cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.48322/vnzr-5v17
title: Ulysses Cosmic Ray and Solar Particle Investigation (COSPIN) Low Energy Telescope (LET) Spin-Integrated Ion Fluxes and Electron Counting Rates, 10 min Average Data
title: COSPIN-LET-RAT-10M

description: This Data Set contains 10 min Averages of: (a) Spin-Integrated Fluxes of Protons (0.9-1.2, 1.2-3.0, 1.8-3.8, 3.8-8.0 and 8.0-19.0 MeV), Alpha Particles (1.0-5.0, 1.9-3.7, 3.7-8.4 and 8.4-19.0 MeV/n), Lithium, Beryllium, and Boron Nuclei (1.9-4.9 and 4.9-26 MeV/n), Carbon, Nitrogen, and Oxygen Nuclei (2.6-7.1 and 7.1-39 MeV/n), Z≥10 Nuclei (3.0-9.0 MeV/n), 10≤Z≤20 Nuclei (9.0-50 MeV/n) and Z≥20 Nuclei (12-75 MeV/n). (b) Eight-Sectored Proton Fluxes (1.8-3.8 and 3.8-8.0 MeV). (c) Count Rates of Electrons (0.3-1.0 MeV) and D1, D2, D3, D4 and D5 single Detector Sensors. The Parameter Keys in the Parameter Level Segments below are specifically relevant to the UFA accessible Versions of the Data.
DOI: 10.48322/27sk-1v19
title: Ulysses Dust Detection System Data

description: This data set contains information collected by the Ulysses Cosmic Dust instrument on the dust environment in interplanetary space within the inner solar system, between Jupiter and the Sun, and at high polar latitudes of the Sun. Both interplanetary and interstellar dust particles have been detected. This information is collected with a dust impact experiment, from which may be inferred direction of motion, mass, velocity and charge (see ULYDINST.CAT). The data presented in this dataset include instrumental readouts, inferred metadata, calibration information and a calendar of events.
DOI: 10.48322/gfwr-5j21
title: Ulysses EPAC full-resolution rates and fluxes at SPDF

description: Full resolution proton and electron fluxes, plus many count rates in annual files
DOI: 10.48322/4y36-ya33
title: Ulysses magnetic field 1-min data

description: This data set contains high resolution samples at about one-minute intervals of the interplanetary magnetic field measured by the Ulysses Magnetic Field experiment. Field vector components are given in units ofnanoteslas and in RTN coordinates, where R is the radial component or the sun-s/c axis, T is the transverse (along-track) component or the cross product of the solar rotation axis and R, and N is the normal (cross-track) component or the cross product of R and T. The field magnitudes in nT are averages of scalar magnitudes at higher time resolution. Times are computed at the mid-point of each 
minute interval and expressed in Spacecraft Event Time - UT (SCET-UT). Data gaps have not been flagged in any way - if there were no available data in a particular hour then there is no data record for that hour. No data from the Feb. 1992 encounter with Jupiter are included. Each file includes one day of data. Further details on the magnetic field measurements can be found in the following reference: Balogh, A., et al., Astron. Astrophys. Suppl. Ser., 92(2), 221, 1992.
DOI: 10.48322/g3r8-tw82
title: Ulysses EPAC hourly rates and fluxes, CDAWeb

description: Hourly proton and electron fluxes with spectral and directional information
DOI: 10.48322/kdyd-tx13
title: Ulysses magnetic field 1-hr data

description: This data set contains high resolution samples at about one-hour intervals 1hrof the interplanetary magnetic field measured by the Ulysses Magnetic Field experiment. Field vector components are given in units ofnanoteslas and in RTN coordinates, where R is the radial component or the sun-s/c axis, T is the transverse (along-track) component or the cross product of the solar rotation axis and R, and N is the normal (cross-track) component or the cross product of R and T. The field magnitudes in nT are averages of scalar magnitudes at higher time resolution. Times are computed at the mid-point of each 
minute interval and expressed in Spacecraft Event Time - UT (SCET-UT). Data gaps have not been flagged in any way - if there were no available data in a particular hour then there is no data record for that hour. No data from the Feb. 1992 encounter with Jupiter are included. Each file includes one day of data. Further details on the magnetic field measurements can be found in the following reference: Balogh, A., et al., Astron. Astrophys. Suppl. Ser., 92(2), 221, 1992.
DOI: 10.48322/mzqv-2n56
title: Ulysses High Resolution Magnetic Field Data

