Find research datasets worth reusing

PVO VENUS EFD BROWSE ELECTRIC FIELD 24SEC AVGS V1.0

This data set contains wave electric field amplitudes measured at four different frequencies by the Pioneer Venus Orbiter Electric Field Detector. The data are averaged over 24 second intervals on 12 second centers. Each averaging interval contains both the minimum amplitude, average amplitude and peak amplitude for that interval at each of the four frequencies. The four frequencies are 100 Hz, 730 Hz, 5.4 kHz, 30 kHz. The frequency filters are narrow-band, with a 30% bandwidth. Thus wave amplitudes are given in V/m/root(Hz). The filters are continuously active, but data are only provided at a rate determined by the spacecraft telemetry rate. The wave antenna is oriented perpendicular to the spacecraft spin axis, and so the wave instrument measures only wave fields in the spacecraft spin plane. The wave antenna is a small Y-shaped structure, with effective separation of 0.76 meters.

VG1 JUP CRS DERIVED PROTON/ION/ELECTRON FLUX BROWSE V1.0

As its name implies, the Cosmic Ray Subsystem (CRS) was designed for cosmic ray studies. 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.

PVO VENUS ONMS BROWSE SUPRTHRML ION MAX COUNT RATE 12S V1.0

This data set represents the maximum count rate per second in a 12 second period beginning with the time of the first data point for a given mass number. Although species other than O+ cannot be reduced to to a flux and direction it is possible to estimate the approximate flux from the maximum count rate per second occurring within one spin period (about 12 seconds). The maximum count rate can be approximately converted to a flux using: [4.E7 (particles/cm**2/sec)]/[1.E4 (counts/sec)]. This sensitivity is for O+. At higher mass numbers the sensitivity is less, being about a factor of 2.5 lower for Ar+.

GALILEO EARTH1 MAGNETOMETER BROWSE DATA V1.0

This dataset contains data acquired by the Galileo Magnetometer from the Earth1 encounter. The data have been averaged down to twenty second resolution from the 7.68 kB Low Rate Science (LRS) real time telemetry mode. These data have been fully processed to remove instrument response function characteristics and interference from magnetic sources aboard the spacecraft. The data are provided in both Geocentric Solar Ecliptic (GSE) and Geocentric Solar Magnetic (GSM) coordinates.

VG2 SAT EPHEMERIS HELIOGRAPHIC COORDS BROWSE V1.0

This data set consists of Voyager 2 Saturn encounter ephemeris data in Heliographic coordinates covering the period 1981-08-24 to 1981-09-02. 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.

VG2 SAT EPHEMERIS KRONOGRAPHIC (L1) COORDS BROWSE V1.0

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.

VG2 URA PLS DERIVED SUMM ELECTRON BROWSE 48SEC V1.0

This data set contains the thermal electron density and temperature in the PLS energy range (10-5950 eV) from Voyager 2 at Uranus derived by fitting the low energy electron component with a Maxwellian distribution, and the moment density and temperature of the hot electrons calculated after the signal from the thermal component is subtracted from the electron spectra. The moment density and temperature obtained by integrating over the entire measured distribution function are also given.

VOYAGER 1 SATURN PLASMA DERIVED ION FITS BROWSE 96 SEC

THIS DATA SET CONTAINS THE ION DENSITIES, TEMPERATURES, AND VELOCITIES OBTAINED FROM VOYAGER 1 PLS DATA (VOLTAGE RANGE 10-5950 EV/Q) AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS. IT IS A SUBSET OF THE DATA SET VG1-S-PLS-5-ION-FIT-96.0SEC WHICH SHOULD BE OBTAINED BEFORE THIS DATA IS USED. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE OXYGEN. OUTSIDE L=10-12 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. A COMPLETE DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: FIRST 5 COLUMNS ARE TIME TAG (YEAR, DAY, HOUR, MIN SEC.MSEC), FOLLOWED BY PROTON DENSITY (CM-3), PROTON TEMPERATURE (EV), HEAVY ION DENSITY (CM-3), HEAVY ION TEMPERATURE (EV), AND THREE VELOCITY COMPONENTS, (RHO, PHI,Z) IN KM/S. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. EACH ROW HAS THE FORMAT (2I4,2I3,F7.3,7E11.3). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

PVO VENUS ONMS BROWSE THERMAL ION 12 SECOND V1.0

Thermal ions can be measured with the filament off and the ion repeller set at 0 V. Species observed include He+, N+, O+, CO+ and/or N2+, NO+, O2+ and CO2+. H+ is not measurable with the current instrument configuration. One component of the ion drift in the ecliptic plane can also be determined. Thermal ion measurements have been taken sporadically at the end of neutral density passes and on alternate orbits when superthermal ions are not being measured.

VG1 SAT PLS DERIVED ION SOLAR WIND BROWSE 96SEC V1.0

This data set contains solar wind plasma browse data near the Voyager 1 Saturn encounter. Moment parameters are given. Since only the first 72 or last 72 energy/charge channels are telemetered to Earth from each M-mode spectra, derived parameters change significantly only every other set of spectra so the effective time resolution is 96 second.

VO1/VO2 MARS VISUAL IMAGING SS EXPRMNT DATA REC BROWSE V2.0

This data set includes sub-sampled versions of Viking Orbiter images that are intended to facilitate rapid viewing of the image collection. The image data in these browse images have been reduced in size by sub-sampling the original image by a factor of 4 in both lines and samples. Thus, the data volume has been reduced by a factor of 16. A Viking Orbiter browse image contains 264 lines and 300 samples. A filtering procedure was used in generating the browse images because Viking Orbiter images commonly contain noisy data or are missing data. The brightness value of a pixel in a browse image is the median brightness value of an array of 4 by 4 pixels from the original image. If the 4 by 4 array of original pixels contained zero values, those zero value pixels were not used in determining the median value. Of course, if the entire 4 by 4 array contained zero value pixels, the corresponding pixel in the browse image was assigned a zero value.

