AndreaBozzo/ceres-open-data-index huggingface dataset:
MARS EXPRESS SUN MRS 1/2/3                                     EXTENDED MISSION 8 4403 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 Solar Conjunction                                     measurement and covers the time                                     2023-12-22T03:51:17.000 to                                     2023-12-22T09:10:20.000.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 1 0454 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 1 phase 2014-11-20 to 2015-03-10. It is a Global Gravity measurement at the comet 67P and covers the time 2014-11-24T02:53:05.000 to 2014-11-24T13:20:37.000.

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Organization: National Aeronautics and Space Administration
DAWN GRAND MAP CERES  HYDROGEN MAP V1.0

A global map of the  concentration of hydrogen within the regolith of asteroid 1 Ceres  on twenty-degree quasi-equal-area pixels is provided. Hydrogen  concentrations were determined from thermal+epithermal neutron  counting data acquired by the NASA Dawn mission's Gamma Ray and Neutron Detector (GRaND) while in low altitude mapping orbit, about 385 km from Ceres' surface (about 0.8 body radii altitude). The concentrations are representative of Ceres's bulk regolith to depths up to a few  decimeters with a spatial resolution of about 600-km  full-width-at-half-maximum of arc length on the surface. The methods  used to determine hydrogen concentration are described by  PRETTYMANETAL2017.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 PRELANDING 0378 V1.0

This is a Rosetta Radio Science data set, collected during the PRELANDING phase 2014-01-21 to 2014-11-18. It is a Global Gravity measurement at the comet 67P and covers the time 2014-10-22T15:48:15.000 to 2014-10-22T22:57:04.000.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 1 0450 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 1 phase 2014-11-20 to 2015-03-10. It is a Global Gravity measurement at the comet 67P and covers the time 2014-11-22T03:34:50.000 to 2014-11-22T13:25:27.500.

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Organization: National Aeronautics and Space Administration
JNO J JED 3 CDR V1.0

Abstract                                                                      ========                                                                        This data set consists of the JUNO JEDI (Jupiter Energetic-Particle           Detector) calibrated observations, also known as CDRs. The system             is made up of 3 instrument subsystems (pucks) aligned in three                directions on the spinning JUNO spacecraft. The pucks each have 6 look        directions (telescopes) with a time of flight (TOF) and a deposited           energy detection (SSD) system.  In addition, the pulse height of the          signal in the TOF system can be used for energy measurement. The              instruments can be operated in a variety of modes, differing in the           way they use and combine these measurements. More details are available       in the INSTRUMENT.CAT file and the JEDI SIS.                                                                                                                The CDRs are organized in files covering one day of spacecraft event          time (SCET). There are potentially 10 different files per puck,               corresponding to the available data gathering modes: HIERSESP,                HIERSISP, HIERSTOFXER, HIERSTOFXPHR, LOERSESP, LOERSISP, LOERSTOFXER,         LOERSTOFXPHR, NONPTOFXER, NONPTOFXPHR. Depending on how the pucks are         operated, not all data types will be available for all pucks for any          particular time range.                                                                                                                                      All the measured quantities present in the uncalibrated data files            (EDRs) are present here in three forms: counts per accumulation (the          same numbers as in the EDRs), counts per second (this number may be           corrected for instrument saturation and background), intensity (counts        per second per steradian per cm2 per keV). Additional support                 quantities are also included for the convenience or enlightenment of          the end user.

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Organization: National Aeronautics and Space Administration
Wind Solar Wind Experiment (SWE) Electron Pitch-Angle Distributions (6-12s rate) (VEIS-era Mode)

