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1) Voyager-2 CRS Cruise Mode daily averages maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/CRS/FLUX/P1D
Start:1977-08-24 00:00:00 Observatory:Voyager 2 Cadence:1 day
Stop:2012-08-19 00:00:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
daily averages of selected fluxes

2) Voyager-2 CRS Cruise Mode 15-minute averages maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/CRS/FLUX/PT15M
Start:1977-08-24 00:00:00 Observatory:Voyager 2 Cadence:15 minutes
Stop:2012-08-19 00:00:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
15-minute averages of selected fluxes

3) Voyager 2 CRS Cruise Mode 6-hour averages maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/CRS/FLUX/PT6H
Start:1977-08-22 00:00:00 Observatory:Voyager 2 Cadence:6 hours
Stop:2011-10-01 00:00:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
6-hour averages of selected fluxes

4) VG2 JUP CRS DERIVED PROTON/ION/ELECTRON FLUX BROWSE V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/CRS/Jupiter/PT15S
Start:1979-07-03 00:00:00 Observatory:Voyager 2 Cadence:15 seconds
Stop:1979-08-03 23:45:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
Data Set Overview ================= Instrument P.I. : Rochus E. Vogt Data Supplier : National Space Science Data Center Data sampling rate : variable (1 hr for FPHA data, 15 min. for all others) Data Set Start Time : 1979-07-03T00:00:00.000Z Data Set Stop Time : 1979-08-03T23:45:00.000Z (The following description has been excerpted from [NSSDCCRS1979]) As its name implies, the Cosmic Ray Subsystem (CRS) was designed for cosmic ray studies [STONEETAL1977B]. It consists of two high Energy Telescopes (HET), four Low Energy Telescopes (LET) and The Electron Telescope (TET). The detectors have large geometric factors (~ 0.48 to 8 cm^2 ster) and long electronic time constants (~ 24 [micro]sec) for low power consumption and good stability. Normally, the data are primarily derived from comprehensive ([Delta]E[1], [Delta]E[2] and E) pulse-height information about individual events. Because of the high particle fluxes encountered at Jupiter and Saturn, greater reliance had to be placed on counting rates in single detectors and various coincidence rates. In inter- planetary space, guard counters are placed in anticoincidence with the primary detectors to reduce the background from high-energy particles penetrating through the sides of the telescopes. These guard counters were turned off in the Jovian magnetosphere when the accidental anticoincidence rate became high enough to block a substantial fraction of the desired counts. Fortunately, under these conditions the spectra were sufficiently soft that the background, due to penetrating particles, was small. The data on proton and ion fluxes at Jupiter were obtained with the LET. The thicknesses of individual solid-state detectors in the LET and their trigger thresholds were chosen such that, even in the Jovian magnetosphere, electrons made, at most, a very minor contribution to the proton counting rates [LUPTON&STONE1972]. Dead time corrections and accidental coincidences were small (< 20%) throughout most of the magnetotail, but were substantial (> 50%) at flux maxima within 40 R[J] Of Jupiter. Data have been included in this package for those periods when the corrections are less than ~ 50% and can be corrected by the user with the dead time appropriate to the detector (2 to 25 [micro]sec). The high counting rates, however, caused some baseline shift which may have raised proton thresholds significantly. In the inner magnetosphere, the L[2] counting rate was still useful because it never rolled over. This rate is due to 1.8- to 13-MeV protons penetrating L[1] (0.43 cm^2 ster) and > 9-MeV protons penetrating the shield (8.4 cm^2 ster). For an E^-2 spectrum, the two groups would make comparable contributions; but in the magnetosphere, for the E^-3 to E^-4 spectrum above 2.5 MeV [MCDONALDETAL1979], the contribution from protons penetrating the shield would be only 3 to 14%. The LET L[1]L[2]L[4] and L[1]L[2]L[3] coincidence- anticoincidence rates give the proton flux between 1.8 and 8 MeV and 3 to 8 MeV with a small alpha particle contribution (~10^-3). Corrections are required for dead time losses in L[1], accidental L[1]L[2] coincidences and anticoincidence losses from L[4]. Data are given only for periods when these corrections are relatively small. In addition to the rates listed in the table, the energy lost in detectors L[1], L[2] and L[3] was measured for individual particles. For protons, this covered the energy range from 0.42 to 8.3 MeV. Protons can be identified positively by the [Delta]E vs. E technique, their spectra obtained and accidental coincidences greatly reduced. Because of telemetry limitations, however, only a small fraction of the events could be transmitted, and statistics become poor unless pulse-height data are averaged over a period of one hour. HET and LET detectors share the same data lines and pulse- height analyzers; thus, the telescopes can interfere with one another during periods of high counting rates. To prevent such an interference and explore different coincidence conditions, the experiment was cycled through four operating modes, each 192 seconds long. Either the HETs or the LETs were turned on at a time. LET-D was cycled through L[1] only and L[1]L[2] coincidence requirements. The TET was cycled through various coincidence conditions, including singles from the front detectors. At the expense of some time resolution, this procedure permitted us to obtain significant data in the outer magnetosphere and excellent data during the long passage through the magnetotail region. Some of the published results from this experiment required extensive corrections for dead time, accidental coincidences and anticoincidences ([VOGTETAL1979A], [VOGTETAL1979B]; [SCHARDTETAL1981]; [GEHRELS1981]). These corrections can be applied only on a case-by-case basis after a careful study of the environment and many self-consistency checks. They cannot be applied on a systematic basis and we have no computer programs to do so; therefore, data from such periods are not included in the Data Center submission. The scientists on the CRS team will, however, be glad to consider special requests if the desired information can be extracted from the data. Description of the Data

