AndreaBozzo/ceres-open-data-index huggingface dataset:
NEAR NIS SPECTRA FOR EROS/FLY/BY

This data set contains the NEAR infrared spectrometer (NIS) data for the EROS/FLY/BY phase. The data set begins on 1998-12-23T00:00:00.000 and ends 1998-12-23T23:59:59.999 . The data are raw telemetry data, provided in engineering units, that have been reformatted into FITS file format (NASA Office of Science and Technology (NOST), 100-1.0). In addition to the raw spectrometer data, a calibration file and algorithm are available. This data set is archived as a set of CDROM images as a part of the NEAR EDR volume set.

Tags: __
Organization: National Aeronautics and Space Administration
NEW HORIZONS REX JUPITER ENCOUNTER RAW V2.0

This data set contains Raw data taken by the New Horizons Radio Science Experiment instrument during the Jupiter encounter mission phase. This is VERSION 2.0 of this data set. The REX datasets over the mission include calibrations using known radio sources, Jupiter, and cold sky measurements; operational readiness tests (ORTs); internal test pattern calibration; and prime science radiometry and occultation observations during the Pluto Encounter.

Tags: __
Organization: National Aeronautics and Space Administration
Wind SMS Suite, SupraThermal Ion Composition Spectrometer (SMS/STICS) Proton Distribution Function and Differential Flux, Solar Wind, Level 2 (L2), PT3M Data

The Suprathermal Ion Composition Spectrometer (STICS) is a Time of Flight (TOF) Plasma Mass Spectrometer, capable of identifying Mass and Mass per Charge for incident Ions up to 200 keV/q. It uses an Electrostatic Analyzer to admit Ions of a particular Energy per Charge (E/Q) into the TOF Chamber. The E/Q Voltage is stepped through 32 Values, sitting at each Value for approximately 24 s, to measure Ions over the full E/Q Range of 6 keV/q to 200 keV/q. Ions then pass through a Carbon Foil and TOF Chamber, before finally impacting on a Solid-State Detector (SSD) for Energy Measurement. STICS combines these three Measurements of E/Q, TOF and Residual Energy, producing PHA Words. This Triple-Coincidence Technique greatly improves the Signal to Noise Ratio in the Data. Measurements of E/Q and TOF without Residual Energy also produce PHA Words. These Double-Coincidence Measurements are characterized by better Statistics since Ions whose Energy does not allow them to be registered by the SSD can still be counted in Double-Coincidence Measurements. However, Ion Identification in Double-Coincidence Measurements are limited to a select Number of Ions that are well separated in E/Q - TOF Space. The STICS Instrument provides full 3D Velocity Distribution Functions, through a Combination of multiple Telescopes and Spacecraft Spin. The Instrument includes three separate TOF Telescopes that view three separate Latitude Sectors, as shown in Figure 1. In addition, the WIND Spacecraft Spins, allowing the three Telescopes to trace out a nearly 4π sr Viewing Area. The Longitudinal Sectors are shown in Figure 2. The Solar Direction is in Sectors 8-10 while the Earthward Direction is in Sectors 0-2.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
Wind Energetic Particle Acceleration, Composition and Transport (EPACT)/LEMT 1-Hr H,He,O,Fe Anisotropies for Events

This data set contains hourly resolution anisotropies\nin spacecraft and solar wind frames for 2.5-5 MeV/n H, He, O and Fe \nnuclei, plus 5-8 MeV/n He nuclei.  First-, second- and third-order \nspacecraft-frame anisotropies, and the magnitude and direction angles, \nrelative to the mean magnetic field, of the spacecraft-frame first-order \nanisotropy vectors are given.  Ion spectral parameters used in anisotropy \ndeterminations, namely spectral power law index (gamma), mean energy of \nions in sampled energy range, and ion flux at the mean energy, are given.  \nMany solar wind parameter averages are given, including magnetic field \nmagnitude and direction, solar wind density and flow speed and azimuthal \nangle.  Standard deviations in all hourly averages are also given.  See \nTan et al, Ap.J.,661, 1297-1310, 2007, for discussions of anisotropies, \nreference frames, etc.  As of 10/2011, the data cover 39 1997-2006 multi-\nday intervals that include energetic solar particle events.  ASCII data \nwords are comma-separated.  For a given particle event, there are \nspecies-specific files.  File naming uses the convention XX_a1s_YYYYMMDD, \nwhere XX = H (or Hng), He2 (2.5-5 MeV/n), He5 (5-8 MeV/n), O or Fe, and \nwhere YYYYMMDD is the day of the first record of the file. "Hng" means\nhydrogen - no gamma (as obtained from IMP 8 GME data); but see the \nreadme file cited below on the use of EPACT/LEMT He data as providing\nan alternative power law index.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
CASSINI V/E/J/S/SS RPWS RAW COMPLETE TLM PACKETS V1.0

