Created instruments PSP/ISOIS/epiHi and epiLow and dataset HET

Quentin Brzustowski
1 parent 21b76408
Showing 3 changed files with 229 additions and 0 deletions Show diff stats
Instrument/CDPP-AMDA/PSP/epiHi.xml
Instrument/CDPP-AMDA/PSP/epiLo.xml
NumericalData/CDPP-AMDA/PSP/epiHi/psp-het-1min.xml
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+<?xml version="1.0" encoding="UTF-8"?>
+<Spase xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xmlns="http://www.spase-group.org/data/schema" xsi:schemaLocation="http://www.spase-group.org/data/schema http://amda.irap.omp.eu/public/schemas/spase-2_3_1.xsd">
+  <Version>2.2.6</Version>
+  <Instrument>
+    <ResourceID>spase://CNES/Instrument/CDPP-AMDA/PSP/epiHi</ResourceID>
+    <ResourceHeader>
+      <ResourceName>ISoIS EPI-Hi</ResourceName>
+      <AlternateName>Energetic Particle Instrument Hi-Energy</AlternateName>
+      <ReleaseDate>2019-11-12T16:00:05Z</ReleaseDate>
+      <Description>The science objective of the Integrated Science Investigation of the Sun, ISOIS, 
+        experiment is to explore the physical mechanisms that produce, accelerate, and transport energetic 
+        particles in the inner heliosphere. This will be achieved by observing energetic electrons, protons, 
+        and heavy ions in the Sun's atmosphere and inner heliosphere to learn about the origin and seed population 
+        of solar energetic particles, how these and other particles are accelerated, and what mechanisms are 
+        responsible for transporting the different particle populations into the heliosphere. It will also 
+        contribute to tracing the flow of energy that heats and accelerates the solar corona and solar wind, 
+        and determining the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind. 
+        The Integrated Science Investigation of the Sun consists of two instruments, EPI-Lo and EPI-Hi, mounted on 
+        the side of the spacecraft near the back ram-facing side, protected by the heat shield.
+        The EPI-Hi instrument system is based on ion-implanted solid-state detectors. It comprises three detector stacks 
+        (particle telescopes). One is designated a High Energy Telescope (HET) and two are designated Low-Energy Telescopes (LET1 and LET2). 
+      </Description>
+      <Acknowledgement>Please Acknowledge the National Aeronautics and Space Administration, NASA</Acknowledgement>
+      <Contact>
+        <PersonID>spase://SMWG/Person/David.J.McComas</PersonID>
+        <Role>PrincipalInvestigator</Role>
+      </Contact>
+      <Contact>
+        <PersonID>spase://SMWG/Person/Eric.R.Christian</PersonID>
+        <Role>DeputyPI</Role>
+      </Contact>
+      <InformationURL>
+        <Name>Parker Solar Probe Mission Instrument web page, JPL</Name>
+        <URL>http://parkersolarprobe.jhuapl.edu/Spacecraft/index.php#Instruments</URL>
+      </InformationURL>
+      <InformationURL>
+        <Name>Parker Solar Probe Mission Instrument web page, NASA</Name>
+        <URL>https://www.nasa.gov/content/goddard/parker-solar-probe-instruments/</URL>
+      </InformationURL>
+    </ResourceHeader>
+    <InstrumentType>SolidStateDetector</InstrumentType>
+    <InvestigationName>Parker Solar Probe ISOIS Investigation</InvestigationName>
+    <ObservatoryID>spase://CNES/Observatory/CDPP-AMDA/PSP</ObservatoryID>
+  </Instrument>
+</Spase>
@@ -0,0 +1,52 @@
+<?xml version="1.0" encoding="UTF-8"?>
+<Spase xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xmlns="http://www.spase-group.org/data/schema" xsi:schemaLocation="http://www.spase-group.org/data/schema http://amda.irap.omp.eu/public/schemas/spase-2_3_1.xsd">
+  <Version>2.2.6</Version>
+  <Instrument>
+    <ResourceID>spase://CNES/Instrument/CDPP-AMDA/PSP/epiLo</ResourceID>
+    <ResourceHeader>
+      <ResourceName>ISoIS EPI-Lo</ResourceName>
+      <AlternateName>Energetic Particle Instrument Low-Energy</AlternateName>
+      <ReleaseDate>2019-11-12T16:00:05Z</ReleaseDate>
+      <Description>The science objective of the Integrated Science Investigation of the Sun, ISOIS, 
+        experiment is to explore the physical mechanisms that produce, accelerate, and transport energetic 
+        particles in the inner heliosphere. This will be achieved by observing energetic electrons, protons, 
+        and heavy ions in the Sun's atmosphere and inner heliosphere to learn about the origin and seed population 
+        of solar energetic particles, how these and other particles are accelerated, and what mechanisms are 
+        responsible for transporting the different particle populations into the heliosphere. It will also 
+        contribute to tracing the flow of energy that heats and accelerates the solar corona and solar wind, 
+        and determining the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind. 