5) VG2 NEP CRS CALIB RDR D1 RATE HI RESOLUTION ELEC 6SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/CRS/Neptune/PT6S
Start:1989-08-25 05:08:50 Observatory:Voyager 2 Cadence:6 seconds
Stop:1989-08-25 05:21:02 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
Data Set Overview ================= This data set describes the data of the high time resolution counting rate from the D1 detector in the Cosmic Ray System (CRS) electron telescope (TET) on Voyager 2 during the Neptune encounter. The D1 detector nominally responds to electrons with kinetic energies above approximately 1 MeV (see detector description for details). Parameters ========== Sampling parameter name : time Sampling parameter resolution : 6.0 seconds Minimum sampling parameter : n/a Maximum sampling parameter : n/a Sampling parameter interval : 6.0 seconds Minimum available sampling interval : 6.0 seconds Data set parameter name : D1 rate Noise level : 0.000 counts/second Data set parameter unit : counts/second The D1 rate is the counting rate from the D1 detector of the Cosmic Ray System (CRS) electron telescope (TET). When the rate is above background it is approximately proportional to the omnidirectional flux of electrons with kinetic energy greater than ~1 MeV. To obtain an accurate flux the D1 calibration tables should be used (see below). When the rate is near background, the background rate should be subtracted. The background rate is due to gamma rays generated in the spacecraft RTG and to penetrating cosmic rays. It varies slightly with time on the time scale of months, but is generally near 25 counts per second. When the rate is near saturation, corrections for discriminator deadtime should be made. The discriminator deadtime is approximately 20 micro-seconds (it varies slightly with the electron energy spectrum), so that the saturation level is approximately 50,000 counts per second. When the correction is near a factor of two or less a reliable corrected rate can be obtained from the formula {corrected rate} = {uncorrected rate}/(1+deadtime*{uncorrected rate}) When the deadtime correction is substantially larger than a factor of two, reliable corrections are not available. In this case, electron pileup and baseline shift may also be important, which may increase or decrease the expected rate. The data points are 6 second averages taken once every 96 seconds. Table 1 below provides the D1 response function R(E,theta) which is a function of electron energy E in MeV (column at left) and angle theta in degrees from the TET axis (row at top). Each table entry is R in cm**2 for the corresponding E and theta. The D1 electron rate is related to the differential intensity j(E,alpha) in (cm**2 s sr MeV)**-1, where alpha is the electron pitch-angle, by integrating the product R*j over E and solid angle. Note that the angle between the TET axis and the local magnetic field direction is also required. The D1 RATE is then obtained by adding the background rate and applying the inverse of the deadtime correction described above. At energies above the maximum provided R can be approximated by the value at the highest provided energy. At angles above the maximum provided R can be approximated by zero. ------------------------------------------------------------------- Table 1. D1 response function ------------------------------------------------------------------- | 11. 15. 23. 32. 41. 51. 61. ------------------------------------------------------------------- | 0.618 | 0.014 0.005 0.007 0.007 0.006 0.003 0.001 0.801 | 0.151 0.134 0.103 0.087 0.038 0.016 0.008 0.989 | 1.384 1.440 1.219 0.998 0.610 0.311 0.143 1.179 | 2.233 2.402 2.095 1.796 1.255 0.689 0.380 1.372 | 2.829 2.938 2.593 2.241 1.636 0.956 0.583 1.567 | 3.212 3.283 2.936 2.536 1.940 1.167 0.724 1.763 | 3.495 3.534 3.206 2.772 2.161 1.356 0.860 1.959 | 3.708 3.705 3.404 2.964 2.357 1.495 0.969 2.157 | 3.620 3.790 3.452 3.053 2.427 1.602 1.049 2.355 | 3.995 3.948 3.576 3.231 2.617 1.758 1.155 2.553 | 4.096 4.091 3.735 3.395 2.735 1.875 1.263 2.752 | 4.154 4.098 3.808 3.426 2.792 1.927 1.298 2.951 | 4.043 4.054 3.727 3.371 2.819 1.951 1.339 3.150 | 3.946 4.029 3.700 3.335 2.648 1.956 1.358 3.350 | 3.876 4.194 3.611 3.573 2.863 1.927 1.290 ------------------------------------------------------------------- Table 1. D1 response function (continued) ------------------------------------------------------------------- | 70. 80. 90. 100. ------------------------------------------------------------------- 0.618 | 0.002 0.001 0.000 0.000 0.801 | 0.010 0.007 0.004 0.001 0.989 | 0.163 0.095 0.047 0.018 1.179 | 0.386 0.217 0.113 0.056 1.372 | 0.526 0.301 0.163 0.087 1.567 | 0.617 0.366 0.201 0.117 1.763 | 0.679 0.413 0.241 0.146 1.959 | 0.730 0.461 0.270 0.179 2.157 | 0.760 0.484 0.296 0.207 2.355 | 0.809 0.518 0.329 0.242 2.553 | 0.836 0.551 0.363 0.292

6) VG2 NEP CRS RESAMPLED SUMMARY D2 RATE ELEC 96SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/CRS/Neptune/PT96S
Start:1989-08-24 22:00:00 Observatory:Voyager 2 Cadence:96 seconds
Stop:1989-08-25 10:00:00 Instrument:Cosmic Ray System (CRS) Resource:NumericalData
Data Set Overview ================= Counting rate from the D2 detector in the Cosmic Ray System (CRS) electron telescope (TET) on Voyager 2 during the Neptune encounter. The D2 detector nominally responds to electrons with kinetic energies above approximately 2.5 MeV (see detector description for details). Parameters ========== Sampling parameter name : time Sampling parameter resolution : 6.0 seconds Minimum sampling parameter : n/a Maximum sampling parameter : n/a Sampling parameter interval : 96.0 seconds Minimum available sampling interval : 96.0 seconds Data set parameter name : D2 rate Noise level : 0.000 counts/second Data set parameter unit : counts/second The D2 detector is located behind the D1 detector in the TET telescope, so that most of the electrons observed by D2 have to penetrate D1 first. The D2 rate therefore applies to higher energy electrons and the threshold energy is less distinct than for D1, but is near 2.5 MeV. The rate can be calculated from the electron differential flux in the same way as the D1 RATE (see D1 RATE description) with the following calibration table. ------------------------------------------------------------------- Table 1. D2 response function ------------------------------------------------------------------- | 11. 23. 41. 61. 80. 90. 100. ------------------------------------------------------------------- 0.989 | 0.000 0.000 0.000 0.001 0.002 0.001 0.001 1.179 | 0.000 0.000 0.000 0.013 0.023 0.021 0.018 1.372 | 0.000 0.000 0.000 0.037 0.052 0.051 0.043 1.567 | 0.000 0.019 0.028 0.063 0.082 0.066 0.061 1.763 | 0.041 0.034 0.045 0.090 0.111 0.098 0.080 1.959 | 0.106 0.078 0.072 0.119 0.142 0.125 0.097 2.157 | 0.255 0.186 0.127 0.152 0.170 0.146 0.109 2.355 | 0.488 0.381 0.228 0.206 0.212 0.176 0.126 2.553 | 0.772 0.627 0.361 0.272 0.255 0.202 0.139 2.752 | 1.019 0.864 0.501 0.340 0.299 0.226 0.152 2.951 | 1.220 1.053 0.634 0.400 0.335 0.250 0.165 3.150 | 1.461 1.218 0.746 0.459 0.375 0.289 0.188 3.350 | 1.628 1.378 0.940 0.515 0.456 0.411 0.282 Processing ========== The ENCYCLOPEDIA GENERATOR program was run by Nand Lal at Goddard Space Flight Center to read the EDR tape, check for error conditions, and reformat the data to generate a CRS encyclopedia tape. The resulting tape was sent to CalTech for subsequent data analysis. The VCRUSH program was run at CalTech to select data of interest from CRS encyclopedia tapes. In the case of counting rate data, no further analysis was done to produce the data in the PDS data sets. Note: Neither the ENCYCLOPEDIA GENERATOR or VCRUSH software are available for public use.

