AndreaBozzo/ceres-open-data-index huggingface dataset:
SAMPEX Polar-Cap-Averaged Fluxes, all instruments

This data set contains 17 differential fluxes of protons (mainly), helium ions, Z.GE.6 ions, and electrons, plus one integral flux of protons and electrons, as averaged over polar cap passes of the SAMPEX spacecraft. A polar cap pass covers the time poleward of geomagnetic latitude 70 deg. (Not all orbits have two polar cap passes.). For any given species, the fluxes typically come from more than one of the sensors (LICA, HILT, MAST, PET). Hence the inclusion of all instruments' data in each single record. Differential fluxes are those for (mainly) protons (Z.GE.1 channels at 5-12 and 19-27 MeV/n), helium ions (0.50-6.6, 4-9, 8-15, 9-38 MeV/n), Z.GE.6 ions (0.49-8.3, 8-42, 19.3-22.8, 22.8-31.0, 31.0-51.7, 41-220, 51.7-76.2, 76.2-113, 113-156 MeV/n), and electrons (1.5-6.0 MeV from PET only). One LICA channel measured integral fluxes of ions .GT. 0.8 MeV/n plus electrons .GT. 0.6 MeV). Data available for each polar cap pass are time tags of the begin and end points of the averaging interval, the fluxes, statistical uncertainties in the fluxes, instrument-specific flags, and a flag indicating a north or south polar cap pass. Data are organized in two different ways. Monthly ~500-KB ASCII files with records organized by instrument are available from the SAMPEX Data Center at Caltech and from nssdcftp at GSFC/SPDF, while monthly ~260 KB CDF-formatted files with records organized by species are available from the ftp area underlying CDAWeb. The parameter level information given below in this descriptor corresponds to the CDAWeb organization of data. Format information for the ASCII version is given in the Information URL of this descriptor.

Tags: energeticparticles, ioncomposition
Organization: National Aeronautics and Space Administration
SDO/AIA 211 Angstrom FITS Data

The SDO/AIA 211 Å Level 1 FITS Data. The 211 Å channel observes the Fe xiv line from active region corona (2.0 MK).  \n\nThe Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.\n\nAIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.

Tags: imageintensity
Organization: National Aeronautics and Space Administration
DAWN SPICE KERNELS V1.0

This data set includes the complete set of DAWN SPICE data files      (``kernel files''), which can be accessed using SPICE software.      The SPICE data contain geometric and other ancillary information      needed to recover the full value of science instrument data. In      particular SPICE kernels provide spacecraft and planetary      ephemerides, instrument mounting alignments, spacecraft      orientation, and data needed for relevant time conversions.

Tags: __
Organization: National Aeronautics and Space Administration
CAMEX-4 MIPS SODAR V1

The University of Alabama in Huntsville (UAH) Mobile Integrated Profiling System (MIPS) is a mobile atmospheric profiling system. It includes a 915 MHz Doppler profiler, lidar ceilometer, 12 channel microwave profiling radiometer, Doppler Sodar, Radio Acoustic Sounding System (RASS), Field Mills, and surface observing station. This dataset consists of cdf and mom files tarred together for a day. The 'cdf' file collects 15 minute average 3-D wind profiles from the Doppler Sodar starting at the beginning of each day. The 'mom' file contains data from each beam about radial velocity and backscattter intensity. Each horizontal beam is approximately 7 seconds apart; vertical beams are approximately 21 seconds apart.

Tags: earth-science-atmospheric-pressure-atmosphere-planetary-boundary-layer-height, earth-science-atmospheric-temperature-atmosphere-surface-temperature-air-temperature, earth-science-atmospheric-temperature-atmosphere-surface-temperature-boundary-layer-temperature, earth-science-atmospheric-winds-atmosphere-surface-winds, earth-science-atmospheric-winds-atmosphere-wind-profiles
Organization: National Aeronautics and Space Administration
SDO/AIA 1600 Angstrom FITS Data

The SDO/AIA 1600 Å Level 1 FITS Data. The 1600 Å channel observes the C iv line and continuum from the transition region and the upper photosphere, respectively. \n\nThe Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.\n\nAIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.

Tags: imageintensity
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 3 1101 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 3 phase 2015-07-01 to 2015-10-21. It is a Global Gravity measurement at the comet 67P and covers the time 2015-10-14T20:35:40.000 to 2015-10-14T23:45:08.000.