+        The Integrated Science Investigation of the Sun consists of two instruments, EPI-Lo and EPI-Hi, mounted on 
+        the side of the spacecraft near the back ram-facing side, protected by the heat shield.
+        The EPI-Lo instrument is disc-shaped and divided into 8 sections, or wedge assemblies, each section holding 10 
+        foil-covered apertures. Each aperture faces a slightly different direction, together they provide coverage of 
+        nearly a full hemisphere. The apertures allow particles to enter the wedge interior, which contains a time-of-flight 
+        mass spectrometer. Ions pass through the thin foils in the apertures and then hit a stop foil backed by a 
+        solid-state detector. Electrons are detected by independent solid-state detectors covered by ~2 micron thick 
+        aluminum flashing. Epi-Lo measures energetic ions from 0.02 MeV/n to 15 MeV total energy, protons from 
+        about 0.04 MeV to 7 MeV, and energetic electrons from approximately 25 keV to 1000 keV. 
+        It measures the ion composition and pitch-angle distributions from 30 keV/n up to 0.3 MeV/n or 1.0 MeV/n 
+        every 5 or 30 seconds. It can return data for up to 64 energy bins and 80 angular ranges (one for each aperture). 
+      </Description>
+      <Acknowledgement>Please Acknowledge the National Aeronautics and Space Administration, NASA</Acknowledgement>
+      <Contact>
+        <PersonID>spase://SMWG/Person/David.J.McComas</PersonID>
+        <Role>PrincipalInvestigator</Role>
+      </Contact>
+      <Contact>
+        <PersonID>spase://SMWG/Person/Eric.R.Christian</PersonID>
+        <Role>DeputyPI</Role>
+      </Contact>
+      <InformationURL>
+        <Name>Parker Solar Probe Mission Instrument web page, JPL</Name>
+        <URL>http://parkersolarprobe.jhuapl.edu/Spacecraft/index.php#Instruments</URL>
+      </InformationURL>
+      <InformationURL>
+        <Name>Parker Solar Probe Mission Instrument web page, NASA</Name>
+        <URL>https://www.nasa.gov/content/goddard/parker-solar-probe-instruments/</URL>
+      </InformationURL>
+    </ResourceHeader>
+    <InstrumentType>MassSpectrometer</InstrumentType>
+    <InvestigationName>Parker Solar Probe ISOIS Investigation</InvestigationName>
+    <ObservatoryID>spase://CNES/Observatory/CDPP-AMDA/PSP</ObservatoryID>
+  </Instrument>
+</Spase>
@@ -0,0 +1,132 @@
+<?xml version="1.0" encoding="UTF-8"?>
+<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_3_0.xsd">
+   <Version>2.3.0</Version>
+   <NumericalData>
+      <ResourceID>spase://CNES/NumericalData/CDPP-AMDA/PSP/epiHi/psp-het-1min</ResourceID>
+      <ResourceHeader>
+          <ResourceName>HET 1min</ResourceName>
+          <AlternateName>High Energy Telescope 1 min rate</AlternateName>      
+          <ReleaseDate>2019-11-12T10:48:29Z</ReleaseDate>
+         <Description>         
+             The HET is a cylinder containing a central stack of detector disks and two single detector disks, 
+             one at each end. The individual detectors in the central stack have thicknesses of 1000 microns. 
+             Three of the detectors in the central stack comprise two 1000-micron disks connected to act as single 
+             2000 micron detectors. The end detector disks are 500 microns thick. The front end detector and the 
+             outermost detectors at each end of the central stack are each divided into five active elements, 
+             a central bulls-eye and four quadrants, each of equal area. Which active area hit on different disks 
+             gives directional information on the particle. An outer annular segment of each detector acts as an 
+             anti-coincidence shield to detect particles that exit the cylinder before passing through all the detectors. 
+             The HET covers electrons up to approximately 6 MeV and protons and heavy ions to at least 100 MeV/n. 
+             The lower range overlaps the high end of the Low Energy Telescopes. 