7) 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

8) VOYAGER 2 DAILY POSITION V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/Ephemeris/Heliosphere/P1D
Start:1977-08-25 00:00:00 Observatory:Voyager 2 Cadence:1 day
Stop:2005-01-09 00:00:00 Instrument:Voyager 2 Positions Resource:NumericalData
Data Set Overview ================= These data were obtained from running the program HELICOOR in the public directory NSSDCA::ANON_DIR:[ACTIVE.HELIO]. These data are based on predicted trajectories calculated with the GTDS code by the NSSDC Satellite Situation Center and converted to solar ecliptic and heliographic coordinates by the HELIOCOOR program. The HELICOOR code was written by R. Parthasarathy. The program GENTRJCON added the HILLON longitude. Note that the solar ecliptic coordinates are given with respect to true equinox and ecliptic of date. The solar ascending node was located at ecliptic longitude +74.367 degrees as of 1 Jan. 1900 at 1200 UT; this longitude increases by 1.4 degrees/century. Data Formats ============ field description ----- ------------------------------ 1. Date YYYY DDD.DD where YY=year and DDD.DD=decimal day 2. Range Heliocentric range in AU 3. SE_Lat Solar Ecliptic latitude in degrees 4. SE_Lon Solar Ecliptic longitude in degrees 5. HG_Lat Heliographic latitude in degrees 6. HG_Lon Heliographic longitude in degrees 7. IHG_Lon Inertial Heliographic longitude in degrees with respect to the ascending node of the solar equator in the ecliptic. Contact Information =================== R. P. (Sardi) Parthasarathy Hughes STX Corporation / Space Physics Data Facility NASA Goddard Space Flight Center Greenbelt, Maryland sardi@nssdca.gsfc.nasa.gov Phone: (301) 286-8105 Acknowledgement =============== Use of these data in publications should be accompanied at minimum by acknowledgements of the National Space Science Data Center and the responsible Principal Investigator defined in the experiment documentation provided here.

9) VG2 JUP EPHEMERIS SYSTEM III (1965) COORDS BROWSE V1.1 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/Ephemeris/Jupiter/PT96S
Start:1979-07-05 00:00:47 Observatory:Voyager 2 Cadence:96 seconds
Stop:1979-08-12 16:54:20 Instrument:Voyager 2 Positions Resource:NumericalData
Data Set Overview ================= Version 1.1 ----------- The SEDR based data provided as part of this data set were originally reviewed and archived with the NSSDC and PDS as version 1.0 (DATA_SET_ID = VG2-J-POS-4-48.0SEC). Version 1.1 includes additional columns not present in the previous version, 96 second rather than 48 second time samples, times converted to 'PDS Style' or 'Zulu time', and upgrading of PDS labels and templates to version 3.4. The SPICE based data that are also part of this data set were not previously archived with the PDS. This version 1.1 data set replaces previously archived versions. Data Set Description -------------------- This data set consists of Voyager 2 Jupiter encounter ephemeris data in System III (1965) left handed coordinates covering the period 1979-07-05 to 1979-08-12. 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 2 SEDR, the other by the PDS/PPI node using the VG2_JUP.BSP and PCK00003.TCP SPICE kernels. Due to inaccuracies in Voyager SEDR, as well as changes in the values of some key parameters (e.g. Jovian 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 : 1979-07-05T00:00:47.269Z Data Set Stop Time : 1979-08-12T16:54:20.608Z SPICE generated ephemeris ------------------------- Instrument P.I. : N/A Data Supplier : S. Joy Data sampling rate : 48 seconds Data Set Start Time : 1979-07-05T00:00:47.269Z Data Set Stop Time : 1979-08-12T16:55:08.608Z Parameters ========== SEDR generated ephemeris ------------------------ PARAMETER RESOLUTION/ DESCRIPTION NAME UNITS time 96.0 Sec time of the sample (UT) in the format yyyy-mm-ddThh:mm:ss.sssZ m65536 counts spacecraft clock counts mod60 counts fds_line counts sc_x R[J] jovicentric (System III) cartesian sc_y R[J] cartesian position vectors: X, Y, and sc_z R[J] Z vel_x km/s jovicentric X, Y, and Z spacecraft vel_y km/s velocity components vel_z km/s sc_r R[J] jovicentric (System III) spherical sc_lat degrees coordinates position vectors: range, sc_lon degrees latitude, and longitude CartSys3_to_SphSys3 cartesian system III to spherical system III coordinates rotation matrix containing 9 1pe15.8 elements SC_to_CartSys3 payload (spacecraft) to cartesian system III coordinates rotation matrix containing 9 1pe15.8 elements SC_to_SphSys3 payload (spacecraft) to spherical system III coordinates rotation matrix containing 9 1pe15.8 elements SPICE generated ephemeris ------------------------- PARAMETER RESOLUTION/ DESCRIPTION NAME UNITS time 48.0 Sec time of the sample (UT) in the format yyyy-mm-ddThh:mm:ss.sssZ R AU jovicentric (System III 1965) LAT degrees spherical coordinates position LON degrees range, latitude, and longitude LocTime hours angular separation between the meridian containing the sun and the