The Cassini Radio and Plasma Wave Science (RPWS) raw complete data      set includes all RPWS telemetry data for the entire Cassini      mission.  This data set includes raw telemetry values for each      frequency channel for each sensor for all times during the mission      including the two Venus flybys, the Earth flyby, the Jupiter      flyby, interplanetary cruise, and the entire Saturn tour.  Data      for this data set are acquired from the RPWS Low Frequency      Receiver (LFR), Medium Frequency Receiver (MFR), Medium Frequency      Digital Receiver (MFDR) (which can be used to replace MFR band 2      data), High Frequency Receiver (HFR), Sounder, and Langmuir Probe      (LP).  Data are decompressed and internal receiver minipackets are      unsegmented.  This data set is intended to preserve the telemetry      data and is to be used only as a last resort.  Other RPWS archived      data sets are designed to be complete and more easily used.      Browse data sets associated with the other data sets provide a      graphical search of the data included in this data set.  This data      set should be the last used by a user of any of the RPWS archive      as it is in the least user-friendly form.

Tags: __
Organization: National Aeronautics and Space Administration
Wind SMS Key Parameter 4-hour Data

Combined SWICS and STICS data containing 4 hour averaged alpha particle velocity, C/O abundance ratio, and carbon and oxygen ionization temperatures. Time is for the start of the averaging interval. Computed are the average alpha velocity, average C/O abundance ratio, average carbon ionization temperature (in million degs K) from C6 and C5 (using the tables of Arnaud and Rothenflug, 1985), the average oxygen ionization temperature from O7 and O6 (in million degs K, using tables of Arnaud and Rothenflug, 1985). These averages are made over 4 hours. He velocity and He kinetic temperature are computed every 3 minutes and are contained in the K1 CDF. References: Space Science Reviews 71:79-124, 1995, Kluwer Academic Publishers, Belgium Instrument consist of: Solar Wind Ion Composition Spectrometer (SWICS); high resolution mass spectrometer (MASS); Supra-Thermal Ion Composition Spectrometer (STICS) and common DPU

Tags: energeticparticles, ioncomposition
Organization: National Aeronautics and Space Administration
ICE SOLAR WIND PLASMA ELECTRON ANALYSER DATA V1.0

These data were obtained from the LANL plasma experiment on ICE (Principal Investigator: S.J. Bame assistance from K. Sofaly and S. Kedge). The instrument measures the 2-D electron distribution function in one spacecraft rotation (3 s) once every 24 s, by obtaining 16 evenly spaced energy spectra, each with 15 contiguous levels covering the energy range 8.5 eV to 1140 eV. From these 2-D distributions the density, velocity, and temperature of the electrons are then derived. A 2-D temperature matrix is calculated which is subsequently diagonalized. Then nominally the maximum temperature corresponds to the parallel temperature and the minimum temperature corresponds to the perpendicular temperature. This is done independently of the magnetic field measurements however, the direction of maximum temperature determined in this manner is usually found to be within 15 degrees of the magnetic field direction inferred from the magnetometer measurements. The time resolution is 24 sec from the start of Day 253 (September 10) until Day 255 (September 12), 18:38. At that time the bit rate dropped from 1024 to 512 bps, and the nominal time resolution went to 48 sec.

Tags: __
Organization: National Aeronautics and Space Administration
Wind Magnetic Field Investigation (MFI) Composite Data in RTN Coordinates

Wind MFI composite data in RTN coordinates. The files contain multiple time resolution data: 3-second, 1-minute, and 1-hour. Final Version 5 data are accessible to within about 3 months of current date, newly defined Version 4 data (with final Bz offsets and not-yet-final spacecraft position vectors) between 3 months and about 2 weeks of current date, and newly defined Version 3 data (with the most recently determined Bz offset value, not yet final for the Version 3 interval) from 2 weeks to about 2 days of current.

Tags: magneticfield
Organization: National Aeronautics and Space Administration
APOLLO 15 LSRP SOIL MECHANICS DATA V1.0

This dataset contains tables of raw readings and reduced data from all six runs on 01 August 1971 of the Lunar Self-Recording Penetrometer (LSRP) on the surface of the Moon for the Apollo 15 Soil Mechanics experiment. Supporting documentation includes digitized scans in JPEG and PDF format of the original LSRP soil mechanics dataset on microfilm, videos and transcripts of the LSRP as it was operated on the Moon, diagrams and maps of the experiment areas, and photography of the Apollo 15 Station 8 where the experiment was performed.