description: This data set contains high resolution samples at about one-second intervals of the interplanetary magnetic field measured by the Ulysses Magnetic Field experiment. Field vector components are given in units of nanoteslas and in RTN coordinates, where R is the sun-s/c axis, T is the cross product of the solar rotation axis and R, and T is the cross product of R and T. The field magnitudes in nT are averages of scalar magnitudes at higher time resolution. Times are computed at the mid-point of each averaging interval and expressed in Spacecraft Event Time - UT (SCET-UT). Data gaps have not been flagged in any way - if there were no available data in a particular hour then there is no data record for that hour. No data from the Feb. 1992 encounter with Jupiter are included. Each file includes one day of data. Parameter key information given below is specific to the data version at nssdcftp and at the ESA Research and Scientific Support Department site identified below. Further details on the magnetic field measurements can be found in the following reference: Balogh, A., et al., Astron. Astrophys. Suppl. Ser., 92(2), 221, 1992.
DOI: 10.48322/90zn-mv12
title: Ulysses GAS UV Full-Sky Data

description: This Ulysses GAS experiment data set consists of pixel map data and image files for sky maps generated from GAS measurements in a mode primarily sensitive to ultraviolet photons. The accumulated counts and Ecliptic (spacecraft-centered) angle coordinates for each sky map pixel are given in the ascii files *.TXT. The positions of the Sun and the planets vary with time and with the position of the spacecraft along its trajectory, while the positions of stars remain fixed. The full images are provided in GIF (*.GIF files) and postscript (*.PS files) format, the GIF files being easily viewed on-line (see below) with an Internet web browser. The actual positions of Sun, Earth, and Jupiter are indicated by yellow, green, and white dots, respectively. The area around the Sun is excluded from observation to avoid damaging intensities from direct sunlight.

The files USER_GUIDE.TXT, FORMAT.TXT, and REFERENCE.TXT, respectively, give an overall description of the various datatypes, the record format for the DATA datatype, and a list of GAS-related publications. The users guide defines the nomenclature of the file names.
DOI: 10.48322/m0b0-fg03
title: Ulysses GAS Interstellar Helium Maps

description: This Ulysses GAS experiment data set consists of pixel map data and image files for sky maps generated from GAS measurements in the mode primarily sensitive to neutral helium atoms from inflow of interstellar gas into the heliosphere. The accumulated counts and Ecliptic (spacecraft-centered) angle coordinates for each sky map pixel are given in the ascii files *.TXT. The positions of the Sun and the planets vary with time and with the position of the spacecraft along its trajectory, while the positions of stars remain fixed. The full images are provided in GIF (*.GIF files) and postscript (*.PS files) format, the GIF files being easily viewed on-line (see below) with an Internet web browser. The actual positions of Sun, Earth, and Jupiter are indicated by yellow, green and white dots, respectively. The area around the Sun is excluded from observation to avoid damaging intensities from direct sunlight. The files USER_GUIDE.TXT, FORMAT.TXT, and REFERENCE.TXT, respectively, give an overall description of the various datatypes, the record format for the DATA datatype, and a list of GAS-related publications. The users guide defines the nomenclature of the file names. Further details about the data and the experiment may be found in Witte et al., Astron. Astrophys. Suppl. Ser., 92, No. 2, 333-348, 1992 (NSSDC TRF # B40459-000A). Data analysis methods for interstellar helium are described in Banaszkiewicz et al., Astron. Astrophys. Suppl. Ser., 120, 587-602, 1996 (B45706-000A).
DOI: 10.48322/xpsw-g004
title: Ulysses HISCALE LEM120 ion and electron counts

description: This data set contains 1-hour spin averaged count rates of the ion and electron from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Foil Spectrometer at 120 degrees to the spacecraft spin axis. Count rate units are /s.  For references, see Astron. Astrophys. Suppl. Ser., 92(2), 349-363, 1992.
DOI: 10.48322/66bw-pp17
title: Ulysses HISCALE LEFS150 ion and electron counts

description: This data set contains 1-hour spin averaged count rates of the ion and electron from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Foil Spectrometer at 150 degrees to the spacecraft spin axis. Count rate units are /s.  For references, see Astron. Astrophys. Suppl. Ser., 92(2), 349-363, 1992.
DOI: 10.48322/yq68-e458
title: Ulysses HISCALE LEMS30 ion and electron counts

description: This data set contains 1-hour spin averaged count rates of the ion and electron from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Foil Spectrometer at 30 degrees to the spacecraft spin axis. Count rate units are /s.  For references, see Astron. Astrophys. Suppl. Ser., 92(2), 349-363, 1992.
DOI: 10.48322/6ed8-h760
title: Ulysses HISCALE LEFS60 ion and electron counts