10) VG2 NEP TRAJECTORY DERIVED SUMM NLS COORDS 12SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/Ephemeris/Neptune/PT12S
Start:1989-08-24 18:00:00 Observatory:Voyager 2 Cadence:12 seconds
Stop:1989-08-26 08:19:48 Instrument:Voyager 2 Positions Resource:NumericalData
Data Set Overview ================= This dataset contains Voyager 2 spacecraft position vectors relative to Neptune in minus NLS coordinates. The NLS or Neptune West Longitude System coordinate system is a planetocentric system fixed to Neptune which is rotating with a 16.11 hour period. The NLS coordinate system is defined as follows: - X lies in the equatorial plane of Neptune, positive away from the planet, and through the prime meridian. - Z is parallel to the Neptune spin axis, and, - Y is X x Z (lefthanded) The prime meridian of the this system is defined such that at 1989-08-25T03:56:00.000 the Voyager 2 spacecraft was at 167.7 degrees west longitude. For the PDS archive dataset, the original data archive has been converted to an east longitude (righthanded) coordinate system minus NLS (-NLS). This is achieved by reversing the direction of the Y-axis or in spherical coordinates, subtracting the NLS longitude from 360.0 degrees. The data are provided in units of Neptune radii which was taken to be 24,765km by the Voyager project. Angles are given in degrees. Both cartesian and spherical coordinates are provided. Parameters ========== Sampling parameter name : time Sampling parameter resolution : 12.0 seconds Minimum sampling parameter : n/a Maximum sampling parameter : n/a Sampling parameter interval : 12.0 seconds Minimum available sampling interval : 12.0 seconds Data set parameter name : position vector Noise level : n/a Data set parameter unit : Neptune radii (24,765km) or degrees Coordinates =========== Neptune West Longitude System (NLS) Coordinates ----------------------------------------------- Coordinate System Center Name = NEPTUNE Coordinate system Ref Epoch = UNK /* 1989-08-25:03:56:00.000 */ The orientation of Neptune's pole is specified by a right ascension of 298.90 and declination of 42.84 at the time of the encounter, as given in the Jet Propulsion Laboratory's distribution of physical constants dated 11/06/89. Planetary longitudes are based on a 16.11 hour rotation period (Warwick et al., 1989) adopted by the Voyager Project shortly after the encounter. The zero longitude is defined by the requirement that the West Longitude of the spacecraft at 0356 SCET day 237 (near closest approach) be 167.7 NLS; West Longitudes of the Neptune Longitude System (NLS) are simply related to the angle PHI: WLONG = 360. - PHI (degrees) This definition of the zero longitude was adopted by the Voyager Project Steering Group in order to minimize differences in longitudes resulting from changes in the assumed rotation period. Position is given in terms of the following: RANGE (R) - Range from the planet center to the spacecraft in units of Rn where Rn = 24,765km. LATITUDE (LAT) - Spacecraft latitude in degrees. Valid range -90.0 -> +90.0. LONGITUDE (W_LONG) - West longitude where the zero longitude is defined by the requirement that the West Longitude of Voyager 2 at 1989-08-25T03:56:00.00 was 167.7 degrees.

11) VG2 NEP TRAJECTORY DERIV SUMM HELIOGRAPHIC COORDS 48SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/Ephemeris/Neptune/PT48S
Start:1989-08-22 00:00:47 Observatory:Voyager 2 Cadence:48 seconds
Stop:1989-08-29 23:59:58 Instrument:Voyager 2 Positions Resource:NumericalData
Data Set Overview ================= This dataset contains Voyager 2 position vectors relative to the Sun in both cartesian and spherical Heliographic coordinates for the time period when Voyager was near Neptune but not within its magnetosphere. The magnetospheric gap in this dataset occurs from 1989-08-25 02:00 -> 1989-08-26 00:00. Spacecraft position vectors are given in Neptune Longitude System (NLS) coordinates in this interval. The position vectors are given every 48 seconds. The units of the vector components are Au and degrees. Vectors are stored as 4-byte floating point values. The Heliographic coordinate system is defined in the reference epoch of 1950. The unit vectors which define the coordinate system are as follows: X points away from the Sun toward the ascending node, in the solar equatorial plane, Z points along the Sun's spin axis, positive above the equatorial plane, and Y completes the right handed set. Parameters ========== Sampling parameter name : time Sampling parameter resolution : 96.0 seconds Minimum sampling parameter : n/a Maximum sampling parameter : n/a Sampling parameter interval : 48.0 seconds Minimum available sampling interval : 48.0 seconds Data set parameter name : position vector Noise level : n/a Data set parameter unit : AU or degrees Coordinates =========== MEAN INERTIAL HG 1950 --------------------- COORDINATE_SYSTEM_CENTER_NAME = SUN COORDINATE_SYSTEM_REF_EPOCH = UNK /* 09-23-1950 */ The Heliographic coordinate system is defined in the reference epoch of 1950. The unit vectors which define the coordinate system are as follows: X points away from the Sun towards the ascending node, in the solar equatorial plane, Z points along the Sun's spin axis, positive above the equatorial plane, and Y completes the right handed set. Position is given in terms of the following: RANGE (R) - The range or R component of the spherical Heliographic coordinate system is the distance from the Sun's position at the reference epoch to the spacecraft measured in AU. LATITUDE (LAT) - The latitude component of the spherical Heliographic coordinate system is the angle between the solar equatorial plane of the reference epoch measured in the plane that contains the solar spin axis of that epoch. LONGITUDE (LONG) - The longitude component of the spherical Heliographic coordinate system is zero in the direction of the ascending node at the reference epoch (X direction) and increases for a body orbiting the Sun as the Earth does. X - The X component of the Heliographic coordinate system points away from the Sun, towards the ascending node, and lies in the solar equatorial plane. Y - The Y vector of the Heliographic coordinate system is formed by the righthanded cross product of the X and Z unit vectors. It lies in the solar equatorial plane and it points away from the Sun, but does not extend in the direction of any particular body. Z - The Z component of the Heliographic coordinate system is parallel to the Sun's spin axis, taken as positive above the equatorial plane of the Sun.

12) VG2 SAT EPHEMERIS KRONOGRAPHIC (L1) COORDS BROWSE V1.1 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/Ephemeris/Saturn/PT96S
Start:1981-08-23 10:34:23 Observatory:Voyager 2 Cadence:96 seconds
Stop:1981-08-29 23:57:35 Instrument:Voyager 2 Positions Resource:NumericalData
Data Set Overview ================= Data Set Description -------------------- This data set consists of Voyager 2 Saturn encounter ephemeris data in Kronographic (L1) coordinates covering the period 1981-08-23 to 1981-08-29. 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 2 SEDR, the other by the PDS/PPI node using the VG2_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 : 1981-08-23T10:34:23.645Z Data Set Stop Time : 1981-08-29T23:57:35.078Z SPICE generated ephemeris ------------------------- Instrument P.I. : N/A Data Supplier : S. Joy Data sampling rate : 96 seconds Data Set Start Time : 1981-08-23T10:34:23.645Z Data Set Stop Time : 1981-08-29T23:57:35.078Z 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

13) 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

14) Voyager2 LECP H Fluxbox Fluxes in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/H-FLUX-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Calibrated, Cadence PT5D

15) Voyager2 LECP H Fluxbox Fluxes in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/H-FLUX-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Calibrated, Cadence P5D

