/A SAMPLING_PARAMETER_INTERVAL = 138.8 MINIMUM_AVAILABLE_SAMPLING_INT = 138.8 SAMPLING_PARAMETER_UNIT = MICROSECOND DATA_SET_PARAMETER_NAME = RADIO WAVE SPECTRUM NOISE_LEVEL = 2400 DATA_SET_PARAMETER_UNIT = MILLIBEL

13) VG2 URA PRA RESAMPLED SUMMARY BROWSE 48SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/PRA/Uranus/PT48S
Start:1986-01-19 00:00:00 Observatory:Voyager 2 Cadence:48 seconds
Stop:1986-01-31 23:59:59 Instrument:Voyager 2 Planetary Radio Astronomy (PRA) experiment Resource:NumericalData
This dataset consists of edited browse data derived from an original dataset obtained from the Voyager 2 Planetary Radio Astronomy (PRA) instrument in the vicinity of Uranus. Data are provided for 70 instrument channels covering the range from 1.2 kHz to 1326 kHz in uniform 19.2 kHz steps, each 1 kHz wide. Data are included for the period 1986:019:00:00 through 1986:031:23:59. In order to produce this dataset from the original raw PRA data, several steps have been taken: 1. The PRA operates in a variety of modes; data from modes in which the receiver does not scan rapidly through its frequency range have been removed; 2. The data have been calibrated as best we know how; 3. The data have been split into Left Hand Circular (LHC) and Right Hand Circular (RHC) components; 4. The data have been binned into 48-second intervals. Thus, values at a given channel are separated in time by an increment of 48 seconds; each 48-second time interval has associated with it a value for LHC polarization and one for RHC polarization. During data gaps, the entire record is absent from the dataset; that is, missing records have not been zero-filled or otherwise marked. Bad data within a record is indicated by the value zero, which cannot otherwise occur. Each datum is returned as a 16-bit quantity; it represents the mean power received in the given channel at the specified time and polarization. The returned quantity is the value in milliBels (mB) about a reference flux density. The value of 0 mB represents a voltage of 1 microvolt across the front end of the receiver. To convert a returned quantity to flux, use the formula: flux = 7.0x10^(-22)x10^(Mb/1000) W m-2 Hz-1

14) N/A maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/PRA/Uranus/PT6S
Start:1986-01-19 00:00:00 Observatory:Voyager 2 Cadence:6 seconds
Stop:1986-01-31 00:00:00 Instrument:Voyager 2 Planetary Radio Astronomy (PRA) experiment Resource:NumericalData
Voyager 2 PRA lowband 6 second data recorded at Uranus.

15) VG2 URA PWS RAW EXPERIMENT WAVEFORM 60MS V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/PWS/Uranus/PT0.60S
Start:1985-11-08 07:04:08 Observatory:Voyager 2 Cadence:0.60 seconds
Stop:1986-02-22 20:41:34 Instrument:Plasma Wave System (PWS) Resource:NumericalData
This data set consists of electric field waveform samples from the Voyager 2 Plasma Wave Receiver waveform receiver obtained during the Uranus encounter. The waveforms are collections of 4-bit samples of the electric field measured by the dipole electric antenna at a rate of 28,800 samples per second. 1600 samples are collected in 55.56 msec followed by a 4.44-msec gap. Each 60-msec interval constitutes a line of waveform samples. The data set includes about 271 frames of waveform samples consisting of up to 800 lines, each. The telemetry format for the waveform data is identical to that for images, hence the use of line and frame as constructs in describing the form of the data. The waveform is sampled through a bandpass filter with a passband of 40 Hz to 12 kHz. The 4-bit samples provide sixteen digital values of the electric field with a linear amplitude scale, but the amplitude scale is arbitrary because of the automatic gain control used in the waveform receiver. The instantaneous dynamic range afforded by the 4 bit samples is about 23 db, but the automatic gain control allows the dominant signal in the passband to be set at the optimum level to fit within the instantaneous dynamic range. With the gain control, the overall dynamic range of the waveform receiver is about 100 db. The automatic gain control gain setting is not returned to the ground, hence, there is no absolute calibration for the data. However, by comparing the waveform spectrum derived by Fourier transforming the waveform to the spectrum provided by the spectrum analyzer data, an absolute calibration may be obtained in most cases. The data may be plotted in raw form to show the actual waveform; this is useful for studying events such as dust impacts on the spacecraft. But the normal method of analyzing the waveform data is by Fourier transforming the samples from each line to arrive at an amplitude versus frequency spectrum. By stacking the spectra side-by-side in time order, a frequency- time spectrogram can be produced. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Gurnett et al. [1986] and a complete instrument description can be found in Scarf and Gurnett [1977]. SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 0.000034722 MINIMUM_SAMPLING_PARAMETER = N/A MAXIMUM_SAMPLING_PARAMETER = N/A SAMPLING_PARAMETER_INTERVAL = 0.000034722 MINIMUM_AVAILABLE_SAMPLING_INT = 0.000034722 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = PLASMA WAVE WAVEFORM NOISE_LEVEL = 0.000005 DATA_SET_PARAMETER_UNIT = VOLT/METER (Data not absolutely calibrated)

