AndreaBozzo/ceres-open-data-index huggingface dataset:
IMP-8 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates

IMP-8 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.

Tags: bow-shock, imp-8, magnetic-field, magneticfield-1-min, magnetometer, magnetopause, magnetotail, propagated-solar-wind-data, solar-wind
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER CHECKOUT OSINAC 3 CVP2 RDR V1.0

This CODMAC level 3 data set contains radiometric calibrated image data in W/m^2/sr/nm,  acquired by the OSIRIS Narrow Angle Camera on the Rosetta spacecraft  during the COMMISSIONING 2 mission phase, covering the period  from 2004-09-06T00:00:00.000 to 2004-10-16T23:59:59.000. The prime objective was commissioning / calibration. Several targets of opportunity were observed, but none of them is identifiable as prime target. After the October 2018 PSA/PDS external peer review, the COMMISSIONING  data set was reprocessed and split into multiple data sets. This  version V1.0 is one part and supersedes the previous delivery.

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Organization: National Aeronautics and Space Administration
IMP-8 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates

IMP-8 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, imp-8, magnetic-field, magneticfield-1-min, magnetometer, magnetopause, magnetotail, propagated-solar-wind-data, solar-wind
Organization: National Aeronautics and Space Administration
Coastal Ocean Observation and Analysis (COOA) Gulf of Maine measurements

Measurements from the Gulf of Maine between 2008 and 2009 made by the Coastal Observing Center at UNH (sometimes called COOA).

Tags: earth-science-ocean-chemistry-oceans, earth-science-ocean-optics-oceans, earth-science-ocean-temperature-oceans, earth-science-salinity-density-oceans
Organization: National Aeronautics and Space Administration
CASSINI S INMS LEVEL 1A EXTRACTED DATA V1.0

The Cassini Ion and Neutral Mass Spectrometer (INMS) level 1A data      set includes all mass samples for the entire Cassini mission. The      data set includes mass spectra data from the instrument checkout      periods, SOI and the entire Saturn tour. The data is organized as      a spread sheet with one row for each sample period. Each column in      the spread sheet contains the ancillary data and the output of the      counters.

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Organization: National Aeronautics and Space Administration
ISEE 1 Linearly Interpolated 60 s Resolution Fast Plasma Experiment data in GSM Coordinates

ISEE-1 Fast Plasma Experiment data linearly interpolated to have the measurements on the minute at 60 s resolution data in GSM coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind.

Tags: bow-shock, fast-plasma-experiment, isee-1, magnetopause, magnetotail, plasma-data, solar-wind, thermalplasma-1-min
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P SREM 2 PRELANDING MTP003 V1.0

This data set contains count rates (1/s) as measured by the Standard Radiation Environment Monitor (SREM) instrument on the Rosetta spacecraft, along with their standard deviations. The primary target is comet 67P/Churyumov-Gerasimenko. These are CODMAC Level 2 Experiment Data Record data, and provide a measure of the radiation in the spacecraft environment during the Medium Term Plan 3 period of the PRELANDING mission phase.

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Organization: National Aeronautics and Space Administration
ISEE 1 Linearly Interpolated 60 s Resolution Fast Plasma Experiment data in GSE Coordinates

ISEE-1 Fast Plasma Experiment data linearly interpolated to have the measurements on the minute at 60 s resolution data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind.

Tags: bow-shock, fast-plasma-experiment, isee-1, magnetopause, magnetotail, plasma-data, solar-wind, thermalplasma-1-min
Organization: National Aeronautics and Space Administration
Geotail Weimer Propagated using LEP 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates

Geotail Weimer propagated solar wind data using LEP 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.

Tags: bow-shock, geotail, magnetic-fields, magneticfield-1-min, magnetometer, magnetopause, magnetotail, mgf, propagated-solar-wind-data, solar-wind
Organization: National Aeronautics and Space Administration
GO EARTH EPD RESAMPLED SUMMARY EARTH1 15.0 MIN V1.0

This data set contains fifteen minute averages for            the energetic particle detector rate data obtained            from the LEMMS telescope during the time the detector            was operated during the Earth 1 encounter.  The data            are recorded in thirty minute averages for each of 32            LEMMS channels and 32 CMS channels.