16) Voyager2 LECP H Fluxbox Rates in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/H-RATE-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Uncalibrated, Cadence PT5D

17) Voyager2 LECP H Fluxbox Rates in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/H-RATE-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Uncalibrated, Cadence P5D

18) Voyager2 LECP He Fluxbox Fluxes in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/HE-FLUX-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Calibrated, Cadence PT5D

19) Voyager2 LECP He Fluxbox Fluxes in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/HE-FLUX-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Calibrated, Cadence P5D

20) Voyager2 LECP He Fluxbox Rates in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/HE-RATE-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Uncalibrated, Cadence PT5D

21) Voyager2 LECP He Fluxbox Rates in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/HE-RATE-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Uncalibrated, Cadence P5D

22) Voyager2 LECP O Fluxbox Fluxes in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/O-FLUX-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Calibrated, Cadence PT5D

23) Voyager2 LECP O Fluxbox Fluxes in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/O-FLUX-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Calibrated, Cadence P5D

24) Voyager2 LECP O Fluxbox Rates in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/O-RATE-P26D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:26 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Uncalibrated, Cadence PT5D

25) Voyager2 LECP O Fluxbox Rates in ASCII Format 5-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/FLUXBOX/O-RATE-P5D
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:5 days
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Weighted Count Rates, Derived from PHA Data plus Rate Data by sectors and averaged, Voyager2, LECP, Uncalibrated, Cadence P5D

26) Voyager 2 LECP Cosmic Ray Proton Rates in ASCII Format daily maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/Flux.Cosmic.Ray.P1D
Start:1977-09-07 00:00:00 Observatory:Voyager 2 Cadence:24 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager2, LECP, Filtered, Channel, Calibrated, CadencePT24H

27) Voyager 2 LECP Cosmic Ray Proton Rates in ASCII Format 26-day maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/Flux.Cosmic.Ray.P26D
Start:1977-09-07 00:00:00 Observatory:Voyager 2 Cadence:26 days
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager2, LECP, Filtered, Channel, Calibrated, CadenceP26D

28) Voyager 2 LECP Key Channel Intensities in ASCII Format daily maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/Flux.Ion.P1D
Start:1977-09-07 00:00:00 Observatory:Voyager 2 Cadence:24 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager2, LECP, Filtered, Channel, Calibrated, CadencePT24H Each file in this directory contains one year's worth of data from the LECP instrument on the Voyager 1 spacecraft. Each record in a file contains 1-day (24-hour) averages of fluxes and flux uncertainties of ions (Z>=1) in eight contiguous energy channels, from 0.040-4.00 Mev/ion. Each file contains a 2-line header that identifies the spacecraft, data type and time resolution, and labels each column of data. Statistical uncertainties represent one standard deviation. Differential (in energy) flux units are: Ions/(cm^2 sec ster MeV).

29) Voyager 2 LECP Key Channel Intensities in ASCII Format hourly maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/Flux.Ion.PT1H
Start:1977-09-07 00:00:00 Observatory:Voyager 2 Cadence:1 hour
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager2, LECP, Filtered, Channel, Calibrated, CadencePT1H

30) Voyager 2 LECP Key Channel Intensities By Sector in ASCII Format 3-hour maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/Flux.Ion.Sectored.PT3H
Start:1991-01-03 00:00:00 Observatory:Voyager 2 Cadence:3 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, For All Sectors, Voyager2, LECP, Filtered, Channel, Calibrated, CadencePT3H

31) Voyager 2 LECP Proton Intensities in ASCII Format daily maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/Flux.Proton.P1D
Start:1977-09-07 00:00:00 Observatory:Voyager 2 Cadence:24 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager2, LECP, Filtered, Channel, Calibrated, CadencePT24H Each file in this directory contains one year's worth of data from the LECP instrument on the Voyager 1 spacecraft. Each record in a file contains 1-day (24-hour) averages of fluxes and flux uncertainties of ions (Z>=1) in eight contiguous energy channels, from 0.040-4.00 Mev/ion. Each file contains a 2-line header that identifies the spacecraft, data type and time resolution, and labels each column of data. Statistical uncertainties represent one standard deviation. Differential (in energy) flux units are: Ions/(cm^2 sec ster MeV).

32) Voyager 2 LECP Proton Intensities in ASCII Format hourly maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/Flux.Proton.PT1H
Start:1977-09-07 00:00:00 Observatory:Voyager 2 Cadence:1 hour
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, Averaged Over All Sectors, Voyager2, LECP, Filtered, Channel, Calibrated, CadencePT1H

33) VG2 LECP 0.4S HIGH RESOLUTION JUPITER FAR ENCOUNTER DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Jupiter/PT0.400S
Start:1979-07-01 00:00:23 Observatory:Voyager 2 Cadence:0.400 seconds
Stop:1979-08-08 00:00:18 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 Jupiter. 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 Jupiter far encounter, the entire LEPT (Low Energy Particle Telescope) and part of the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystems were turned on for data collection. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 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