description: This data set contains 1-hour spin averaged count rates of the ion and electron from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Foil Spectrometer at 60 degrees to the spacecraft spin axis. Count rate units are /s.  For references, see Astron. Astrophys. Suppl. Ser., 92(2), 349-363, 1992.
DOI: 10.48322/txc7-w438
title: Ulysses HISCALE LEMSDE deflected electron counts

description: This data set contains 1-hour spin averaged count rates of the deflected electron from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Low Energy Foil Spectrometer at 30 degrees to the spacecraft spin axis. Count rate units are /s.  For references, see Astron. Astrophys. Suppl. Ser., 92(2), 349-363, 1992.
DOI: 10.48322/3hn7-hc82
title: Ulysses HISCALE 1-hour ion counts

description: This data set contains 1-hour spin averaged count rates of the ion data from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Composition Aperture Telescope at 60 degrees to the spacecraft spin axis. Count rate units are /s.  For references, see Astron. Astrophys. Suppl. Ser., 92(2), 349-363, 1992.
DOI: 10.48322/g487-b498
title: Ulysses HISCALE 1-hour proton counts

description: This data set contains 1-hour spin averaged count rates of proton data from the Ulysses Heliosphere Instrument for Spectra, Composition and Anisotropy at Low Energies (HI-SCALE) Composition Aperture Telescope at 60 degrees to the spacecraft spin axis. Count rate units are /s.  For references, see Astron. Astrophys. Suppl. Ser., 92(2), 349-363, 1992.
DOI: 10.48322/14fy-2640
title: Ulysses GRB Integral 0.5-Second Omnidirectional Counting Rates

description: This data set contains data and software for integral 0.5-second omnidirectional counting rates from the Ulysses Gamma Ray Burst
(GRB) experiment. It consists of count rates from the sum of two hemispherical detectors convering 4 pi steradians and operating continuously. The detectors
are 3 mm thick CsI scintillators coupled to photomultiplier tubes. The nominal energy range is 25-150 keV, but Table 1 (see below) should be consulted to find
the accurate thresholds for any day of the mission. A more complete description of the instrument may be found in Hurley et al. (1992) and Cotin et al. (1983).
Althoughthe prime objectives of this investigation are the study of solar and cosmic x- and gamma-ray bursts, it should be noted that the experiment is also
sensitive to solar protons and electrons. The former deposit energy directly in the scintillator if they are energetic enough, while the latter may produce x-
radiation locally by bremsstrahlung. Thus although the counting rates are generally stable at about 500 c/s over the long term, there are periods of
weeks to a month or so when the rates increase considerably due to particles. Examples may be found in March 1991 (solar protons) and February 1992
(particles in the Jovian magnetosphere).
         
The time resolution of the data takes on one of four values depending on the telemetry rate and instrument operating mode: 0.25, 0.5, 1, or 2 seconds. Data
rate changes produce short spikes in the count rates due to a processing artefact. These can in principle be corrected if the data are scanned and the
rate changes are identified; the count rate spikes can then be adjusted to their correct values. There are also short (one sample long) count rate
dropouts, due to an artefact of the onboard software. These may be seen in the sample plots; they cannot be corrected for.
         
Two figures give examples of solar and cosmic events in the data. The upper panel gives the count rates for day 142, 1993, around 8.24 hours UT. The solar event is evident as a 300 second long increase. Note the count rate dropouts. The bottom panel includes a 20 second long cosmic gamma-ray burst from day 237, 1993 around 8.79 hours UT.
DOI: 10.48322/ak7p-0510
title: Ulysses hourly merged magnetic field and plasma data

description: This is an hourly resolution, merged magnetic field and plasma data set created at NSSDC for COHOWeb. Magnetic field vectors and plasma flow direction angles are given in RTN coordinates. Spacecraft position data are given in Heliographic inertial (HGI) coordinates.
DOI: 10.48322/qx8j-rj13
title: Ulysses Solar Wind Ion Composition Spectrometer (SWICS) Average Solar Wind Velocity, Isotope Ratios, and Iron Charge States, (M1), 3.5 h Data