VOYAGER 1 SATURN PLASMA DERIVED ELECTRON BROWSE 96 SEC

THIS DATA SET CONTAINS THE THERMAL ELECTRON DENSITY AND TEMPERATURE IN THE PLS ENERGY RANGE (10-5950 EV) FROM VOYAGER 1 AT SATURN DERIVED BY FITTING THE LOW ENERGY ELECTRON COMPONENT WITH A MAXWELLIAN DISTRIBUTION, AND THE MOMENT DENSITY AND TEMPERATURE OF THE HOT ELECTRONS CALCULATED AFTER THE SIGNAL FROM THE THERMAL COMPONENT IS SUBTRACTED FROM THE ELECTRON SPECTRA. IT IS A SUBSET OF THE DATA SET VG1-S-PLS-5-ELE-FIT-96.0SEC WHICH SHOULD BE OBTAINED BEFORE THIS DATA IS USED. SPACECRAFT CHARGING MAY RESULT IN FACTOR OF 2-3 ERRORS IN THE THERMAL ELECTRON DENSITY. THE FIRST SIX COLUMNS ARE THE TIME TAG (YEAR, DAY, HOUR, MIN, SEC, MSEC), COLUMN 7 AND 8 ARE THE FIT DENSITY AND TEMPERATURE OF THE THERMAL ELECTRON COMPONENT, AND 9 AND 10 ARE THE MOMENT DENSITY AND TEMPERATURE OF THE SUPRATHERMAL ELECTRONS. EACH ROW HAS THE FORMAT (6I5,4E12.4). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN SITTLER ET AL. (1983) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

VG2 JUP CRS DERIVED PROTON/ION/ELECTRON FLUX BROWSE V1.0

The Cosmic Ray Subsystem (CRS) was designed for cosmic ray studies. 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.

VG2 JUP EPHEMERIS SYSTEM III (1965) COORDS BROWSE V1.1

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.

VG2 NEP PRA RESAMPLED SUMMARY BROWSE 48SEC V1.0

This dataset consists of edited browse data derived from an original dataset obtained from the Voyager 2 Planetary Radio Astronomy (PRA) instrument in the vicinity of Neptune. Data are provided for 70 instrument channels covering the range from 1.2 kHz to 1326 kHz in uniform 19.2 kHz steps, each 1 kHz wide. Data are included for the period 1989:0:0:0 through 1989:23:59:59.

VOYAGER 2 SATURN PLASMA DERIVED ION FITS BROWSE 96 SEC

THIS DATA SET CONTAINS THE ION DENSITIES, TEMPERATURES, AND VELOCITIES OBTAINED FROM VOYAGER 2 PLS DATA (VOLTAGE RANGE 10-5950 EV/Q) AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS. IT IS A SUBSET OF THE DATA SET VG2-S-PLS-5-ION-FIT-96.0SEC WHICH SHOULD BE OBTAINED BEFORE THIS DATA IS USED. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE OXYGEN. OUTSIDE L=10-12 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. A COMPLETE DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: FIRST 5 COLUMNS ARE TIME TAG (YEAR, DAY, HOUR, MIN SEC.MSEC), FOLLOWED BY PROTON DENSITY (CM-3), PROTON TEMPERATURE (EV), HEAVY ION DENSITY (CM-3), HEAVY ION TEMPERATURE (EV), AND THREE VELOCITY COMPONENTS, (RHO, PHI,Z) IN KM/S. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. EACH ROW HAS THE FORMAT (2I4,2I3, F7.3,7E11.3). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

VG1 JUP EPHEMERIS SYSTEM III (1965) COORDS BROWSE V1.1

This data set consists of Voyager 1 Jupiter encounter ephemeris data in System III (1965) left handed coordinates covering the period 1979-03-03 to 1979-03-16. Two versions, both covering the same time period, but containing slightly different data, are provided.

VG1 SAT EPHEMERIS HELIOGRAPHIC COORDS BROWSE V1.0

Voyager 2 ephemeris data in Heliographic (RTN) coordinates from the Saturn encounter. The data set provides 96 second data generated from SPICE and SEDR.

VG1 SAT EPHEMERIS KRONOGRAPHIC (L1) COORDS BROWSE V1.0

This data set consists of Voyager 1 Saturn encounter ephemeris data in Kronographic (L1) coordinates covering the period 1980-11-10 to 1980-11-18. Two versions, both covering the same time period, but containing slightly different data, are provided. One version was generated by the Voyager MAG team from Voyager SEDR, the other by the PDS/PPI node using the VG1_SAT.TSP and PCK00006.TPC SPICE kernels.

PVO VENUS ONMS BROWSE NEUTRAL DENSITY 12 SECOND V1.0

The instrument was designed to determine the composition of the neutral thermosphere/exosphere of Venus. The term composition includes both the type of neutral gases present and their quantitative amount. The measurements begin at the orbit's periapsis altitude and extend to a limiting altitude at which the ambient signal becomes comparable to the gas background and/or detector measurement threshold. The neutral composition includes helium, atomic nitrogen, atomic oxygen, molecular nitrogen, carbon monoxide and carbon dioxide. The data reduction has been described in Niemann et al. (1980a) and Kasprzak et al. (1980).