Tags: __
Organization: National Aeronautics and Space Administration
VO1/VO2 MARS VISUAL IMAGING SS EXPRMNT DATA REC BROWSE V2.0

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

Tags: __
Organization: National Aeronautics and Space Administration
CAMEX-4 NOAA WP-3D VIDEO V1

The CAMEX-4 NOAA WP-3D Video dataset was collected during the fourth field campaign in the CAMEX series (CAMEX-4), which ran from 16 August to 25 September, 2001 and was based out of Jacksonville Naval Air Station, Florida. An important addition to CAMEX-4 was the participation of the NOAA weather reconnaissance WP-3D that collected radar, video and microphysical data.The NOAA WP-3D Videos were created giving a forward, left, right and downward views relative to the aircraft. Each view is a separate tape. All are recoreded in SVHS format in compressed time mode. That means that the video shows time passing at a rate approximately 12.5 times that of normal speed (e.g. 1 minute real time takes 5 seconds on the video). For further information and to obtain this data, please contact GHRC at support-ghrc@earthdata.nasa.gov

Tags: earth-science-visible-wavelengths-spectral-engineering-visible-imagery
Organization: National Aeronautics and Space Administration
SDO/AIA 4500 Angstrom FITS Data

The SDO/AIA 4500 Å Level 1 FITS Data. The 4500 Å channel observes the continuum from the photosphere.  \n\nThe Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.\n\nAIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.

Tags: imageintensity
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER COMET ESCORT 2 OSIWAC 3 RDR MTP016 V2.0

This data set contains images acquired by the OSIRIS Wide Angle Camera during the COMET ESCORT 2 phase of the Rosetta mission at the comet 67P, covering the period from 2015-05-05T23:25:00.000 to 2015-06-02T23:24:59.000. This version V2.0 supersedes previous deliveries of the same dataset.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/AIA 1700 Angstrom FITS Data

The SDO/AIA 1700 Å Level 1 FITS Data. The 1700 Å channel observes the continuum from the 4500 K photosphere (temperature minimum).  \n\nThe Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) focuses on the evolution of the magnetic environment in the Sun’s atmosphere, and its interaction with embedded and surrounding plasma. The AIA investigation covers a broad range of science objectives that focus on five core research themes that both advance solar and heliospheric physics in general and provide advanced warning of coronal and inner-heliospheric disturbances of interest to the Living With a Star (LWS) program, i.e., global change, space weather, human exploration of space, and technological infrastructure in space and on Earth.\n\nAIA provides the following essential capabilities: i) A view of the entire Sun in 4k x 4k resolution (pixel size of 0.6 arcseconds), with full thermal coverage of the corona; ii) A high signal-to-noise ratio for two- to three-second exposures that reaches 100 in quiescent conditions for the low-temperature coronal-imaging channels and during flaring in the higher-temperature channels, with a dynamic range of up to 10,000; iii) Essentially uninterrupted viewing for months at a temporal cadence of 12 seconds in seven extreme UV (EUV) band passes (94, 131, 171, 193, 211, 304 and 335 Å), and 24 seconds for two UV channels (1600 and 1700 Å) band passes; iv) In special observing modes, AIA can capture images of the Sun at higher cadence while keeping within the instrument allocated telemetry by using a subset of bandpass channels, and/or using a crop table.

Tags: imageintensity
Organization: National Aeronautics and Space Administration
CAMEX-4 DC-8 INFORMATION COLLECTION AND TRANSMISSION SYSTEM V1

The CAMEX-4 DC-8 Information Collection and Transmission System dataset was collected by the Information Collection and Transmission System (ICATS), which is designed to: 1) Interface and process avionics and environmental paramaters from the Navigational Management System, GPS, Central Air Data Computer, Embedded GPS/INS, and analog voltage sources from aircraft and experimenters, 2) Furnish engineering unit values of selected parameters and computed functions for real-time video display, and archive ASCII data at experimenter stations, 3) Archive engineering unit values of 'Appendix A' (to the ICATS document included with dataset documentation) on data storage for post flight retrieval.

