{ "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 https://www.spase-group.org/data/schema/spase-2_3_2.xsd", "Version": "2.3.2", "NumericalData": { "ResourceID": "spase://NASA/NumericalData/Ulysses/COSPIN/KET/Rates/PT10M", "ResourceHeader": { "ResourceName": "Ulysses Cosmic Ray and Solar Particle Investigation (COSPIN) Kiel Electron Telescope (KET) Proton, Helium, and Electron Spin-Integrated Counting Rates Data, 10 min Average Data", "AlternateName": "COSPIN-KET-RAT-10M", "ReleaseDate": "2021-04-27T15:38:11Z", "Description": "This Data Set contains 10 min Averages of: (a) Spin-Integrated Count Rates of Protons (2.7-5.4, 5.4-23.1, 34.1-125.0, 125.0-320.0, 320.0-2100 and >2100.0 MeV), Alpha Particles (6.0-20.4, 34.2-125.0, 125.0-320.0, 320.0-2100.0 and >2100.0 MeV/n), and Electrons (2.5-7.0, 7.0-170.0 and >170.0 MeV). (b) Eight-Sectored Count Rates of Protons (5.4-23.1 MeV) and Electrons (2.5-7.0 MeV). (c) Count Rates of D10, D20, C10, C20 and A01 single Detector Sensors. The Parameter Keys in the Parameter Level Segments below are specifically relevant to the UFA accessible Versions of the Data.", "Acknowledgement": "Please acknowledge the COSPIN PI, R. Bruce McKibben, the KET Co-PI, Bernd Heber, and the UDS and/or NSSDC", "Contact": [ { "PersonID": "spase://SMWG/Person/R.Bruce.McKibben", "Role": "PrincipalInvestigator" }, { "PersonID": "spase://SMWG/Person/Bernd.Heber", "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 4.5 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/KET Data Files", "URL": "http://ufa.esac.esa.int/ufa-sl-server/data-action?PROTOCOL=HTTP&PRODUCT_TYPE=ALL&FILE_NAME=cospin_ket_un.html&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 Kiel Electron Telescope Telescope, KET, 10 min Average Proton, Helium and Electron Count Rates and detector Count Rates" } ], "PriorID": [ "spase://VEPO/NumericalData/Ulysses/COSPIN/KET/RATES/PT10M", "spase://VSPO/NumericalData/Ulysses/COSPIN/KET/Rates/PT10M" ] }, "AccessInformation": [ { "RepositoryID": "spase://SMWG/Repository/ESA/ESAC/UlyssesFinalArchive", "Availability": "Online", "AccessRights": "Open", "AccessURL": { "Name": "Ulysses Final Archive Access to COSPIN/KET 10 min Average Proton, Helium, and Electron Spin-Integrated Counting Rates Data", "URL": "http://ufa.esac.esa.int/ufa/#data", "Description": "Parent Directory containing compressed Ulysses COSPIN/KET 10 min Average Rates Data organized in Daily ASCII Files ucosketaYYDOY.dat (YY and DOY are the two digit Year and the Day of Year, respectively) grouped together into Yearly Files (cosketYY.zip, where YY is the two digit Year)" }, "Format": "Text", "Encoding": "ZIP", "Acknowledgement": "Please acknowledge the COSPIN KET Co-PI, Bernd Heber, CAU Kiel" }, { "RepositoryID": "spase://SMWG/Repository/NASA/GSFC/SPDF", "Availability": "Online", "AccessRights": "Open", "AccessURL": [ { "Name": "FTP Access to CDF Files at SPDF", "URL": "ftps://spdf.gsfc.nasa.gov/pub/data/ulysses/particle/cospin_cdaweb/ket/", "Description": "KET Data Access via FTP in CDF Format from SPDF" }, { "Name": "HTTP Access to CDF Files at SPDF", "URL": "https://spdf.gsfc.nasa.gov/pub/data/ulysses/particle/cospin_cdaweb/ket/", "Description": "KET Data Access via HTTP in CDF Format from SPDF" } ], "Format": "CDF", "Acknowledgement": "Please acknowledge the Space Physics Data Facility at NASA/GSFC" }, { "RepositoryID": "spase://SMWG/Repository/NASA/GSFC/SPDF", "Availability": "Online", "AccessRights": "Open", "AccessURL": [ { "Name": "CDAWeb", "URL": "https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi?dataset=UY_M0_KET&index=sp_phys", "ProductKey": "UY_M0_KET", "Description": "Subset, Plot, List via CDAWeb" }, { "Name": "FTPS from SPDF (not with most browsers)", "URL": "ftps://spdf.gsfc.nasa.gov/pub/data/ulysses/particle/cospin/ket/10_min/", "Description": "KET Data Access via FTP in ASCII Format from SPDF" }, { "Name": "HTTPS from SPDF", "URL": "https://spdf.gsfc.nasa.gov/pub/data/ulysses/particle/cospin/ket/10_min/", "Description": "KET Data Access via HTTP in ASCII Format from SPDF" } ], "Format": "Text", "Acknowledgement": "Please acknowledge the Space Physics Data Facility at NASA/GSFC" }, { "RepositoryID": "spase://SMWG/Repository/NASA/GSFC/SPDF", "Availability": "Online", "AccessRights": "Open", "AccessURL": { "Name": "CDAWeb HAPI Server", "URL": "https://cdaweb.gsfc.nasa.gov/hapi", "Style": "HAPI", "ProductKey": "UY_M0_KET", "Description": "Web Service to this product using the HAPI interface." }, "Format": "CSV", "Acknowledgement": "Please acknowledge the Space Physics Data Facility at