AndreaBozzo/ceres-open-data-index huggingface dataset:
Wind SWE Weimer Propagated 60 s Resolution data in GSM Coordinates

Wind SWE propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution 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.

Tags: bow-shock, magnetopause, magnetotail, plasma-data, solar-wind, thermalplasma-1-min, wind
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3                                     EXTENDED MISSION 8 4313 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                                     2023-08-02T08:30:39.000 to                                     2023-08-02T08:52:47.100.

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Organization: National Aeronautics and Space Administration
Wind SWE Weimer Propagated 60 s Resolution data in GSE Coordinates

Wind SWE 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.

Tags: bow-shock, magnetopause, magnetotail, plasma-data, solar-wind, thermalplasma-1-min, wind
Organization: National Aeronautics and Space Administration
GO E PWS EDITED EARTH 2 WAVEFORM RECEIVER V1.0

This data set includes wideband waveform measurements from the Galileo    plasma wave receiver obtained during the second Earth encounter.  These    measurements are electric or magnetic waveforms obtained by rapidly    sampling the potential at the input to the receiver from either the    electric dipole antenna or the magnetic search coil antenna.  The sample    rates are 201,600 s^-1, 25,200 s^-1, or 3,150 s^-1 taken through bandpass    filters of 80, 10, or 1 kHz, respectively.

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Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RPCMIP 3 ESC4 V1.0

This archive contains data from the RPC-MIP instrument onboard ROSETTA Orbiter, acquired during the comet escort part 3 phase. The primary target was comet 67P/C-G. It also contains documentation which describes the MIP experiment. The data archived in this data set conform to the Planetary Data System Standards, Version 3.6.

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Organization: National Aeronautics and Space Administration
Wind Predicted Attitude, 10 min Data, Spin Axis Orientation Angles in GCI, GSE and GSM Coordinates

Wind Predicted Attitude Body Spin Rate and Spin Axis Orientation Right Ascension and Declination Angles in Geocentric Celestial Inertial, GCI, Geocentric Solar Ecliptic, GSE, and Geocentric Solar Magnetospheric, GSE, Coordinates

Tags: ephemeris
Organization: National Aeronautics and Space Administration
MESSENGER MERCURY RSS/MLA LEVEL 5 DERIVED DATA V1.0

This data set contains archival results from radio science investigations conducted during the MESSENGER mission. Radio measurements were made using the MESSENGER spacecraft and Earth-based stations of the NASA Deep Space Network (DSN). The data set includes three products: 1) high-resolution spherical harmonic models of Mercury's gravity field. These results were derived from raw radio tracking data; 2) measurements of Mercury's radius at several locations around the planet. These radii are derived from radio occultations; and 3) spherical harmonic models of Mercury's surface shape. Both Mercury Laser Altimeter (MLA) data and occultation data were used to generate the shape models. The investigations were conducted by personnel at JHU/APL, GSFC, and JPL.

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Organization: National Aeronautics and Space Administration
ISEE-3 Solar Wind Plasma Weimer Propagated 60 s Resolution in GSM Coordinates

ISEE-3 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma 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.

Tags: bow-shock, isee-3, magnetopause, magnetotail, plasma-data, propagated-solar-wind-data, solar-wind, thermalplasma-1-min
Organization: National Aeronautics and Space Administration
ULYSSES DUST DETECTION SYSTEM V3.1

This data set contains the data from the Ulysses dust detector system (UDDS) from start of mission through the end of mission, 1990-2007. (As the dust detector was turned off after Nov. 30, 2007, this is the last date for which UDDS data is recorded.) Included are the dust impact data, noise data, laboratory calibration data, and location and orientation of the spacecraft and instrument.

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Organization: National Aeronautics and Space Administration
ISEE-3 Solar Wind Weimer Propagation Details at 1 min Resolution

ISEE-3 Weimer propagated solar wind data and linearly interpolated time delay, cosine angle, and goodness information of propagated data at 1 min Resolution. 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.

Tags: bow-shock, isee-3, magneticfield-1-min, magnetopause, magnetotail, propagation-information, propagation-support-data, solar-wind
Organization: National Aeronautics and Space Administration
VG2 NEP PWS RAW EXPERIMENT WAVEFORM 60MS V1.0

This data set consists of electric field waveform samples from the      Voyager 2 Plasma Wave Receiver waveform receiver obtained during      the Neptune encounter. The waveforms are collections of 4-bit      samples of the electric field measured by the dipole electric antenna      at a rate of 28,800 samples per second.  1600 samples are collected      in 55.56 msec followed by a 4.44-msec gap. Each 60-msec interval      constitutes a line of waveform samples. The data set includes about 271      frames of waveform samples consisting of up to 800 lines, each.