34) VG2 JUP LECP CALIBRATED RESAMPLED SECTORED 15MIN V1.1 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Jupiter/PT15M
Start:1979-07-02 07:35:11 Observatory:Voyager 2 Cadence:15 minutes
Stop:1979-08-03 23:44:45 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Data Set Description ==================== Version 1.1 ----------- This version 1.1 data set replaces the version 1.0 data set (DATA_SET_ID = VG2-J-LECP-4-15MIN) previously archived with the PDS. Data records from the version 1.0 data set provided data for each of 8 sectors, plus the average for all sectors in a separate record for each channel. This resulted in 9 repeated times per channel. Data records for the version 1.1 data set provide all data for a given channel and time period (8 sectors, plus the average for all sectors) in a single record. Other changes to this version include upgrading of the associated labels and templates to PDS version 3.4 compliance, modification of the time formats and flag values. Data Set Description -------------------- This data set consists of resampled data from the Low Energy Charged Particle (LECP) experiment on Voyager 2 while the spacecraft was in the vicinity of Jupiter. This instrument measures the intensities of in-situ charged particles (>26 keV electrons and >30 keV ions) with various levels of discrimination based on energy, mass species, and angular arrival direction. A subset of almost 100 LECP channels are included with this data set. The LECP data are globally calibrated to the extent possible (see below) and they are time averaged to about 15 minute time intervals with the exact beginning and ending times for those intervals matching the LECP instrumental cycle periods (the angular scanning periods). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles that it measures. The cycle time for the rotation is variable, but during encounters it is always faster than 15 minutes. Thus, the full angular anisotropy information is preserved with this data. The data is in the form of 'rate' data which has not been converted to the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'rate' to 'intensity' for a particular channel one performs the following tasks: 1) Decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 has a 2 mm Al shield covering it). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. The geometric factor is found in entry 'CHANNEL_GEOMETRIC_FACTOR' as associated with each channel 'CHANNEL_ID'. To determine the energy bandpass, one must judge the mass species of the of the detected particles (for ions but not for electrons). The energy band passes are given in entries 'MINIMUM_INSTRUMENT_PARAMETER' and 'MAXIMUM_INSTRUMENT_PARAMETER' in table 'FPLECPENERGY', and are given in the form 'energy/nucleon'. For channels that begin their names with the designations 'CH' these bandpasses can be used on mass species that are accepted into that channel (see entries 'MINIMUM_INSTRUMENT_PARAMETER' AND 'MAXIMUM_INSTRUMENT_PARAMETER' in table 'FPLECPCHANZ', which give the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The and passes for other 'Z' values are not all known, but some are given in the literature (e.g. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity with the units: counts/(cm^2 str sec keV). 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 : VG2 Data Set Parameter Name : ION RATE Instrument Parameter Name : ION RATE Important Instrument Parameters : 1 Instrument Host ID : VG2 Data Set Parameter Name : ELECTRON RATE Instrument Parameter Name : ELECTRON RATE Important Instrument Parameters : 1 Processing ========== Processing Level Id : 4 Software Flag : Y Processing Start Time : 1988-08-01 Processing History ------------------ Source Data Set ID : VG2-J-LECP-2- Software : PFAT:VGER Product Data Set ID : VG2-J-LECP-4-15MIN Software 'PFAT:VGER' -------------------- Software Name : PFAT:VGER Software Type : PIN Software Release Date : N/A Node ID : N/A Cognizant Engineer : N/A Software Access Description : N/A Data Coverage ============= Filename Records Start Stop ------------------------------------------------------------------- Volume ID: VG_1502 SECTOR.TAB 64944 1979-07-02T07:35:11.000 1979-08-03T23:30:21.000 SECTOR_SUMMARY.TAB 784 1979-07-02T07:00:00.000 1979-08-03T22:00:00.000

35) VG2 LECP 3.2 MINUTE JUPITER FAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Jupiter/PT3M
Start:1979-07-08 05:39:11 Observatory:Voyager 2 Cadence:3 minutes
Stop:1979-07-11 08:18:29 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 Jupiter. 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 Jupiter far encounter, the entire LEPT (Low Energy Particle Telescope) and part of the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystems were turned on for data collection. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 3.2 minute rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'rate' to 'intensity' for a particular channel one performs the following tasks: 1) decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of 'energy/nucleon'. For channels that begin their names with the designations 'ch' these bandpasses can be used on mass species that are accepted into that channel, which gives the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The bandpasses for other 'Z' values are not all known, but some are given in the literature (e.g. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. Far Encounter Channel Definitions for Voyager 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

36) VG2 LECP 48.0 SECOND JUPITER FAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Jupiter/PT48S
Start:1979-06-30 23:59:59 Observatory:Voyager 2 Cadence:48 seconds
Stop:1979-07-22 00:00:04 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 Jupiter. 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 Jupiter far encounter, the entire LEPT (Low Energy Particle Telescope) and part of the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystems were turned on for data collection. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 48.0 second rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'rate' to 'intensity' for a particular channel one performs the following tasks: 1) decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of 'energy/nucleon'. For channels that begin their names with the designations 'ch' these bandpasses can be used on mass species that are accepted into that channel, which gives the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The bandpasses for other 'Z' values are not all known, but some are given in the literature (e.g. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. 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

37) VG2 LECP 0.4S HIGH RESOLUTION NEPTUNE FAR ENCOUNTER DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Neptune/PT0.400S
Start:1989-08-24 00:00:23 Observatory:Voyager 2 Cadence:0.400 seconds
Stop:1989-08-28 00:00:20 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 Neptune. 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 Neptune 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

38) VG2 LECP 12.8 MINUTE NEPTUNE FAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Neptune/PT12M48S
Start:1989-08-24 12:12:00 Observatory:Voyager 2 Cadence:12 minutes; 48 seconds
Stop:1989-08-26 23:44:00 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 Neptune. 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 Neptune 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 12.8 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

39) VG2 NEP LECP RESAMPLED SUMMARY SCAN AVERAGED 24SEC V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Neptune/PT24S
Start:1989-08-24 00:00:00 Observatory:Voyager 2 Cadence:24 seconds
Stop:1989-08-27 00:00:00 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Description of the PDS LECP Neptune Scan data. 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 Neptune. The period covered is 1989-08-24T00:00:00.000 SCET to 1989-08-27T00:00:00.000 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 (12 or 24 sec, see below) for the periods when the detectors are stationary. The angle averaged records represent periods of time equal to 48 or 96 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. Three 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), 2) a special Neptune scan cyclic with the following sequence: 7, scan, 1, scan, 7, scan, scan, repeat; where the 7 and the 1 represent 5.2 minute periods when the instrument is fixed in sectors 7 or 1, respectively, and where the word scan represents a period of scanning (6 sec stepping for a total scan time of 48 sec); and 3) periods when the detectors are fixed for more extended periods in sector 7 (periods bracketing the ring plane crossings). For this Neptune Scan data, the 6.4 minute scan records during stepping mode (1) have been time averaged to 12.8 minute records. Also, during stepping mode (2), the double scans that have no fixed periods between them have been averaged together into a single (96 sec) record. The single scans represent 48 sec records. The schedule for the three stepping modes is as follows: prior to day 236/1600 SCET: Mode (1) 236/1600 to 237/0239: Mode (2) 237/0239 to 237/0319: Mode (3) 237/0319 to 237/0503: Mode (2) 237/0503 to 237/0554: Mode (3) 237/0554 to 238/0400: Mode (2) after 237/0400: Mode (1) Obviously these stepping mode changes, and the angle sample switching that occurs during stepping mode (2), gives the data a disjointed appearance. Two channel sample modes also occurred during the Neptune encounter. These two modes affect this data set only by changing the primary record time length for the LECP Experiment Data Records (EDR's). These time lengths have, in turn, been utilized for the averaging times of this data set for non-stepping periods. The schedule is: prior to day 237/0200 SCET: Far Encounter (24 sec records) 237/0200 to 237/0551: Near Encounter (12 sec records) after 237/0551: Far Encounter (24 sec records) 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