NASA/GSFC" } ], "InstrumentID": "spase://SMWG/Instrument/Ulysses/COSPIN/KET", "MeasurementType": "EnergeticParticles", "TemporalDescription": { "TimeSpan": { "StartDate": "1990-10-23T00:00:00.000", "StopDate": "2008-12-31T23:59:59.999" }, "Cadence": "PT10M" }, "ObservedRegion": "Heliosphere.Outer", "Parameter": [ { "Name": "Time for the record", "ParameterKey": "Time_PG1", "Description": "Time for the record given in Year, Day of Year, Hour, Minute, Seconds and coverage in percent. The given time represents the start of the averaging interval.", "Cadence": "PT10M", "Structure": { "Size": "6", "Element": [ { "Name": "Year", "Index": "1", "ValidMin": "1990", "ValidMax": "2008" }, { "Name": "Day of Year", "Index": "2", "ValidMin": "1", "ValidMax": "366" }, { "Name": "Hour of Day", "Index": "3", "ValidMin": "0", "ValidMax": "23" }, { "Name": "Minute of Hour", "Index": "4", "ValidMin": "0", "ValidMax": "59" }, { "Name": "Seconds of Minute", "Index": "5", "ValidMin": "0", "ValidMax": "59" }, { "Name": "Coverage", "Index": "6", "ValidMin": "0", "ValidMax": "100" } ] }, "Support": { "SupportQuantity": "Temporal" } }, { "Name": "COSPIN/KET 10-Minute Average 2.7-5.4 MeV Proton Spin-Averaged Count Rates (K1)", "ParameterKey": "K1", "Description": "10-minute average KET spin-averaged proton count rates between 2.7 and 5.4 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K1 18 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter. Background fluxes of K1 are a combination of components, including a high RTG background rate. This channel should be used only during event times.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.7", "High": "5.4", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 1 (K21)", "ParameterKey": "K21", "Description": "10-minute average KET proton count rates in spin sector 1 (of 8) between 5.4 and 23.1 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "5.4", "High": "23.1", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 2 (K22)", "ParameterKey": "K22", "Description": "10-minute average KET proton count rates in spin sector 2 (of 8) between 5.4 and 23.1 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "5.4", "High": "23.1", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 3 (K23)", "ParameterKey": "K23", "Description": "10-minute average KET proton count rates in spin sector 3 (of 8) between 5.4 and 23.1 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "5.4", "High": "23.1", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 4 (K24)", "ParameterKey": "K24", "Description": "10-minute average KET proton count rates in spin sector 4 (of 8) between 5.4 and 23.1 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "5.4", "High": "23.1", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 5 (K25)", "ParameterKey": "K25", "Description": "10-minute average KET proton count rates in spin sector 5 (of 8) between 5.4 and 23.1 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "5.4", "High": "23.1", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 6 (K26)", "ParameterKey": "K26", "Description": "10-minute average KET proton count rates in spin sector 6 (of 8) between 5.4 and 23.1 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "5.4", "High": "23.1", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 7 (K27)", "ParameterKey": "K27", "Description": "10-minute average KET proton count rates in spin sector 7 (of 8) between 5.4 and 23.1 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "5.4", "High": "23.1", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Count Rates in Spin Sector 8 (K28)", "ParameterKey": "K28", "Description": "10-minute average KET proton count rates in spin sector 8 (of 8) between 5.4 and 23.1 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K21-K28 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "5.4", "High": "23.1", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 5.4-23.1 MeV Proton Spin-Averaged Count Rates (P4)", "ParameterKey": "P4", "Description": "10-minute average KET spin-averaged proton count rates between 5.4 and 23.1 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= P4 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "5.4", "High": "23.1", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 34.1-125.0 MeV Proton Spin-Averaged Count Rates (K3)", "ParameterKey": "K3", "Description": "10-minute average KET spin-averaged proton count rates between 34.1 and 125.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K3 70.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "34.1", "High": "125.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 125.0-320.0 MeV Proton Spin-Averaged Count Rates (K34)", "ParameterKey": "K34", "Description": "10-minute average KET spin-averaged proton count rates between 125.0 and 320.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K34 152.