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Organization: National Aeronautics and Space Administration
Geotail Weimer Propagated using CPI 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates

Geotail Weimer propagated solar wind data using CPI 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.

Tags: bow-shock, geotail, magnetic-fields, magneticfield-1-min, magnetometer, magnetopause, magnetotail, mgf, propagated-solar-wind-data, solar-wind
Organization: National Aeronautics and Space Administration
CERES ERBE-like Time-Interpolated TOA Fluxes Terra Crosstrack Edition4

CER_ES4_Terra-Xtrk_Edition4 is the Clouds and the Earth's Radiant Energy System (CERES) Earth Radiation Budget Experiment (ERBE)-like Time-Interpolated Top-of-the-Atmosphere (TOA) Fluxes Terra Cross-track Edition 4 data product, which was collected using the CERES-Flight Model (FM1) and FM2 instruments on the Terra platform. Data collection for this product is complete. The ERBE-like Monthly Geographical Averages (ES-4) product contains a month of space and time-averaged CERES data for a single satellite using measurements from the primary cross-track instrument. For each observed 2.5-degree spatial region, the daily average, the hourly average over the month, and the overall monthly average of shortwave and longwave fluxes at the TOA from the CERES ES-9 product are spatially nested up from 2.5-degree regions to 5- and 10-degree regions, to 2.5-, 5-, and 10-degree zonal averages, and to global monthly averages. For each nested area, the albedo and net flux are given. For each region, the daily average flux is estimated from an algorithm that uses the available hourly data, scene identification data, and diurnal models. This algorithm is "like" the algorithm used for ERBE. CERES is a key Earth Observing System (EOS) program component. The CERES instruments provide radiometric measurements of the Earth's atmosphere from three broadband channels. The CERES missions are a follow-on to the successful ERBE mission. The first CERES instrument, the protoflight model (PFM), was launched on November 27, 1997, as part of the Tropical Rainfall Measuring Mission (TRMM). Two CERES instruments (FM1 and FM2) were launched into polar orbit on board the Earth Observing System (EOS) flagship Terra on December 18, 1999. Two additional CERES instruments (FM3 and FM4) were launched on board Earth Observing System (EOS) Aqua on May 4, 2002. The CERES FM5 instrument was launched on board the Suomi National Polar-orbiting Partnership (NPP) satellite on October 28, 2011. The newest CERES instrument (FM6) was launched on board the Joint Polar-Orbiting Satellite System 1 (JPSS-1) satellite, now called NOAA-20, on November 18, 2017.

Tags: earth-science-atmospheric-radiation-atmosphere-albedo, earth-science-atmospheric-radiation-atmosphere-longwave-radiation, earth-science-atmospheric-radiation-atmosphere-net-radiation, earth-science-atmospheric-radiation-atmosphere-outgoing-longwave-radiation, earth-science-atmospheric-radiation-atmosphere-radiative-flux, earth-science-atmospheric-radiation-atmosphere-shortwave-radiation
Organization: National Aeronautics and Space Administration
MGS MARS/MOONS MAG/ER MAPPING MAG FULL WORD RESOLUTION V1.0

This data set contains vector magnetic    field data acquired by the Fluxgate section of the Magnetometer /    Electron Reflectometer instrument aboard the Mars Global Surveyor (MGS)    spacecraft. The data are provided at a variable time resolution depending    on the telemetry rate available to the investigation for the time period    beginning with the prime mission mapping (1999-03-08). The data in the    dataset cover the entire mapping time period.

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Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 3 3276 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 2012-05-03T13:48:38.000 to 2012-05-03T16:13:19.500.

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Organization: National Aeronautics and Space Administration
MARS EXPRESS SUN MRS 1/2/3 EXTENDED MISSION 7 4037 V1.0

This is a Mars Express Radio Science data set, collected during the extended mission phase 2019-01-01 to 2020-12-31. It is a Solar Conjunction measurement and covers the time 2019-08-19T07:20:00.000 to 2019-08-19T12:50:00.000.