40) VG2 LECP 3.2 MINUTE NEPTUNE FAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Neptune/PT3M
Start:1989-08-23 19:55:59 Observatory:Voyager 2 Cadence:3 minutes
Stop:1989-08-26 23:53:11 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 Neptune. 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 Neptune far encounter, the entire LEPT (Low Energy Particle Telescope) and part of the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystems were turned on for data collection. Particles include electrons, protons, alpha particles, and light, medium, and heavy nuclei particles. The far encounter data are 3.2 minute rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'rate' to 'intensity' for a particular channel one performs the following tasks: 1) decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of 'energy/nucleon'. For channels that begin their names with the designations 'ch' these bandpasses can be used on mass species that are accepted into that channel, which gives the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The bandpasses for other 'Z' values are not all known, but some are given in the literature (e.g. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. Far Encounter Channel Definitions for Voyager 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

41) VG2 LECP 6 MINUTE NEPTUNE STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Neptune/PT6M
Start:1989-08-19 19:55:59 Observatory:Voyager 2 Cadence:6 minutes
Stop:1989-09-02 19:53:10 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
TBD

42) Voyager2 LECP PHA Events in ASCII maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/PHA
Start:1993-01-01 00:00:00 Observatory:Voyager 2 Cadence:
Stop:2010-12-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
PHA Events, Voyager2, LECP, Uncalibrated

43) Voyager 2 LECP Survey Plots at JHU_APL maxmize
Resource ID:spase://VSPO/DisplayData/Voyager2/LECP/PLOTS
Start:1977-09-07 00:00:00 Observatory:Voyager 2 Cadence:
Stop:2016-09-14 07:59:48 Instrument:Low-Energy Charged Particles (LECP) Resource:DisplayData
26-day, 104-day and 1-year plots of fluxes of 40-4000 keV ions in 8 channels and of .57-31 MeV protons in 3 channels

44) Voyager 2 LECP - Daily Average Interplanetary Data maxmize
Resource ID:spase://VSPO/NumericalData/Voyager2/LECP/Particle/PT24H
Start:1977-09-07 00:00:00 Observatory:Voyager 2 Cadence:24 hours
Stop:1994-12-30 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
This data file contains 1 day averages of count rates for 11 energetic ion channels from the Low Energy Charged Particle (LECP) instrument on Voyager 2. The data listed are averaged over 24 hours, with the start time of the averging interval begining at the start of the day listed. For example, 77/300 is an average over hours 0-23 on day 300 of 1977. Times are given in SCET-UT. The count rates R are in counts per second. The statistical uncertainty for each channel is the inverse square root of the total number of counts during each 24 hour period times the average count rate R. Included in the data table are the passbands in KeV for protons, the logarithmic mean energy Em for the differential energy channels, the geometric factor "g" (cm**2-steradian), and the flux conversion factor "f". To get from count rate R to differential in energy flux "dj(E)/dE", multiply R by f, i.e., dj(E)/dE=f*R. Note that f is simply the inverse of the energy passband multiplied by the geometric factor. Generally one uses a more elaborate algorithm to calculate fluxes by determining the local slope of the energy spectrum within each energy passband, usually by an iterative algorithm, and then evaluating the flux corresponding to each channel using this slope. However, if the slope of the energy spectrum is not to steep, the approximation dj(E)/dE=f*R is very good if the flux is evaluated at the mean energy Em=Sqrt(EL*EH), where EL and EH are the low and high energy ends of the passband. Since the slopes of low energy ion spectra in the interplanetary medium are in the range of -1 to -3, the approximation is very good.

45) Voyager2 LECP Average Filtered Rate Data in ASCII Format daily maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/Rates.P1D
Start:1977-08-22 00:00:00 Observatory:Voyager 2 Cadence:24 hours
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, All Sectors, Voyager2, LECP, Filtered, Channel, CadencePT24H

46) Voyager2 LECP Average Filtered Rate Data in ASCII Format hourly maxmize
Resource ID:spase://VEPO/NumericalData/Voyager2/LECP/Rates.PT1H
Start:1977-08-22 00:00:00 Observatory:Voyager 2 Cadence:1 hour
Stop:2009-05-31 23:59:59 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Count Rates, All Sectors, Voyager2, LECP, Filtered, Channel, CadencePT1H

47) VG2 LECP 0.4S HIGH RESOLUTION SATURN NEAR ENCOUNTER DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Saturn/PT0.400S
Start:1981-08-26 01:09:35 Observatory:Voyager 2 Cadence:0.400 seconds
Stop:1981-08-26 07:01:30 Instrument:Low-Energy Charged Particles (LECP) Resource:NumericalData
Data Set Overview ================= Data Set Description -------------------- This near encounter data set consists of electron and ion counting rate data from the Low Energy Charged Particle (LECP) experiment on Voyager 1 while the spacecraft was within the very close vicinity of Saturn. 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 Saturn near encounter, the LEMPA (Low Energy Magnetospheric Particle Analyzer) subsystem was turned on for data collection. Particles include low energy electrons, protons, alpha particles, medium energy protons and ions, high energy and intensity protons, electrons, alpha particles, and Z >= nuclei. The near encounter data are 0.4 second rate measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'rate' to 'intensity' for a particular channel one performs the following tasks: 1) decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of 'energy/nucleon'. For channels that begin their names with the designations 'ch' these bandpasses can be used on mass species that are accepted into that channel, which gives the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The bandpasses for other 'Z' values are not all known, but some are given in the literature (e.g. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. Near Encounter Channel Definitions for Voyager 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 44 AL01 1.040 1.850 1.000 0.12000 CALC. 45 AL02 1.850 3.700 2.500 0.12000 CALC. 77 ESA0 2.500 99.999 2.500 0.49350 A-B COINC. 78 ESB0 8.500 99.999 8.500 0.94620 B 4 PI SR 79 AB10 8.500 99.999 8.500 0.05040 A-B COINC. 80 DP09 0.285 5.020 0.250 0.00084 DELTA' 81 DP10 0.480 2.580 0.600 0.00084 DELTA' 82 DP11 0.725 1.640 1.000 0.00084 DELTA' 83 PD09 0.285 5.250 0.250 0.00260 DELTA 84 PD10 0.480 2.720 0.600 0.00260 DELTA 85 PD11 0.725 1.580 1.000 0.00260 DELTA 86 AB12 54.000 87.300 50.000 0.05040 A-B COINC. 87 AB13 87.300 152.000 100.000 0.05040 A-B COINC. 88 PSA1 15.800 158.000 15.000 0.49350 A 2 PI SR 89 PSA2 15.800 49.000 25.000 0.49350 A 2 PI SR 90 PSA3 16.300 26.200 25.000 0.49350 A 2 PI SR 91 PSB1 54.000 174.000 50.000 0.94620 B 4 PI SR 92 PSB2 54.000 87.300 50.000 0.94620 B 4 PI SR 93 PSB3 54.000 59.000 50.000 0.94620 B 4 PI SR 94 DA03 0.480 2.450 0.600 0.00084 DELTA' 95 DA04 0.780 1.410 1.000 0.00084 DELTA' 96 DZ01 0.405 18.800 0.600 0.00084 DELTA' 97 AD03 0.480 2.580 0.600 0.00260 DELTA 98 AD04 0.780 1.480 1.000 0.00260 DELTA 99 ZD01 0.400 19.800 0.600 0.00260 DELTA -------------------------------------------------------- Near encounter data are stored in files for channels from different rate groups indicated by the file names, e.g. V2YYDOY{A,B,...,H}NG0{1,2, ..., 9}.CSV ------- --------- -------------- | | | | | | | | | rate group number | | | | | | | starting time A: 00:00:00 | | | B: 03:00:00 | | | C: 06:00:00 | | | D: 09:00:00 | | | E: 12:00:00 | | | F: 15:00:00 | | | G: 18:00:00 | | | H: 21:00:00 | | | | | 3-digit day of year | | | 2-digit year | Voyager 2 Rate group definitions are listed as below: ------------------------------------------------------- rate channel names group in # the rate group ------------------------------------------------------- 1 PL01 PL02 PL03 EB04 EBP04 2 EB01 EBP01 EB02 EBP02 EB03 EBP03 EG06 3 PD09 DP09 PD10 DP10 PD11 DP11 AD03 DA03 4 EG07 EG08 EG09 EB05 EBP05 5