Tags: __
Organization: National Aeronautics and Space Administration
Wind Magnetic Field Investigation (MFI) Full Resolution Data in RTN Coordinates

This data product contains Wind MFI full resolution magnetic field magnitude and RTN Cartesian components. Time resolution is typically 0.046s or 0.092s from launch through 1997, and is 0.092s thereafter. Final Version 5 data are accessible to within about 3 months of current date, newly defined Version 4 data (with final Bz offsets and not-yet-final spacecraft position vectors) between 3 months and about 2 weeks of current date, and newly defined Version 3 data (with the most recently determined Bz offset value, not yet final for the Version 3 interval) from 2 weeks to about 2 days of current.

Tags: magneticfield
Organization: National Aeronautics and Space Administration
Wind Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates

Wind Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ‘‘Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,’’ J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405. There are now two version of this data set. An off set has been found in the Wind MFI Bz component that is present after November 2004. Version 2 has this offset removed. Prof. R.L. McPherron determined the correction to be Bz = Bz - (-0.000000130406219.*odoy.*odoy + 0.000576303146.*odoy + 0.679940509 + 0.3215*cos(2*pi*(doy-171)/366)) where doy is the day of the year in units of days and odoy is the days sinces Jan 1, 1999 00:00:00 UT in units of days.

Tags: bow-shock, magnetic-fields, magneticfield-1-min, magnetometer, magnetopause, magnetotail, propagated-solar-wind-data, solar-wind, wind
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3                                     EXTENDED MISSION 8 4326 V1.0

This is a Mars Express                                     Radio Science data set, collected                                     during the extended mission phase                                     2023-01-01 to 2023-12-31.                                     It is a Occultation                                     measurement and covers the time                                     2023-08-19T05:43:48.100 to                                     2023-08-19T06:05:56.000.

Tags: __
Organization: National Aeronautics and Space Administration
Wind Magnetic Fields Instrument (MFI) Magnetic Field Vector and Spacecraft Position, Key Parameter (K0), 92 s Data

Wind Magnetic Fields Investigation, MFI, Key Parameter magnetic field data in GSE and GSM coordinates.\n\nReferences:\n\n* 1. Panetta P, GSFC, GGS Wind MFI Operators Manual, September 15, 1992.\n* 2. Computer Sciences Corporation, Data Format Control Document, DFCD, between the International Solar-Terrestrial Physics, ISTP, program information investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992.\n* 3. Behannon, K.W., International Solar Terrestrial Physics, ISTP, program investigator data analysis requirements for Wind and Geotail spacecraft magnetometer experiment, September 1987.

Tags: ephemeris, instrumentstatus, magneticfield
Organization: National Aeronautics and Space Administration
Wind Energetic Particle Acceleration Composition Transport (EPACT) SupraThermal Energetic Particle Telescope (STEP) Differential, Directional Iron Fluxes, 10 min Data

The EPACT Instrument on Wind STEP - SupraThermal Energetic Particle Telescope measures Ion Fluxes of Protons (H) in 0.12.5 MeV Energy Range and He-Fe Nuclei in the ~0.032 MeV/nucleon Energy Ranges in two identical Telescopes, each with a Geometrical Factor of 0.4 cm^2 sr and a rectangular Field of View with an Angular Acceptance of 44° in Azimuth and 17° in Polar Angle.

Tags: energeticparticles, ephemeris, magneticfield, thermalplasma
Organization: National Aeronautics and Space Administration
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.

Tags: __
Organization: National Aeronautics and Space Administration
Wind Energetic Particle Acceleration, Composition and Transport (EPACT)/LEMT 1-Hr Spin-Sectored H,He,O,Fe Counts for Events

This data set contains hourly counts of H, He, O \nand Fe nuclei in 16 look directions about the spacecraft spin axis.  \nCounts for each of the four species are given at 2.5-5 MeV/n, and an \nadditional count is given for 5-8 MeV/n He.  As of 10/2011, the data \ncover 39 1997-2006 multi-day intervals that include energetic solar \nparticle events.  ASCII data words are comma-separated.  For a given \nparticle event, there are species-specific files.  File naming uses \nthe convention XX_sec_YYYYMMDD, where XX = H, He2 (2.5-5 MeV/n), \nHe5 (5-8 MeV/n), O or Fe, and where YYYYMMDD is the day of the first \nrecord of the file.  Sectoring is defined with respect to the \necliptic plane projection of the concurrently measured magnetic\nfield vector.  The edge of sector #1 is coincided with the projection \nof B on the ecliptic plane, so phi value of the center of sector i \nis phiB+11.25+(i-1)*22.5 deg, where phiB is the longitudinal angle \nof B.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P VIRTIS 2 ESCORT 3 MTP020 V2.0