16) VG2 URA PWS RESAMPLED SUMMARY SPECTRUM ANALYZER 48SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/PWS/Uranus/PT48S
Start:1986-01-23 00:00:00 Observatory:Voyager 2 Cadence:48 seconds
Stop:1986-01-31 00:00:00 Instrument:Plasma Wave System (PWS) Resource:NumericalData
This data set consists of 48-second calibrated, averaged wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Uranian magnetosphere. For each 48-second interval, a geometric average field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kilo- Hertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of averages is the beginning of the 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 dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Gurnett et al. [1986] and a complete instrument description can be found in Scarf and Gurnett [1977]. SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 48.000000 MINIMUM_SAMPLING_PARAMETER = 197708201553.000000 MAXIMUM_SAMPLING_PARAMETER = N/A SAMPLING_PARAMETER_INTERVAL = 48.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 4.000000 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = PLASMA WAVE SPECTRUM NOISE_LEVEL = 0.000005 DATA_SET_PARAMETER_UNIT = VOLT/METER

17) VG2 URA PWS EDITED RDR UNCALIB SPECTRUM ANALYZER 4SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/PWS/Uranus/PT4S
Start:1986-01-23 00:00:00 Observatory:Voyager 2 Cadence:4 seconds
Stop:1986-01-31 00:00:00 Instrument:Plasma Wave System (PWS) Resource:NumericalData
This data set consists of 4-second edited, wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Uranian 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 tables are given in two plain ASCII text files named VG1PWSCL.TAB and VG2PWSCL.TAB (for Voyagers-1 and -2, respectively). These provide 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. 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 2 PWS: real*4 cal (16,0:255) open ( unit=10, file='vg2pwscl.tab', status='old' ) do i=0,38 read (10,*) ! skip 38 lines of label info end do 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, 7.07m. 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 2 PWS are given below: VOYAGER 2 PWS SPECTRUM ANALYZER Voyager-2 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 5 100. Hz 13.8 Hz 6 178. Hz 28.8 Hz 7 311. Hz 39.8 Hz 8 562. Hz 75.9 Hz 9 1.00 kHz 75.9 Hz 10 1.78 kHz 151. Hz 11 3.11 kHz 324. Hz 12 5.62 kHz 513. Hz 13 10.0 kHz 832. Hz 14 17.8 kHz 1260. Hz 15 31.1 kHz 2400. Hz 16 56.2 kHz 3800. Hz A failure in the Voyager 2 Flight Data System which occurred about 3 months after launch has adversely affected the calibration of PWS channels 9 through 16. An algorithm has been devised to partially correct for this failure, and has proven useful for Voyager 2 Jupiter, Saturn, and Uranus encounters, but is not valid for Earth-Jupiter cruise and may be modified in the future. The following implementation of this correction algorithm in VAX FORTRAN assumes that uncalibrated data numbers are stored in a 16-element integer array, idn, with the array index equal to the PWS channel number: real*4 tonl(9:16) ! the old noise level for v2 data tonl/2.0,1.0,-1.0,-2.0,-3.0,1.0,2.0,1.0/ do ichan=9,16 if (idn(ichan).gt.0) then if(idn(ichan).lt.64) idn(ichan)=64 if (idn(ichan).le.72) then idn(ichan)=int(tonl(ichan)-530.4+8.6 *real(idn(ichan))) else idn(ichan)=int(tonl(ichan)+20.113+0.99 *real(idn(ichan))) end if end if end do This correction should not be applied permanently to the Voyager 2 calibration table since it is valid for a limited time span and may be modified in the future. Additional information about this dataset and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in Gurnett et al. [1986] and a complete instrument description can be found in Scarf and Gurnett [1977]. SAMPLING_PARAMETER_NAME = TIME SAMPLING_PARAMETER_RESOLUTION = 4.000000 MINIMUM_SAMPLING_PARAMETER = 197708201553.000000 MAXIMUM_SAMPLING_PARAMETER = N/A SAMPLING_PARAMETER_INTERVAL = 4.000000 MINIMUM_AVAILABLE_SAMPLING_INT = 4.000000 SAMPLING_PARAMETER_UNIT = SECOND DATA_SET_PARAMETER_NAME = PLASMA WAVE SPECTRUM NOISE_LEVEL = 0.000005 DATA_SET_PARAMETER_UNIT = VOLT/METER

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