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Organization: National Aeronautics and Space Administration
VG2 JUP MAG RESAMPLED HELIOGRAPHIC (RTN)COORDS 1.92SEC V1.0

This data set includes Voyager 2 Jupiter     encounter magnetometer data given in Heliographic coordinates and     averaged from the 60 ms instrument sample rate to a 1.92 second resampled     rate. The data set consists of the following columns: 1) UT of the sample     in the format yyyy-mm-ddThh:mm:ss.sssZ, 2) spacecraft clock     (m65536:mod60:fds-line), 3) magnetometer id (1 = LFM, 2 = HFM), 4) Br     (radial, Sun to spacecraft, B-field component), 5) Bt (azimuthal B-field     component, positive in the direction of planetary orbital motion),     6) Bn (North/South B-field component, positive northward), 7) Bmag     (magnitude of the averaged components), 8) avg_Bmag (average of the     magnetic field magnitudes), 9) delta (latitude = arcsin(Bn/Bmag)),     10) lambda (longitude = 180. - atan(Bt/Br)), 11-13) rms vectors,     14) npts (number of points in average). All magnetic field observations     are measured in nanoTesla.  All of the magnetic field data are calibrated     (see the instrument calibration description for more details).

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Organization: National Aeronautics and Space Administration
DEEP IMPACT HRII/HRIV/MRI INSTRUMENT TEMPERATURES V1.0

Resampled (raw, averaged) temperature measurements from 27 sensors located in the HRII, HRIV, and MRI instruments and on the HRI and MRI telescopes, instrument platform, and solar wings of the Deep Impact flyby spacecraft. The data begin on 15 January 2005, three days after launch, and continue through 9 July 2005, five days after the encounter with comet 9P/Tempel 1.

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Organization: National Aeronautics and Space Administration
ISEE-3 Solar Wind Plasma Weimer Propagated 60 s Resolution in GSE Coordinates

ISEE-3 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma 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.

Tags: bow-shock, isee-3, magnetopause, magnetotail, plasma-data, propagated-solar-wind-data, solar-wind, thermalplasma-1-min
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3                                     EXTENDED MISSION 8 4317 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                                     2023-08-06T17:18:31.500 to                                     2023-08-06T17:40:39.000.

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Organization: National Aeronautics and Space Administration
Wind Hot Plasma and Charged Particles (3DP) Electron Electrostatic Analyzer (EESA) Low, Omnidirectional Flux Spectra, 5 eV to 1100 eV, 24 s Data

Wind Three-Dimensional Particle, 3DP, instrument, Electron Electrostatic Analyzer, EESA, Low Energy Spectra, ELSP, omni directional electron differential number flux spectra, 3 eV to 30 keV.

Tags: energeticparticles
Organization: National Aeronautics and Space Administration
Coastal Wetland Elevation and Carbon Flux Inventory with Uncertainty, USA, 2006-2011

This dataset provides maps of coastal wetland carbon and methane fluxes and coastal wetland surface elevation from 2006 to 2011 at 30 m resolution for coastal wetlands of the conterminous United States. Total coastal wetland carbon flux per year per pixel was calculated by combining maps of wetland type and change with soil, biomass, and methane flux data from a literature review. Uncertainty in carbon flux was estimated from 10,000 iterations of a Monte Carlo analysis. In addition to the uncertainty analysis, this dataset also provides a probabilistic map of the extent of tidal elevation, as well as the geospatial files used to create that surface, and a land cover and land cover change map of the coastal zone from 2006 to 2011 with accompanying estimated median soil, biomass, methane, and total CO2 equivalent annual fluxes, each with reported 95% confidence intervals, at 30 m resolution. Land cover was quantified using the Coastal Change Analysis Program (C-CAP), a Landsat-based land cover mapping product.

Tags: earth-science-carbon-flux-climate-indicators, earth-science-ecosystems-biosphere-aquatic-ecosystems-wetlands, earth-science-ecosystems-biosphere-terrestrial-ecosystems-wetlands, earth-science-geomorphic-landforms-processes-land-surface-coastal-processes, earth-science-soils-land-surface-carbon, earth-science-vegetation-biosphere-carbon
Organization: National Aeronautics and Space Administration
VG1 LECP 0.4S HIGH RESOLUTION SATURN FAR ENCOUNTER DATA

This far 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        vicinity of Saturn. This instrument measures the intensities        of in-situ charged particles ( >15 keV electrons and >30 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 0.4 second rate measurements within 1/8 of the LECP        instrumental motor rotation period (the angular scanning        periods, or step period).

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Organization: National Aeronautics and Space Administration
ISEE-3 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates

ISEE-3 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 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.

Tags: bow-shock, isee-3, magnetic-fields, magneticfield-1-min, magnetometer, magnetopause, magnetotail, propagated-solar-wind-data, solar-wind
Organization: National Aeronautics and Space Administration
NIMS EXPERIMENT DATA RECORDS: EARTH/MOON 1 AND 2 ENCOUNTERS

NIMS Experiment Data Record (EDR) files contain raw data from the Galileo Orbiter Near-Infrared Mapping Spectrometer (CARLSONETAL1992). This raw data requires considerable processing before it is readily amenable to science analysis. The EDRs comprise the base dataset from which spectral image cubes will be created by continually evolving software using successively more accurate calibration and geometry data.

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Organization: National Aeronautics and Space Administration