Tags: earth-science-atmospheric-temperature-atmosphere-surface-temperature-air-temperature, earth-science-atmospheric-temperature-atmosphere-upper-air-temperature, earth-science-atmospheric-temperature-atmosphere-upper-air-temperature-dew-point-temperature, earth-science-atmospheric-winds-atmosphere-upper-level-winds-wind-direction, earth-science-atmospheric-winds-atmosphere-upper-level-winds-wind-speed, earth-science-platform-characteristics-spectral-engineering-airspeed-ground-speed
Organization: National Aeronautics and Space Administration
MOTHE-DINIZ ASTEROID DYNAMICAL FAMILIES V1.1

This dataset contains an updated compilation of asteroid families and clusters, resulting from the application of the Hierarchical Clustering Method (HCM) on a set of around 120,000 asteroids with available proper elements. Whenever available, the classification in the Bus taxonomy is provided for family members, based on spectra from the SMASS, SMASS2 and S3OS2 spectroscopic surveys.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/EVE Level 3 Version 8 Data

EVE level 3 data files were created at the Laboratory for Atmospheric and Space Physics in Boulder, Colorado for the NASA Solar Dynamics Observatory (SDO) Extreme Ultraviolet Variability Experiment (EVE). The Science Processing and Operations Center (SPOC) is responsible for creating and maintaining access to all EVE products. For a high-level introduction to the EVE instrumentation please visit:\nhttps://lasp.colorado.edu/home/eve/science/instrument/\n\nLevel 3 products are defined to contain daily averages beginning on 2010, day 120, April 30. This version change includes updated long-term degradation corrections for MEGS-B and ESP. A small dark adjustment was applied to MEG-B and large degradation changes were applied based on SDO EVE sounding rocket measurements. The MEGS-P (Lyman-alpha) diode processing has been updated to replace the Kalman filter with a Fourier transform filter, and the calibration has been updated to match SORCE SOLSTICE version 17.

Tags: irradiance, spectrum
Organization: National Aeronautics and Space Administration
SDO/EVE Level 2 Version 8 Data

EVE level 2 data files were created at the Laboratory for Atmospheric and Space Physics in Boulder, Colorado for the NASA Solar Dynamics Observatory (SDO) Extreme Ultraviolet Variability Experiment (EVE). The Science Processing and Operations Center (SPOC) is responsible for creating and maintaining access to all EVE products. For a high-level introduction to the EVE instrumentation please visit:\nhttps://lasp.colorado.edu/eve/science/instrument/\n\nLevel 2 products are defined to contain 10-second intervals and span the time range from 2010 day 120 through 2018 day 108. The integration rate was changed to 60-seconds so the level 2B products were created to provide future spectra. This release of EVE Level 2 data products replaces all previous versions. We have made significant effort at verification and validation, but if you have any questions or encounter any problems with the data, please let us know about them.\n\nTwo types of EVE level 2 products are routinely created: Spectra (EVS) and Lines (EVL). Level 2 spectra are the merged spectral measurements from the two spectrographs, MEGS-A and MEGS-B. The A detector is designed to measure from 6 –17 nm, and 17–37 nm using two filters, while the B detector is designed to measure 37–106. After the MEGS-A anomaly, MEGS-B was extended down to 33.33 nm. \n\nLevel 2 processing stitches these pieces to form one spectrum. This version includes all measured wavelengths. The file spans 3.01-106.99 nm, but this extends beyond where there is no signal on the detectors, so there will be fill values at the extreme ends of the range. All level 2 irradiances are adjusted to 1 AU. Level 2 lines files contain selected lines derived from the level 2 spectra, ESP diode values and bands that correspond to other SDO instruments and some derived proxies.

Tags: irradiance, spectrum
Organization: National Aeronautics and Space Administration
VG2 JUP EPHEMERIS HELIOGRAPHIC COORDSBROWSE V1.0

This data set consists of Voyager 2    Jupiter encounter ephemeris data in Heliographic coordinates covering the    period 1979-06-20 to 1979-08-18. Two versions, both covering the same time    period, but containing slightly different data, are provided. One version    was generated by the Voyager MAG team from Voyager 2 SEDR, the other by    the PDS/PPI node using the VG2_JUP.BSP and PCK00003.TPC SPICE kernels.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/HMI Continuum, 45-Second Data