Wind SWE electron pitch angle product providing electron fluxes at 30 directional bins relative to the instantaneous magnetic field direction at 16 different energy levels from the old mode (VEIS-era) of the electron instrument. The electron pitch-angle distributions included in this data set are derived from sorting, by pitch (wrt B) and energy, the solar wind electron distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955). Pitch-angle distrubutions, organized by energy, are computed from 3s measurements which are spaced either 6s or 12s in time. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the electron pitch-angle distributions reported in this data set. For each 'energy spectrum', observations are made at 16 energy channels ranging from about 10 eV to as much as 3 keV. The exact energies at which observations are made is time-varying, and this data set reports the energy each channel observes (along with the observations themselves) at any time. The observations made at each energy are sorted into pitch-angle bins, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). A "spin-averaged" set of observations (aggregated from all pitch-angle bins, each energy) is also reported, one value for each energy channel. The value reported for any bin (including the spin-averaged "energy bins") is given as a phase-space density, f [#/{cc*(cm/s)^3}], averaged over contributing detectors. The data set reported here contains: f_pitch_E00, f_pitch_E01, f_pitch_E02, f_pitch_E03, f_pitch_E04, f_pitch_E05, f_pitch_E06, f_pitch_E07, f_pitch_E08, f_pitch_E09, f_pitch_E10, f_pitch_E11, f_pitch_E12, f_pitch_E13, f_pitch_E14, f_pitch_E15 (the pitch-angle distributions for each energy channel, with 30 pitch-angle bins for each), and f_pitch_SPA (with 16 spin-averaged energy bins). For reference, the electron speeds ( V , in cm/s) corresponding to the energy channels used, are reported in this data set.

Tags: thermalplasma
Organization: National Aeronautics and Space Administration
Chang SSM/I Derived Monthly Rain Indices 5 x 5 degree V2.3 (RAIN_CHANG) at GES DISC

These data are transitioned to a state of permanent preservation. They are available upon request. More advanced datasets have been developed since. One recommended replacement is the GPCP (doi: 10.5067/DBVUO4KQHXTK) product developed under the MEaSUREs project. Futhermore, the NASA Precipitation Measurement Missions Project released newly processed SSM/I datasets as output from the GPROF (Goddard Profiling Algorithm). (doi: 10.5067/GPM/SSMI/F11/GPROFCLIM/2A/05, 10.5067/GPM/SSMI/F11/GPROFCLIM/3A-MONTH/05, 10.5067/GPM/SSMI/F11/GPROFCLIM/3A-DAY/05) The "RAIN_CHANG" SSM/I Derived Oceanic Monthly Rainfall Indices data set was an early Global Precipitation Climatology Project (GPCP) product. Monthly rainfall indices over the oceans were derived from Special Sensor Microwave Imager (SSM/I) data from the Defense Meteorological Satellite Program (DMSP) satellites F8 and F11, on channels 19 and 22 V. The data set covered the period from July 1987 to December 1995. The monthly rainfall indices are on a 5 degree by 5 degree grid extending from 50 N to 50 S. The Wilheit, Chang and Chiu (1991) method used to derive the indices gives valid values only over ocean areas. Land pixels (including island pixels) and erroneous pixels return a -10 flag. The data are stored on a 72 x 20 grid. Grid point (1,1) contains the index for 45-50 N, 0-5 E, grid point (2,1) contains the index for 45-50 N, 5-10 E, ... and grid point (72,20) contains the index for 45-50 S, 175-180 W. In the data set, each month starts with an ASCII header to identify the year and month. The data is in 10F8.1 format. Each value is the average of AM and PM estimates and corrected for beam filling error. The equation used is: (AM PM)/2.0 * 1.8. Land pixels are set to -10.0. Also there are 33 pixels blocked out due to island contamination (-10.0). If the rain retrieval did not converge, a -10.0 is assigned to the pixel. The objective of this data set was to provide a long term monthly rainfall data set to be used in EOS global change and GEWEX related research.

Tags: earth-science-precipitation-atmosphere-liquid-precipitation-rain-oceanic-precipitation, earth-science-precipitation-atmosphere-precipitation-amount
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 1 0595 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 1 phase 2014-11-20 to 2015-03-10. It is a Global Gravity measurement at the comet 67P and covers the time 2015-02-21T22:31:25.000 to 2015-02-22T00:42:59.000.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P OSIWAC 4 PRL-MTP006 RDR V1.0

This CODMAC level 4 data set contains radiometric calibrated and geometric distortion corrected (resampled) image data in W/m^2/sr/nm acquired by the OSIRIS Wide Angle Camera during the PRELANDING phase of the Rosetta mission, covering the period from 2014-08-01T10:00:00.000 to 2014-09-02T09:59:59.000.