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Organization: National Aeronautics and Space Administration
CERES MODIS Cloud Retrievals in ISCCP-D2like Format Nighttime Aqua FM3 Edition3A

CER_ISCCP-D2like-Nit_Aqua-FM3-MODIS_Edition3A is the Clouds and the Earth's Radiant Energy System (CERES) Moderate Resolution Imaging Spectroradiometer (MODIS) Cloud Retrievals in International Satellite Cloud Climatology Project (ISCCP) Day 2 like Format Nighttime Aqua Flight Model 3 (FM3) Edition 3A data product, which was collected using the CERES-FM3 and MODIS instruments on the Aqua platform. Data collection for this product is complete. The Monthly Gridded Cloud Averages (ISCCP-D2like-Day) data product contains monthly and monthly 3-hourly (GMT-based) gridded regional mean CERES MODIS-derived cloud properties as a function of 18 cloud types, similar to the ISCCP D2 product, where the cloud properties are stratified by pressure, optical depth, and phase. There are separate daytime and nighttime data sets for both Terra-MODIS and Aqua-MODIS. The retrievals, and therefore the quality, are different for each data set. The CERES MODIS-derived cloud properties are not the official NASA MODIS cloud retrievals but are based on the CERES cloud working group retrievals, also available in other CERES products. The CERES MODIS-derived cloud properties have coverage from pole to pole. For these MODIS-based ISCCP-D2like products, the cloud fractions for 42 cloud types, similar to the ISCCP D1 product, are also available. The Single Scanner Footprint TOA/Surface Fluxes and Clouds (SSF) data product is the input to this product. Each ISCCP-D2like file covers a single month. CCERES is a key Earth Observing System (EOS) program component. The CERES instruments provide radiometric measurements of the Earth's atmosphere from three broadband channels. The CERES missions follow the successful Earth Radiation Budget Experiment (ERBE) mission. The first CERES instrument, the protoflight model (PFM), was launched on November 27, 1997, as part of the Tropical Rainfall Measuring Mission (TRMM). Two CERES instruments (FM1 and FM2) were launched into polar orbit on board the Earth Observing System (EOS) flagship Terra on December 18, 1999. Two additional CERES instruments (FM3 and FM4) were launched on board Earth Observing System (EOS) Aqua on May 4, 2002. The CERES FM5 instrument was launched on board the Suomi National Polar-orbiting Partnership (NPP) satellite on October 28, 2011. The newest CERES instrument (FM6) was launched on board the Joint Polar-Orbiting Satellite System 1 (JPSS-1) satellite, now called NOAA-20, on November 18, 2017.

Tags: earth-science-clouds-atmosphere-cloud-microphysics-cloud-droplet-concentration-size, earth-science-clouds-atmosphere-cloud-microphysics-cloud-liquid-water-ice, earth-science-clouds-atmosphere-cloud-microphysics-cloud-optical-depth-thickness, earth-science-clouds-atmosphere-cloud-properties, earth-science-clouds-atmosphere-cloud-properties-cloud-fraction, earth-science-clouds-atmosphere-cloud-properties-cloud-midlayer-temperature, earth-science-clouds-atmosphere-cloud-radiative-transfer-cloud-emissivity, earth-science-infrared-wavelengths-spectral-engineering
Organization: National Aeronautics and Space Administration
Geotail Weimer Propagated using LEP 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates

Geotail Weimer propagated solar wind data using LEP 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, geotail, magnetic-fields, magneticfield-1-min, magnetometer, magnetopause, magnetotail, mgf, propagated-solar-wind-data, solar-wind
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER MARS RPCLAP2 MARS EDITED2 V1.0

This data set contains EDITEDdata from Rosetta RPC-LAP, acquired during the MARS SWING-BY missionphase where the primary target was the planet MARS. It containsuncalibrated raw data, i.e. the digital output of the instrument.

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Organization: National Aeronautics and Space Administration