description: This Data Set contains 3.5 hour Averages of the Solar Wind Ion Density Ratio (to O6+), Velocity And Temperature from the Ulysses Solar Wind Ion Composition Spectrometer. Data Set Contact: R. von Steiger, International Space Science Institute, Bern, Switzerland. Principal Investigators: J. Geiss, International Space Science Institute, Bern, Switzerland, and G. Gloeckler, University of Maryland, College Park, Maryland, USA. Reference: Astron. Astrophys. Suppl. Ser., 92(2), 267-289 (1992). Relevant Web Sites: http://space.umd.edu/UMD_sensors/uls_swics.html.
DOI: 10.48322/rz8e-rm43
title: Ulysses GRB data via CDAWeb

description: This data set from the Ulysses Gammay-Ray Bursts experiment contains 5-minute resolution filtered averages of cosmic gamma ray and solar X-Ray count rates. Count rate units are c/s. See Astron. Astrophys. Suppl. Ser., 92(2), 401-410, 1992 for more information.
DOI: 10.48322/39wd-b341
title: Ulysses olar Wind Ion Composition Spectrometer (SWICS) Full Resolution Matrix Rate Data

description: The Ulysses/SWICS instrument is a mass spectrometer combining an electrostatic analyzer with post acceleration, followed by a time-of-flight and energy measurement. The instrument covers an energy per charge range from 0.16 to 59.6 keV/e with a time resolution of about 13 minutes. SWICS is designed to determine uniquely the elemental and ionic-charge composition, the temperatures and mean speeds of all major solar wind ions, from H through Fe. For more information see G. Gloeckler, J. Geiss et al., Astron. Astrophys. Suppl. Ser. 92, 267-289, 1992. These data consist of all 18 Matrix Rates (MR) as a function of energy per charge (E/q) and of time. Each MR represents a specific element in one or several ionization states, but it may also contain significant contributions from neighbouring elements due to spillover. The MRs are given in units of count rates only. SAPRO (SWICS Archive Processor) software can be used both to convert the MR count rates to physical units (differential flux, phase space density), to correct for spillover between different MRs, and to obtain kinetic parameters (density, speed, thermal speed) of selected ions (to be used with caution).
DOI: 10.48322/6gsv-6k69
title: Ulysses SWICS 3-hour averages data via CDAWeb

description: This data set contains 3-hour averages of ion data from the Ulysses Solar Wind Ion Composition Spectrometer (SWICS) instrument. Density, velocity, and temperature data are available for 10 speciess (H, He, C, N, O, Ne, Mg, Si, S, and Fe) and charge states at 3-hr resolution.
DOI: 10.48322/8c4a-c187
title: Ulysses SWICS Solar Wind Moments of Main Heavy Ions 3.5 Hour Data

description: This ASCII data set consists of a table of 3.5-hour averages of velocities (km/s), temperatures (deg.-K), and density ratios (relative to oxygen 6+) of solar wind ion composition measurements by the Ulysses SWICS experiment for alphas, carbon 6+, oxygen 6+ (density ratio = unity), neon 8+, magnesium 10+, silicon 9+, sulfur 10+, and iron 11+. Data accumulation times for the averages ensure that percentage errors are less than twenty percent for the density ratios. Each ASCII data file contains one month of data. The experiment and data processing are further described in G. Gloeckler, et al., The Solar Wind Ion Composition Spectrometer, Astron. Astrophys., 92(2), 267-289, 1992.
DOI: 10.48322/c8ps-gj36
title: Ulysses SWICS Selected Charge States and Ratios of Solar Wind Heavy Ions 3-Hour Data

description: This ASCII data set consists of three hour averages of selected charge states and abundance ratios for solar wind heavy ions. The average charge state of Fe is given for states from Fe6+ to Fe16+; normal values vary from 9 to 12 in slow and fast solar wind with higher values in coronal mass ejection (CME) events. For carbon and oxygen the C6+/C5+ and O7+/O6+ ratios are given. The carbon on ratio is about ten times that for oxygen. Low ratios of these are indicative of fast solar wind streams. The Fe/O ratio is also provided as a proxy for the strength of the first ionization potential (FIP) fractionation when divided by the standard solar abundance value for Fe/O of about 0.05. Other data parameters include the alpha particle speed and the number of 13-min instrument cycles (normally 12 to 14) used for each 3-hour value. Each ASCII data file contains up to one year of data. The experiment and data processing are further described in G. Gloeckler, et al., The Solar Wind Ion Composition Spectrometer, Astron. Astrophys., 92(2), 267-289, 1992.
DOI: 10.15468/dl.seyfew
title: Occurrence Download

description: A dataset containing 373 species occurrences available in GBIF matching the query:
{
 "and" : [
 "TaxonKey is Kageneckia lanceolata",
 "HasCoordinate is true",
 "OccurrenceStatus is Present",
 {
 "not" : {
 "BasisOfRecord" : [
 "is Fossil"
 ]
 }
 }
 ]
}