The HMI continuum data refers to map of the continuum intensity of the solar spectrum in the region of the Fe I absorption line at 6173 Å on the surface of the sun.\n\nHMI samples the Fe I absorption line at 6173.3 Å at six points. Assuming that the "pure" solar Fe I line profile is a Gaussian, and the HMI filter filter transmission profiles are delta functions, the first and second Fourier coefficients of the of the Fe I line can be calculated and an estimate of the Doppler Velocity can be made. An estimate (proxy) for the continuum intensity Ic is obtained by "reconstructing" the solar line from the estimates of the Doppler shift λo, the linewidth σ, and the linedepth Id. More details can be found at http://jsoc.stanford.edu/relevant_papers/observables.pdf.\n

Tags: imageintensity
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 1 0618 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 2015-03-02T22:17:55.000 to 2015-03-03T09:44:27.500.

Tags: __
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P MIDAS 3 EXT2 SAMPLES V3.0

The Micro-Imaging Dust Analysis System (MIDAS) is an instrument on theROSETTA Orbiter that will provide 3D images and statistical parametersof pristine cometary particles, collected in the vicinity of comet67P/Churyumov-Gerasimenko. This data set includes all data from theROSETTA EXTENSION 2 mission phase.This release supersedes version 2.0.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/HMI line-of-sight Dopplergram, 45-Second Data

Dopplergrams are maps of solar surface velocity. The HMI (Camera 2) instrument takes 72 filtergrams to construct a single dopplergram. Six filtergrams are taken in six positions across the nominal 6173.3 Å spectral line; each filtergram is taken in two polarization states (right circularly polarized (RCP), or Stokes I-V, and left circularly polarized (LCP), or I+V). Assuming that the absorption line is a Gaussian and that the HMI filter transmission profiles are delta functions, the Fourier coefficients can be calculated and are then used to estimate the line-of-sight magnetic field strength B.

Tags: dopplergram
Organization: National Aeronautics and Space Administration
ROSETTA-ORBITER 67P RSI 1/2/3 COMET ESCORT 4 1268 V1.0

This is a Rosetta Radio Science data set, collected during the COMET ESCORT 4 phase 2015-10-22 to 2015-12-31. It is a Global Gravity measurement at the comet 67P and covers the time 2015-12-19T09:41:05.000 to 2015-12-19T15:40:58.000.

Tags: __
Organization: National Aeronautics and Space Administration
SDO/HMI line-of-sight Magnetogram, 720-Second Data

Magnetograms are maps of the observed solar magnetic field in the photosphere. The line-of-sight component of the field can be accurately measured as it evolves in time over the full visible disk of the Sun. The HMI instrument exploits the Zeeman effect, which allows the strength of the line-of-sight component of the magnetic field to be determined by measurements of the spectral line in circularly polarized light.\n\nHMI makes two independent measurements of the line-of-sight component of the photospheric magnetic field. One is collected every 45 seconds with the HMI Doppler camera. The other is computed every 720 seconds using filtergrams recorded by the Vector Field camera. The spatial resolution is 1 arc second (half arc-second pixels) and the full disk images are collected on a 4096**2 detector. The noise level is nominally 6.3 Gauss. HMI really measures flux density in Mx/cm2 in each pixel.

Tags: magnetogram
Organization: National Aeronautics and Space Administration
MARS EXPRESS MARS MRS 1/2/3 EXTENDED MISSION 7 3994 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 Occultation measurement and covers the time 2019-04-15T06:13:27.000 to 2019-04-15T06:35:35.649.

Tags: __
Organization: National Aeronautics and Space Administration
SHARP Near-Real-Time Data

SHARP Near Real Time data in CCD coordinates.\n\nSHARP stands for Space-weather HMI Active Region Patch. A SHARP is a DRMS series that contains (1) various space-weather quantities calculated from the photospheric vector magnetogram data and stored as FITS header keywords, and (2) 31 data segments (described in detail below), including each component of the vector magnetic field, the line-of-sight magnetic field, continuum intensity, doppler velocity, error maps and bitmaps. The data segments are not full-disk; rather, they are partial-disk, automatically-identified active region patches. SHARPs are calculated every 12 minutes. Often, there is more than one active region on the solar disk at any given time. Thus, SHARPs are indexed by two prime keys: time, T_REC, and HMI Active Region Patch Number, HARPNUM.\n\nNote that HARPNUMs in the nrt and defnitive data series will be different.

Tags: magnetogram
Organization: National Aeronautics and Space Administration