48) VG2 SAT LECP CALIBRATED RESAMPLED SECTORED 15MIN V1.0 maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Saturn/PT15M
Start:1981-08-24 00:00:00 Observatory:Voyager 2 Cadence:15 minutes
Stop:1981-08-30 23:45:00 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 2 while the spacecraft was in the vicinity of Saturn. This instrument measures the intensities of in-situ charged particles (>26 keV electrons and >30 keV ions) with various levels of discrimination based on energy, mass species, and angular arrival direction. A subset of almost 100 LECP channels are included with this data set. The LECP data are globally calibrated to the extent possible (see below) and they are time averaged to about 15 minute time intervals with the exact beginning and ending times for those intervals matching the LECP instrumental cycle periods (the angular scanning periods). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles that it measures. The cycle time for the rotation is variable, but during encounters it is always faster than 15 minutes. Thus, the full angular anisotropy information is preserved with this data. The data is in the form of 'rate' data which has not been converted to the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'rate' to 'intensity' for a particular channel one performs the following tasks: 1) Decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 has a 2 mm Al shield covering it). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. The geometric factor is found in entry 'CHANNEL_GEOMETRIC_FACTOR' as associated with each channel 'CHANNEL_ID'. To determine the energy bandpass, one must judge the mass species of the of the detected particles (for ions but not for electrons). The energy band passes are given in entries 'MINIMUM_INSTRUMENT_PARAMETER' and 'MAXIMUM_INSTRUMENT_PARAMETER' in table 'FPLECPENERGY', and are given in the form 'energy/nucleon'. For channels that begin their names with the designations 'CH' these bandpasses can be used on mass species that are accepted into that channel (see entries 'MINIMUM_INSTRUMENT_PARAMETER' AND 'MAXIMUM_INSTRUMENT_PARAMETER' in table 'FPLECPCHANZ', which give the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The and passes for other 'Z' values are not all known, but some are given in the literature (e.g. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity with the units: counts/(cm^2 str sec keV). 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 : VG2 Data Set Parameter Name : ION RATE Instrument Parameter Name : ION RATE Important Instrument Parameters : 1 Instrument Host ID : VG2 Data Set Parameter Name : ELECTRON RATE

49) VG2 LECP 3.2 MINUTE SATURN FAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Saturn/PT3M12S
Start:1981-08-29 06:30:47 Observatory:Voyager 2 Cadence:3 minutes; 12 seconds
Stop:1981-09-01 06:30:53 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 Saturn. 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 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 3.2 minute rate and flux measurements within 1/8 of the LECP instrumental motor rotation period (the angular scanning periods, or step period). The LECP instrument has a rotating head for obtaining angular anisotropy measurements of the medium energy charged particles. A gear-drive motor steps through eight equal angular sectors per revolution for data collection. The cycle time for the rotation is 48 minutes or 25.6 minutes during cruise mode, and 192 second or 48 second during the planetary encounter. The data were originally collected in the form of 'rates', which were not always converted into the usual physical units. The reason is that such a conversion would depend on uncertain determinations such as the mass species of the particles and the level of background. Both mass species and background are generally determined from context during the study of particular regions. To convert 'rate' to 'intensity' for a particular channel one performs the following tasks: 1) decide on the level of background contamination and subtract that off the given rate level. Background is to be determined from context and from making use of sector 8 rates (sector 8 is covered by a 2 mm Aluminium sunshield and used for data calibration). 2) Divide the background corrected rate by the channel geometric factor and by the energy bandpass of the channel. To determine the energy bandpass, one must judge the mass species of the detected particles (for ions but not for electrons). The energy band passes are given in the form of 'energy/nucleon'. For channels that begin their names with the designations 'ch' these bandpasses can be used on mass species that are accepted into that channel, which gives the minimum and maximum 'Z' value accepted -- these entries are blank for electron channels). For other channels the given bandpass refers only to the lowest 'Z' value accepted. The bandpasses for other 'Z' values are not all known, but some are given in the literature (e.g. [KRIMIGISETAL1979A]). The final product of these instructions will be the particle intensity in the unit of 'counts/(cm**2 sr sec keV)'. LECP data can also be in the form of flux, whose unit is 'cm**-1 sr**-1 sec**-1'. Far Encounter Channel Definitions for Voyager 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)

50) VG2 LECP 6.4 MINUTE SATURN FAR ENCOUNTER STEP DATA maxmize
Resource ID:spase://VMO/NumericalData/Voyager2/LECP/Saturn/PT6M24S
Start:1981-08-23 06:34:23 Observatory:Voyager 2 Cadence:6 minutes; 12 seconds
Stop:1981-08-29 06:30:53 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 Saturn. 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 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 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)

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