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "125.0", "High": "320.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 320.0-2100.0 MeV Proton Spin-Averaged Count Rates (K12)", "ParameterKey": "K12", "Description": "10-minute average KET spin-averaged proton count rates between 320.0 and 2100.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K12 3300.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "320.0", "High": "2100.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average >2100.0 MeV Proton Spin-Averaged Count Rates (K10)", "ParameterKey": "K0", "Description": "10-minute average KET spin-averaged proton count rates >2100.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K10 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Proton", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2100.0", "High": "INF", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 6.0-20.4 MeV/n Helium Spin-Averaged Count Rates (K2)", "ParameterKey": "K2", "Description": "10-minute average KET spin-averaged helium count rates between 6.0 and 20.4 MeV/n", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K2 120 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "AlphaParticle", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "6.0", "High": "20.4", "Units": "MeV/n" } } }, { "Name": "COSPIN/KET 10-Minute Average 34.2-125.0 MeV/n Helium Spin-Averaged Count Rates (K33)", "ParameterKey": "K33", "Description": "10-minute average KET spin-averaged helium count rates between 34.2 and 125.0 MeV/n", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K33 70.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "AlphaParticle", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "34.2", "High": "125.0", "Units": "MeV/n" } } }, { "Name": "COSPIN/KET 10-Minute Average 125.0-320.0 MeV/n Helium Spin-Averaged Count Rates (K29)", "ParameterKey": "K29", "Description": "10-minute average KET spin-averaged helium count rates between 125.0 and 320.0 MeV/n", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K29 88.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "AlphaParticle", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "125.0", "High": "320.0", "Units": "MeV/n" } } }, { "Name": "COSPIN/KET 10-Minute Average 320.0-2100.0 MeV/n Helium Spin-Averaged Count Rates (K31)", "ParameterKey": "K31", "Description": "10-minute average KET spin-averaged helium count rates between 320.0 and 2100.0 MeV/n", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K31 3200.0 On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "AlphaParticle", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "320.0", "High": "2100.0", "Units": "MeV/n" } } }, { "Name": "COSPIN/KET 10-Minute Average >2100.0 MeV/n Helium Spin-Averaged Count Rates (K30)", "ParameterKey": "K30", "Description": "10-minute average KET spin-averaged helium count rates >2100.0 MeV/n", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K30 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "AlphaParticle", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2100.0", "High": "INF", "Units": "MeV/n" } } }, { "Name": "COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 1 (K13)", "ParameterKey": "K13", "Description": "10-minute average KET electron count rates in spin sector 1 (of 8) between 2.5 and 7.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.5", "High": "7.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 2 (K14)", "ParameterKey": "K14", "Description": "10-minute average KET electron count rates in spin sector 2 (of 8) between 2.5 and 7.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.5", "High": "7.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 3 (K15)", "ParameterKey": "K15", "Description": "10-minute average KET electron count rates in spin sector 3 (of 8) between 2.5 and 7.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.5", "High": "7.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 4 (K16)", "ParameterKey": "K16", "Description": "10-minute average KET electron count rates in spin sector 4 (of 8) between 2.5 and 7.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.5", "High": "7.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 5 (K17)", "ParameterKey": "K17", "Description": "10-minute average KET electron count rates in spin sector 5 (of 8) between 2.5 and 7.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.5", "High": "7.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 6 (K18)", "ParameterKey": "K18", "Description": "10-minute average KET electron count rates in spin sector 6 (of 8) between 2.5 and 7.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.5", "High": "7.