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Organization: National Aeronautics and Space Administration
Wind Plasma and Radio Waves (WAVES) Time Domain Sampler (TDS) Dust Impact, Level 3, 1 s Data

Wind WAVES Time Domain Sampler, TDS, Dust Data File References: 1) Bougeret, J.-L., et al., WAVES: The Radio and Plasma Wave Investigation on the Wind Spacecraft, Space Sci. Rev., 71, 231-263, 1995, doi:10.1007/BF00751331. 2) Malaspina, D.M., M. Horanyi, A. Zaslavsky, K. Goetz, L.B. Wilson III, and K. Kersten, Interplanetary and Interstellar Dust observed by the Wind/WAVES Electric Field Instrument, Geophys. Res. Lett., 41, 266-272, 2014, doi:10.1002/2013GL058786. 3) Malaspina, D.M., and L.B. Wilson III, A Database of Interplanetary and Interstellar Dust Detected by the Wind Spacecraft, J. Geophys. Res., 121, 9369-9377, 2016, doi:10.1002/2016JA023209.

Tags: electricfield
Organization: National Aeronautics and Space Administration
VG2 NEP PWS RESAMPLED SUMMARY SPECTRUM ANALYZER 48SEC V1.0

This data set consists of 48-second calibrated, averaged wave      electric field intensities from the Voyager 2 Plasma Wave      Receiver spectrum analyzer obtained in the vicinity of the      Neptunian magnetosphere.  For each 48-second interval, a geometric      average field strength is determined for each of the 16 spectrum      analyzer channels whose center frequencies range from 10 Hertz to      56.2 kiloHertz and which are logarithmically spaced in frequency,      four channels per decade.

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Organization: National Aeronautics and Space Administration
ROSETTA-LANDER 67P COSAC 3 RBD V1.0

This archive contains calibrated data (CODMAC level 3) from the COSAC instrument onboard ROSETTA Lander, acquired during the RBD (comet) phase. It also contains documentation which describes the COSAC experiment. The primary target is the comet 67P/CHURYUMOV-GERASIMENKO. The data archived in this data set conform to the Planetary Data System (PDS) Standards, Version 3.6.

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Organization: National Aeronautics and Space Administration
CASSINI RSS RAW DATA SET - SROC19 V1.0

The Cassini Radio Science Saturn Ring and Atmospheric Occultation experiments (SROC19) Raw Data Archive is a time-ordered collection of radio science raw data acquired on April 12, May 10, 20, 31, and June 24, 2013, during the Cassini Extended Extended Mission.

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Organization: National Aeronautics and Space Administration
Russian MSU Zond-3 Heliopsheric Data

This set of heliospheric data in ASCII contains measurements of energetic particles by the KS-18 instrument onboard the third Russian space probe of the Zond series at heliocentric distances larger than 1 AU.  It includes proton flux intensities at >30 MeV energy from Sun (gas-discharge counter) and at 1-5 MeV energy arriving from the direction perpendicular to the Sun-spacecraft line (stand-alone SSD sensor of 35 micron Si). Subdirectory /lownoise contains the same measured data but in its extra-rectified variant.  Besides the trajectory data in two coordinate systesms, there are overview plots in GIF.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER COMET ESCORT OSINAC 3 RDR MTP 011 V1.0

This data set contains calibrated images acquired by the OSIRIS Narrow AngleCamera during the escort phase of the Rosetta mission at the comet 67P,covering the period from 2014-12-19 to 2015-01-13.

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Organization: National Aeronautics and Space Administration
VEGA2 ORIGINAL MISCHA DATA SUBMISSION

This data set includes the original Vega 2 MISCHA data delivery to PDS. The data were provided by Magda Delva of the MISCHA instrument team. The data are provided in ASCII format as well as the original IBM/PC binary format in which they were delivered to PDS. This data set was created for purposes of 'safing' these data. Significant concerns exist with regards to data quality. Instrument offsets (zero-levels) were highly unstable after 21 Feb 1986. In addition the instrument failed just prior to closest approach to comet Halley.