+             The measurements are divided into two different sides of the instrument, A and B
+         </Description>
+         <Acknowledgement>
+             Please acknowledge the National Aeronautics and Space Administration, NASA
+         </Acknowledgement>
+         <Contact>
+           <PersonID>spase://SMWG/Person/David.J.McComas</PersonID>
+           <Role>PrincipalInvestigator</Role>
+         </Contact>
+          <Contact>
+              <PersonID>spase://SMWG/Person/Eric.R.Christan</PersonID>
+              <Role>DeputyPI</Role>
+          </Contact>
+          <InformationURL>
+           <Name>PSP/ISoIS Energetic Particle Data - User Guide</Name>
+              <URL>https://spdf.sci.gsfc.nasa.gov/pub/data/psp/isois/ISOIS_Data_Glossary.pdf</URL>
+         </InformationURL>
+         <InformationURL>
+            <Name>Parker Solar Probe Mission Instrument web page, JPL</Name>
+             <URL>http://parkersolarprobe.jhuapl.edu/Spacecraft/index.php#Instruments</URL>
+         </InformationURL>
+      </ResourceHeader>
+      <AccessInformation>
+         <RepositoryID>spase://SMWG/Repository/CNES/CDPP-AMDA</RepositoryID>
+         <Availability>Online</Availability>
+         <AccessRights>Open</AccessRights>
+         <AccessURL>
+            <Name>AMDA at CDPP</Name>
+            <URL>
+                http://amda.cdpp.eu
+            </URL>
+         </AccessURL>
+         <Format>Text</Format>
+         <Acknowledgement>
+                AMDA is a science analysis system provided by the Centre de Donnees de la 
+                Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and 
+                Universite Paul Sabatier, Toulouse
+         </Acknowledgement>
+      </AccessInformation>
+      <ProviderName>SPDF</ProviderName> 
+       <ProviderResourceName>psp/fields/l2/mag_rtn_1min/</ProviderResourceName>
+      <ProviderAcknowlegment> 
+          Please acknowledge the CDAWeb team at GSFC/SPDF.</ProviderAcknowlegment>
+      <InstrumentID>spase://CNES/Instrument/CDPP-AMDA/PSP/MAG</InstrumentID>
+      <MeasurementType>EnergeticParticles</MeasurementType>
+      <TemporalDescription>
+         <TimeSpan>
+            <StartDate>2018-09-02T00:00:12Z</StartDate>
+             <StopDate>2025-08-12T23:59:55Z</StopDate>
+         </TimeSpan>
+         <Cadence>PT60S</Cadence>
+      </TemporalDescription>
+      <ObservedRegion>Heliosphere.Inner</ObservedRegion>
+      <ObservedRegion>Sun.Corona</ObservedRegion>
+      <Parameter>
+         <Name>H flux side A</Name>
+         <ParameterKey>psp_het_1min_AHf</ParameterKey>
+         <Description>
+             Proton flux side A
+         </Description>
+         <Units>1/cm²/sr/s/(MeV/nuc)</Units>
+         <RenderingHints>
+              <DisplayType>Spectrogram</DisplayType>
+         </RenderingHints>
+          <Particle>
+              <ParticleQuantity>EnergyFlux</ParticleQuantity>
+          </Particle>
+      </Parameter>
+       <Parameter>
+           <Name>H flux side B</Name>
+           <ParameterKey>psp_het_1min_BHf</ParameterKey>
+           <Description>
+               Proton flux side B
+           </Description>
+           <Units>1/cm²/sr/s/(MeV/nuc)</Units>
+           <RenderingHints>
+               <DisplayType>Spectrogram</DisplayType>
+           </RenderingHints>
+           <Particle>
+               <ParticleQuantity>EnergyFlux</ParticleQuantity>
+           </Particle>
+       </Parameter>
+       <Parameter>
+           <Name>He flux side A</Name>
+           <ParameterKey>psp_het_1min_AHef</ParameterKey>
+           <Description>
+               Helium flux side A
+           </Description>
+           <Units>1/cm²/sr/s/(MeV/nuc)</Units>
+           <RenderingHints>
+               <DisplayType>Spectrogram</DisplayType>
+           </RenderingHints>
+           <Particle>
+               <ParticleQuantity>EnergyFlux</ParticleQuantity>
+           </Particle>
+       </Parameter>
+       <Parameter>
+           <Name>He flux side B</Name>
+           <ParameterKey>psp_het_1min_BHef</ParameterKey>
+           <Description>
+               Helium flux side B
+           </Description>
+           <Units>1/cm²/sr/s/(MeV/nuc)</Units>
+           <RenderingHints>
+               <DisplayType>Spectrogram</DisplayType>
+           </RenderingHints>
+           <Particle>
+               <ParticleQuantity>EnergyFlux</ParticleQuantity>
+           </Particle>
+       </Parameter>
+</NumericalData>
+</Spase>