This release contains the digital numbers (DN) contained in the telemetry (TM) packages of the VIRTIS instrument on board of the spacecraft Rosetta. This volume contains data at the vicinity of comet 67P, from the ESCORT 3 MTP020 phase, which occurred from 2015-08-26 to 2015-09-23. This version of the dataset (2.0) is produced by a fixed EGSE software. The old version of the software produced incomplete products, reduced by one line

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RPCIES 3 ESC3 V1.0

This dataset contains CALIBRATED DATA of the Rosetta RPCIES instrument taken during the comet escort 3 phase (ESC3). The target of this phase was comet 67P/CHURYUMOV-GERASIMENKO 1 (1969 R1). Included are the data taken between 01 Jul 2015 and 21 Oct 2015.

Tags: __
Organization: National Aeronautics and Space Administration
Wind 3DP Weimer Propagated 60 s Resolution in GSE Coordinates

Wind 3DP propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution data in GSE coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ‘‘Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,’’ J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405. There are now two version of this data set. An off set has been found in the Wind MFI Bz component that is present after November 2004. Version 2 has this offset removed. Prof. R.L. McPherron determined the correction to be Bz = Bz - (-0.000000130406219.*odoy.*odoy + 0.000576303146.*odoy + 0.679940509 + 0.3215*cos(2*pi*(doy-171)/366)) where doy is the day of the year in units of days and odoy is the days sinces Jan 1, 1999 00:00:00 UT in units of days.

Tags: 1-min, 3dp, bow-shock, magnetopause, magnetotail, plasma-data, propagated-solar-wind-data, solar-wind, thermalplasma-1-min, wind
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 3 3250 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2010-01-01 to 2012-12-31. It is a Global Gravity measurement and covers the time 2012-05-29T06:22:02.000 to 2012-05-29T09:39:11.500.

Tags: __
Organization: National Aeronautics and Space Administration
Wind Energetic Particle Acceleration Composition Transport (EPACT) SupraThermal Energetic Particle Telescope (STEP) Differential, Directional Helium Fluxes, 10 min Data

The EPACT Instrument on Wind STEP - SupraThermal Energetic Particle Telescope measures Ion Fluxes of Protons (H) in 0.12.5 MeV Energy Range and He-Fe Nuclei in the ~0.032 MeV/nucleon Energy Ranges in two identical Telescopes, each with a Geometrical Factor of 0.4 cm^2 sr and a rectangular Field of View with an Angular Acceptance of 44° in Azimuth and 17° in Polar Angle.

Tags: energeticparticles, ephemeris, magneticfield, thermalplasma
Organization: National Aeronautics and Space Administration
ULYSSES JUPITER HISCALE COMPOSITION                                        APERTURE ION COUNTS

This data set consists of HISCALE                                      Composition Aperture (WARTD) ion                                      counts. These measurements were taken                                      during the Ulysses Jupiter encounter                                      1991-12-31 to 1992-02-16, and include                                      1 hour averaged inbound cruise data                                      (1991-12-31 to 1992-02-01), and 15                                      minute averaged encounter data                                      (1992-02-02 to 1992-02-16).

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P NAVCAM 3 PRELANDING MTP007 V1.0

This dataset contains ROSETTA NAVCAM RADIOMETRICALLY CALIBRATED DATA of the PRELANDING MTP007 Phase from 02 Sep. 2014, 11:34:31 to 23 Sep. 2014, 09:40:03 when at the vicinity of target 67P/CG.

Tags: __
Organization: National Aeronautics and Space Administration
Wind Energetic Particle Acceleration, Composition and Transport (EPACT) 92s KP Fluxes

This set of key parameter flux data from the Wind EPACT (Energetic Particles: Acceleration, Composition and Transport) telescopes contains fluxes of protons (19-72 MeV in 2 energy bins), He nuclei (0.08-72 MeV/n in 5 bins), CNO nuclei (80-640 MeV/n in 2 bins), O nuclei (3.2-6.2 MeV/n in 1 bin), Fe nuclei (0.08-6.2 MeV/n in 3 bins) and 1-10 MeV electrons, each averaged over 92 seconds.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration