{
  "Spase": {
    "xmlns": "http://www.spase-group.org/data/schema",
    "xmlns:xsi": "http://www.w3.org/2001/XMLSchema-instance",
    "xsi:schemaLocation": "http://www.spase-group.org/data/schema http://www.spase-group.org/data/schema/spase-2_2_9.xsd",
    "Version": "2.2.9",
    "NumericalData": {
      "ResourceID": "spase://NASA/NumericalData/Ulysses/COSPIN/HET/PHA/Ion/Fluxes/P1D",
      "ResourceHeader": {
        "ResourceName": "Ulysses Cosmic Ray and Solar Particle Investigation (COSPIN) High Energy Telescope (HET) Proton and Helium PHA based Fluxes in ASCII Format, Daily Average Data",
        "AlternateName": "COSPIN-HET-FLUXES-P1D",
        "ReleaseDate": "2020-07-07T21:15:39Z",
        "Description": "This Data Set contains Daily Average Proton and Helium PHA based Fluxes and Errors from the COSPIN High Energy Telescope (HET) in the approximate Energy Ranges 39-70 MeV/n and 71-94 MeV/n from Day 296, 1990 through Day 181, 2009",
        "Acknowledgement": "Please acknowledge R. Bruce McKibben, Space Science Center, University of New Hampshire",
        "Contact": [
          {
            "PersonID": "spase://SMWG/Person/R.Bruce.McKibben",
            "Role": [
              "PrincipalInvestigator",
              "DataProducer"
            ]
          },
          {
            "PersonID": "spase://SMWG/Person/James.Connell",
            "Role": "CoInvestigator"
          },
          {
            "PersonID": "spase://SMWG/Person/Ming.Zhang",
            "Role": "CoInvestigator"
          },
          {
            "PersonID": "spase://SMWG/Person/Cecil.Tranquille",
            "Role": "ArchiveSpecialist"
          }
        ],
        "InformationURL": [
          {
            "Name": "The Ulysses Cosmic Ray and Solar Particle Investigation, COSPIN",
            "URL": "http://ufa.esac.esa.int/ufa/#instruments",
            "Description": "Published Description of the COSPIN Instrumentation, J.A. Simpson et al., Astron. Astrophys. Suppl. Ser. 92, 365-399, 1992. See especially Section 4.3 for a detailed Description of the High Energy Telescopes, HET. An electronic Copy of this Paper is available at http://adsbit.harvard.edu/cgi-bin/nph-iarticle_query?1992A%26AS...92..365S&defaultprint=YES&filetype=.pdf."
          },
          {
            "Name": "User Notes for the COSPIN/HET Data Files",
            "URL": "http://ufa.esac.esa.int/ufa-sl-server/data-action?PROTOCOL=HTTP&PRODUCT_TYPE=ALL&FILE_NAME=het_usernotes.pdf&FILE_PATH=/ufa/HiRes/doc/cospin",
            "Description": "The User Notes File at the Ulysses Final Archive (UFA) describes the Format of the ASCII Data Files for the COSPIN High Energy Telescope, HET, Daily Average PHA based Protons and Helium in two Energy Intervals covering the approximate Energy Ranges 39-70 and 71-94 MeV/n"
          }
        ],
        "PriorID": [
          "spase://VEPO/NumericalData/Ulysses/COSPIN/HET/PH_Fluxes/P1D",
          "spase://VSPO/NumericalData/Ulysses/COSPIN/HET/PHA/Ion/Fluxes/P1D"
        ]
      },
      "AccessInformation": {
        "RepositoryID": "spase://SMWG/Repository/ESA/ESAC/UlyssesFinalArchive",
        "Availability": "Online",
        "AccessRights": "Open",
        "AccessURL": {
          "Name": "Ulysses Final Archive Access to COSPIN/HET Daily Average Proton and Helium PHA based Fluxes",
          "URL": "http://ufa.esac.esa.int/ufa/#data",
          "Description": "ASCII Data File containing all Ulysses COSPIN/HET Daily Average PHA based Flux Data. Each Day is represented by one Line containing, in eleven Columns:\nFractional Year since 1900 of Midpoint of Average (Day 170, 2007 = 107.46438), Fractional Day of Year of Midpoint of Average (January 1 = 1, so Day 170 = 170.5), Flux of 39-70 MeV Protons, Statistical Error on Flux of 39-70 MeV Protons, Flux of 71-94 MeV Protons, Statistical Error on Flux of 71-94 MeV Protons, Flux of 39-71 MeV/n Helium, Statistical Error on Flux of 39-71 MeV/n, Helium Flux of 71-94 MeV/n Helium, Statistical Error on Flux of 72-95 MeV/n Helium, and Seconds of Data Coverage during the Day, Invalid or Missing Data are represented by -1.000E+00"
        },
        "Format": "Text",
        "Encoding": "ASCII",
        "Acknowledgement": "Please acknowledge R. Bruce McKibben, Space Science Center, University of New Hampshire"
      },
      "InstrumentID": "spase://SMWG/Instrument/Ulysses/COSPIN/HET",
      "MeasurementType": "EnergeticParticles",
      "TemporalDescription": {
        "TimeSpan": {
          "StartDate": "1990-10-23T00:00:00.000",
          "StopDate": "2009-06-30T23:59:59.999"
        },
        "Cadence": "P1D"
      },
      "ObservedRegion": "Heliosphere.Outer",
      "Parameter": [
        {
          "Name": "Time for the record",
          "ParameterKey": "Columns_1_2",
          "Description": "Time for the record given in fractional Year (-1900) and fractional Day of Year. The given time represents the middle of the nominal averaging interval.",
          "Cadence": "P1D",
          "Structure": {
            "Size": "2",
            "Element": [
              {
                "Name": "Year",
                "Index": "1",
                "ValidMin": "90.80959",
                "ValidMax": "110.49589",
                "FillValue": "Null"
              },
              {
                "Name": "Fractional Day of Year",
                "Index": "2",
                "ValidMin": "1.5",
                "ValidMax": "366.5",
                "FillValue": "Null"
              }
            ]
          },
          "Support": {
            "SupportQuantity": "Temporal"
          }
        },
        {
          "Name": "COSPIN/HET 39-70 MeV (H4) Proton Flux",
          "ParameterKey": "Column_3",
          "Description": "Flux [1/(s cm^2 sr MeV)] of 39-70 MeV protons averaged over one Day.",
          "Caveats": "Energy ranges are approximate, based on a minimum error analysis as a function of spectral form (so-called Bow Tie analysis). The effective geometric factor and end point energies have been chosen to give minimal dispersion in calculated fluxes over a range of plausible proton spectra using events generated from various spectra by Monte-Carlo simulations. Typical systematic uncertainties resulting from such spectral dependence of the response are of order +/- 10 per cent on the flux, in addition to statistical counting uncertainties.",
          "Cadence": "P1D",
          "Units": "(cm^2 s sr MeV)^-1",
          "ValidMin": "0.0",
          "ValidMax": "1000000",
          "FillValue": "-1.000E+00",
          "Particle": {
            "ParticleType": "Proton",
            "Qualifier": "Average",
            "ParticleQuantity": "NumberFlux",
            "EnergyRange": {
              "Low": "39",
              "High": "70",
              "Units": "MeV"
            }
          }
        },
        {
          "Name": "COSPIN/HET 39-70 MeV (H4) Proton Flux Statistical Error",
          "ParameterKey": "Column_4",
          "Description": "Square Root of N Statistical Error on Flux [1/(s cm^2 sr MeV)] of 39-70 MeV protons",
          "Caveats": "None beyond those on Flux",
          "Cadence": "P1D",
          "Units": "(cm^2 s sr MeV)^-1",
          "ValidMin": "0.0",
          "ValidMax": "1000000",
          "FillValue": "-1.000E+00",
          "Particle": {
            "ParticleType": "Proton",
            "Qualifier": "StandardDeviation",
            "ParticleQuantity": "NumberFlux",
            "EnergyRange": {
              "Low": "39",
              "High": "70",
              "Units": "MeV"
            }
          }
        },
        {
          "Name": "COSPIN/HET 71-94 MeV (H5) Proton Flux",
          "ParameterKey": "Column_5",
          "Description": "Flux [1/(s cm^2 sr MeV)] of 71-94 MeV protons averaged over one Day.",
          "Caveats": "Energy ranges are approximate, based on a minimum error analysis as a function of spectral form (so-called Bow Tie analysis). The effective geometric factor and end point energies have been chosen to give minimal dispersion in calculated fluxes over a range of plausible proton spectra using events generated from various spectra by Monte-Carlo simulations. Typical systematic uncertainties resulting from such spectral dependence of the response are of order +/- 10 per cent on the flux, in addition to statistical counting uncertainties.",
          "Cadence": "P1D",
          "Units": "(cm^2 s sr MeV)^-1",
          "ValidMin": "0.0",
          "ValidMax": "1000000",
          "FillValue": "-1.000E+00",
          "Particle": {
            "ParticleType": "Proton",
            "Qualifier": "Average",
            "ParticleQuantity": "NumberFlux",
            "EnergyRange": {
              "Low": "71",
              "High": "94",
              "Units": "MeV"
            }
          }
        },
        {
          "Name": "COSPIN/HET 71-94 MeV (H5) Proton Flux Statistical Error",
          "ParameterKey": "Column_6",
          "Description": "Square Root of N Statistical Error on Flux [1/(s cm^2 sr MeV)] of 71-94 MeV protons",
          "Caveats": "None beyond those on Flux",
          "Cadence": "P1D",
          "Units": "(cm^2 s sr MeV)^-1",
          "ValidMin": "0.0",
          "ValidMax": "1000000",
          "FillValue": "-1.000E+00",
          "Particle": {
            "ParticleType": "Proton",