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 7 (K19)", "ParameterKey": "K19", "Description": "10-minute average KET electron count rates in spin sector 7 (of 8) between 2.5 and 7.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.5", "High": "7.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Count Rates in Spin Sector 8 (K20)", "ParameterKey": "K20", "Description": "10-minute average KET electron count rates in spin sector 8 (of 8) between 2.5 and 7.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K13-K20 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.5", "High": "7.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 2.5-7.0 MeV Electron Spin-Averaged Count Rates (E4)", "ParameterKey": "E4", "Description": "10-minute average KET spin-averaged electron count rates between 2.5 and 7.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= E4 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "2.5", "High": "7.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average 7.0-170.0 MeV Electron Spin-Averaged Count Rates (K11)", "ParameterKey": "K11", "Description": "10-minute average KET spin-averaged electron count rates between 7.0 and 170.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K11 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "7.0", "High": "170.0", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average >170.0 MeV Electron Spin-Averaged Count Rates (K32)", "ParameterKey": "K32", "Description": "10-minute average KET spin-averaged electron count rates >170.0 MeV", "Caveats": "Only rates C are given, since no simple estimates of the intensities can be done Intensities (I) must be derived by dividing through the integral geometric factor Gi, and by correcting through Pulse Height Analysis. I=C/Gi Values of the geometrical Factor Gi = (counting rate)/(Intensity): KET Channel Gi ============================= K32 N/A On 10 min averages some of the channels have limitations because of RTG background. Very slow increases are a sign that backgrounf levels are reached (a few percent per year). Get Low Flux Values from the PI for longer Accumulation Time Periods when KET is saturated or is working in a \"calibration mode\" have been omitted: eg. March event 1991 peak fluxes in the June to August period 1991 Jovian encounter.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": "Electron", "Qualifier": "Average", "ParticleQuantity": "CountRate", "EnergyRange": { "Low": "170.0", "High": "INF", "Units": "MeV" } } }, { "Name": "COSPIN/KET 10-Minute Average D10 Detector Counting Rate (D10)", "ParameterKey": "D10", "Description": "10-minute average KET D10 detector counting rate", "Caveats": "Rate channel D10 includes all particles depositing energy greater than the minimum discriminator level.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": [ "Proton", "AlphaParticle", "Ion", "Electron" ], "Qualifier": "Average", "ParticleQuantity": "Counts" } }, { "Name": "COSPIN/KET 10-Minute Average D20 Detector Counting Rate (D20)", "ParameterKey": "D20", "Description": "10-minute average KET D20 detector counting rate", "Caveats": "Rate channel D20 includes all particles depositing energy greater than the minimum discriminator level.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": [ "Proton", "AlphaParticle", "Ion", "Electron" ], "Qualifier": "Average", "ParticleQuantity": "Counts" } }, { "Name": "COSPIN/KET 10-Minute Average C10 Detector Counting Rate (D10)", "ParameterKey": "C10", "Description": "10-minute average KET C10 detector counting rate", "Caveats": "Rate channel C10 includes all particles depositing energy greater than the minimum discriminator level.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": [ "Proton", "AlphaParticle", "Ion", "Electron" ], "Qualifier": "Average", "ParticleQuantity": "Counts" } }, { "Name": "COSPIN/KET 10-Minute Average C20 Detector Counting Rate (D10)", "ParameterKey": "C20", "Description": "10-minute average KET C20 detector counting rate", "Caveats": "Rate channel C20 includes all particles depositing energy greater than the minimum discriminator level.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": [ "Proton", "AlphaParticle", "Ion", "Electron" ], "Qualifier": "Average", "ParticleQuantity": "Counts" } }, { "Name": "COSPIN/KET 10-Minute Average A01 Detector Counting Rate (A01)", "ParameterKey": "A01", "Description": "10-minute average KET A01 detector counting rate", "Caveats": "Rate channel A01 includes all particles depositing energy greater than the minimum discriminator level.", "Cadence": "PT10M", "Units": "s^-1", "ValidMin": "0.0", "ValidMax": "1000000", "FillValue": "-707", "Particle": { "ParticleType": [ "Proton", "AlphaParticle", "Ion", "Electron" ], "Qualifier": "Average", "ParticleQuantity": "Counts" } } ] } } }