 The dataset includes 373 records from 17 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0020922-260208012135463/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.48322/sgf3-hb74
title: Ulysses Solar Wind Observations Over the Poles of the Sun (SWOOPS) Alpha Particle Distribution Functions, Level H2, 4 min Data

description: This File contains the Distribution Function of Alpha Particles. DATA REDUCTION: The SWOOPS (Solar Wind Observations Over the Poles of the Sun) Ion Instrument is a Spherical-Section Curved-Plate Electrostatic Analyzer. Particle Arrival Directions are measured in Spacecraft Coordinates of Azimuth (scanned by Spacecraft Rotation) and Elevation (determined by the Detector Number) Angles. The Spacecraft Spin Axis was oriented toward the Earth. The Energy/Charge (E/q) Resolution was about 2.5% while the Azimuth (Phi) and Elevation (Theta) Resolutions were both ~5.6°. A Description of the SWOOPS is given in a Paper by S.J. Bame, D.J. McComas, B.L. Barraclough, J.L. Phillips, K.J. Sofaly, J.C. Chavez, B.E. Goldstein, and R.K. Sakurai, Astronomy and Astrophysics Supplement Series, Ulysses Instruments Special Issue, Vol. 92, No. 2, p.237-265, 1992. The Number of Counts in each E/q-Phi-Theta Bin were examined to determine the Peak of the Proton and Alpha Particle Distribution, respectively, and the Vector Magnetic Field (in Spacecraft Coordinates) was obtained for the Time at which the Peak was measured. A "coarse" Two-Dimensional Matrix was then formed by rotating the Data into a Coordinate System with Axes parallel and perpendicular to the Field Direction. Note that Gyrotropy is assumed in making that Transformation. The Resolution of the Matrix is "coarse" because the Vector Velocity assigned to each Bin was taken to be at the Center of the Bin. In reality, the Counts in each Bin were probably not smoothly distributed in Velocity Space over the Bin, but were weighted toward the Part of the Bin nearest the Center of the Peak of the Velocity Distribution. The "coarse" Distribution would thus yield Values for the Density and Temperature that were higher than the true Values. A Correction for that effect was accomplished by fitting Contours to the coarse Distribution, breaking each Bin or Pixel into Subpixels, and then using the Contours and the calibrated Angular Responses to distribute the Counts among the Subpixels. New Contours were then computed and the Process was continued until it converged. More Details about this Deconvolution of the Angular Data are given in the Appendix of a Paper by Neugebauer, M., et al., "Ion distributions in large magnetic holes in the fast solar wind" J. Geophys. Res., 106, 5635, 2001. This Procedure generated the Matrix of Velocity Distribution Functions of Protons and Alpha Particles parallel and perpendicular to the simultaneously measured Magnetic Field.
DOI: 10.48322/zb4k-7w57
title: Ulysses Solar Wind Observations Over the Poles of the Sun (SWOOPS) Alpha Particle Distribution Function Fitting Parameters, Key Parameter (K0), 4 min Data

description: This File contains the Parameters obtained by fitting Data to a Bi-Maxwellian Core-Beam Distribution. Under normal Circumstances, the first (slow) Population is the Core and the second (fast) Population is the Beam. When the Interplanetary Magnetic Field is folded back on itself due to Turbulence or other Processes the relation of the first and second Populations to the Core and Beam, respectively, is reversed (see, e.g., M.M. Neugebauer and B.E. Goldstein, AIP Conf. Proc. 1539, 46, 2013). The Vector Magnetic Field is given in RTN Coordinates and it was obtained for the Time at which the Peak of the Alpha Particle Distribution Function was measured. Only good Fits are retained.
DOI: 10.48322/0ct5-8096
title: Ulysses Solar Wind Plasma (SWOOPS) Ion Average Density, Temperature and Velocity

description: This Data Set contains 1 hr Averages of the Ion Density, Temperature and Velocity Data from the Ulysses Solar Wind Observations Over the Poles of the Sun, SWOOPS, Instrument. Density Units are cm^-3, Temperature Units are °K, Velocity Units are km/s. Data Set Contact: B.E. Goldstein, NASA Ames Research Center, USA. Principal Investigator: D.J. McComas, Southwest Research Institute, USA. Reference: Astron. Astrophys. Suppl. Ser., 92(2), 237-265, 1992. Relevant Web Sites: http://swoops.lanl.gov/