            "Qualifier": "StandardDeviation",
            "ParticleQuantity": "NumberFlux",
            "EnergyRange": {
              "Low": "71",
              "High": "94",
              "Units": "MeV"
            }
          }
        },
        {
          "Name": "COSPIN/HET 39-71 (H4) MeV/nucleon Helium Flux",
          "ParameterKey": "Column_7",
          "Description": "Flux [1/(s cm^2 sr MeV/nucleon)] of 39-71 MeV/nucleon Helium nuclei averaged over one Day.",
          "Caveats": "Energy ranges are approximate, based on a minimum error analysis as a function of spectral form (so-called \"Bow Tie analysis\") wherein the effective geometric factor and end point energies are chosen to give minimal dispersion in calculated fluxes over a range of plausible proton spectra using events generated from various spectra by Monte-Carlo simulations. Typical systematic uncertainties resulting from such spectral dependence of the response are of order +/- 10 per cent on the flux, in addition to statistical counting uncertainties.",
          "Cadence": "P1D",
          "Units": "(cm^2 s sr MeV/n)^-1",
          "ValidMin": "0.0",
          "ValidMax": "1000000",
          "FillValue": "-1.000E+00",
          "Particle": {
            "ParticleType": "AlphaParticle",
            "Qualifier": "Average",
            "ParticleQuantity": "NumberFlux",
            "EnergyRange": {
              "Low": "39",
              "High": "71",
              "Units": "MeV/n"
            }
          }
        },
        {
          "Name": "COSPIN/HET 39-71 MeV/nucleon (H4) Helium Flux Statistical Error",
          "ParameterKey": "Column_8",
          "Description": "Square Root of N Statistical Error on Flux [1/(s cm^2 sr MeV)] of 39-71 MeV/nucleon Helium nuclei",
          "Caveats": "None beyond those on Flux",
          "Cadence": "P1D",
          "Units": "(cm^2 s sr MeV/n)^-1",
          "ValidMin": "0.0",
          "ValidMax": "1000000",
          "FillValue": "-1.000E+00",
          "Particle": {
            "ParticleType": "AlphaParticle",
            "Qualifier": "StandardDeviation",
            "ParticleQuantity": "NumberFlux",
            "EnergyRange": {
              "Low": "39",
              "High": "71",
              "Units": "MeV/n"
            }
          }
        },
        {
          "Name": "COSPIN/HET 72-95 (H5) MeV/nucleon Helium Flux",
          "ParameterKey": "Column_9",
          "Description": "Flux [1/(s cm^2 sr MeV)] of 71-95 MeV Helium nuclei averaged over one Day.",
          "Caveats": "Energy ranges are approximate, based on a minimum error analysis as a function of spectral form (so-called Bow Tie analysis). The effective geometric factor and end point energies have been chosen to give minimal dispersion in calculated fluxes over a range of plausible proton spectra using events generated from various spectra by Monte-Carlo simulations. Typical systematic uncertainties resulting from such spectral dependence of the response are of order +/- 10 per cent on the flux, in addition to statistical counting uncertainties.",
          "Cadence": "P1D",
          "Units": "(cm^2 s sr MeV/n)^-1",
          "ValidMin": "0.0",
          "ValidMax": "1000000",
          "FillValue": "-1.000E+00",
          "Particle": {
            "ParticleType": "AlphaParticle",
            "Qualifier": "Average",
            "ParticleQuantity": "NumberFlux",
            "EnergyRange": {
              "Low": "72",
              "High": "95",
              "Units": "MeV/n"
            }
          }
        },
        {
          "Name": "COSPIN/HET 72-95 MeV/nucleon (H5) Helium Flux Statistical Error",
          "ParameterKey": "Column_10",
          "Description": "Square Root of N Statistical Error on Flux [1/(s cm^2 sr MeV)] of 72-95 MeV/nucleon Helium nuclei",
          "Caveats": "None beyond those on Flux",
          "Cadence": "P1D",
          "Units": "(cm^2 s sr MeV/n)^-1",
          "ValidMin": "0.0",
          "ValidMax": "1000000",
          "FillValue": "-1.000E+00",
          "Particle": {
            "ParticleType": "AlphaParticle",
            "Qualifier": "StandardDeviation",
            "ParticleQuantity": "NumberFlux",
            "EnergyRange": {
              "Low": "72",
              "High": "95",
              "Units": "MeV/n"
            }
          }
        },
        {
          "Name": "Seconds of Data Included",
          "ParameterKey": "Column_11",
          "Description": "Seconds of data available for computing the particle fluxes",
          "Cadence": "P1D",
          "Support": {
            "SupportQuantity": "Temporal"
          }
        }
      ]
    }
  }
}