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Organization: National Aeronautics and Space Administration
Wind Radio/Plasma Wave, (WAVES) Hi-Res Parameters CDF

Wind Waves RAD2, RAD1, and TNR data in CDF format. RAD1 RAD1 is the low frequency radio astronomy receiver. It sweeps over the range of 20 to 1040 kHz with as many as 256 channels. However, some of the time the number of channels is restricted to 16 or 32 so that direction of arrival and polarization information can be obtained. RAD2 RAD2 is the high frequency radio astronomy receiver. It sweeps over the range of 1.075 to 13.825 MHz with as many as 256 channels. However, some of the time the number of channels is restricted to 16 or 32 so that direction of arrival and polarization information can be obtained. TNR The thermal noise receiver (TNR) is designed to actively track the solar wind plasma frequency. TNR consists of 5 overlapping bands. Each band covers 2 octaves, with the next band beginning at the mid point of the lower band. The overall frequency range is 4 - 256 kHz. Usually the tnr is operated in a mode where the first, third and fifth bands are sampled, but occassionally the instrument is driven by neural network software which tries to pick the one band containing the plasma frequency. For more information: The Radio and Plasma Wave Investigation on the Wind Spacecraft, Sp.Sci.Rev.,Vol 71, pg, 231-263,1995

Tags: akr, auroral-hiss, auroral-kilometric-radiation, chorus, continuum-radiation, myriametric-radiation, plasmaspheric-hiss, solar-radio-burst, spectrogram, spectrum-dynamic-spectrogram, terrestrial-kilometric-radiation, tkr, type-ii-solar-radio-burst, type-iii-solar-radio-burst, uhr, upper-hybrid-resonance, vlf-station, vlf-transmitter, waves-passive, whistler
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 PRELANDING 0280 V1.0

This is a Rosetta Radio Science data set, collected during the PRELANDING phase 2014-01-21 to 2014-11-18. It is a Global Gravity measurement at the comet 67P and covers the time 2014-09-08T17:36:15.000 to 2014-09-09T00:00:10.000.

Tags: __
Organization: National Aeronautics and Space Administration
Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Energy-Resolved Pitch-Angle Distributions (ERPAs), Level 2 (L2), 30-minute Data in Magnetosphere

The data include Wind STICS 30-minute Energy-Resolved Pitch-Angle Distributions (ERPAs) for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the magnetosphere. ERPAs organize the data by the angle relative to the magnetic field vector direction, in 7.5 degree bins. The energy separation is preserved at the native resolution of the E/q bins. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf.\nThe 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/e. 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 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. 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 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π steradian 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: ioncomposition
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3                                     EXTENDED MISSION 8 4322 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                                     2023-08-14T06:57:40.100 to                                     2023-08-14T07:19:47.800.

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Organization: National Aeronautics and Space Administration
VG1 J/S/SS PWS RESAMP SPECTRUM ANALYZER HOUR AVG V1.0

This data set contains hourly RMS averages and peaks of calibrated     electric field measurements taken by the spectrum analyzer component of     the Plasma Wave System (PWS) onboard Voyager 1 for the entire mission.     Most noise spikes were removed prior to processing in order to provide     more reliable values.  Each record contains the spacecraft event time at     the beginning of the processed hour, 16 RMS electric field averages     corresponding to the 16 frequency channels of the instrument ranging from     50 Hz to 10 kHz, and 16 maximum values in the same units for the same     frequencies.

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Organization: National Aeronautics and Space Administration
GALILEO ORBITER JUPITER RAW MAGNETOMETER DATA V1.0

This data set contains raw magnetic field data acquired by the       Galileo Orbiter magnetometer at Jupiter. The data set covers the       time period from 1995-11-06T00:21:30 UT (Jupiter approach) until       the end of mission (March 2003). The raw magnetometer data set       includes various forms of data: recorded high time resolution,       real-time survey (RTS), optimal averager (opt/avg), snapshot, and       the calibration parameters required to generate processed data       products. In addition corrected rotor angles and spacecraft       relative clock and cone angles are provided to simplify future       calibration and reprocessing of the data.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 1 0525 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 1 phase 2014-11-20 to 2015-03-10. It is a Global Gravity measurement at the comet 67P and covers the time 2015-01-07T12:03:20.000 to 2015-01-07T23:51:21.500.

Tags: __
Organization: National Aeronautics and Space Administration
Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Moments, Level 2 (L2), 3-minute Data in Magnetosphere

The data include Wind STICS 3-minute density (0th moment) and mean value of the energy distribution (1st moment), together with their statistical errors, for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the magnetosphere. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf.\nThe 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/e. 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 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. 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 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π steradian 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: ioncomposition
Organization: National Aeronautics and Space Administration