so-ept-e.total.xml
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<?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/Solar_Orbiter/EPD/so-ept-e.total</ResourceID>
<ResourceHeader>
<ResourceName>total flux</ResourceName>
<AlternateName>Total Electron Flux</AlternateName>
<ReleaseDate>2019-11-12T10:48:29Z</ReleaseDate>
<Description>Solar Orbiter, Level 2 Data, Energetic Particle Detector, Electron and Proton Telescope, Rates.
EPT measures electrons and ions in the lower part of the energetic particle spectrum. It
effectuates measurements in 4 different fields of view :
* Anti-Sunward Flow. Detector looks in the direction of the mean Parker spiral towards the Sun.
* Sunward Flow. Detector looks opposite to the Sun direction.
* Northward Flow. Detector looks towards the south ecliptic hemisphere.
* Southward Flow. Detector looks towards the north ecliptic hemisphere.
Additionally, EPT has 2 channels that separate electrons and ions:
* Magnet channel. Uses a permanent magnet to deflect electrons. It measures protons with energies between 25 keV and 6.5 MeV and alpha particles up to 25 MeV.
* Foil channel. Equipped with a foil that absorbs ions, it measures electrons in the energy range 25–500 keV. Ions with energies above 400 keV can penetrate the foil, contaminating the electron measurements.
</Description>
<Acknowledgement>See http://espada.uah.es/epd/EPD_data.php</Acknowledgement>
<Contact>
<PersonID>spase://CDPP/Person/J.Rodrigues-Pacheco</PersonID>
<Role>PrincipalInvestigator</Role>
</Contact>
<InformationURL>
<Name>SolO Archive Support Data</Name>
<URL>https://issues.cosmos.esa.int/solarorbiterwiki/display/SOSP/Archive+Support+Data</URL>
<Description></Description>
</InformationURL>
<Association>
<AssociationID>solo-epd-eptel</AssociationID>
<AssociationType>PartOf</AssociationType>
<Note>L2 : electron flux</Note>
</Association>
<PriorID>so-ept-e.sun</PriorID>
<PriorID>so-ept-e.anti</PriorID>
<PriorID>so-ept-e.north</PriorID>
<PriorID>so-ept-e.south</PriorID>
</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>http://soar.esac.esa.int/soar</ProviderName>
<ProviderResourceName>EPD-EPT-SUN-RATES</ProviderResourceName>
<ProviderAcknowlegment></ProviderAcknowlegment>
<InstrumentID>spase://CNES/Instrument/CDPP-AMDA/Solar_Orbiter/EPD-EPT</InstrumentID>
<MeasurementType>EnergeticParticles</MeasurementType>
<TemporalDescription>
<TimeSpan>
<StartDate>2018-09-02T00:00:12Z</StartDate>
<StopDate>2025-08-12T23:59:55Z</StopDate>
</TimeSpan>
<CadenceMin>PT60S</CadenceMin>
<CadenceMax>PT300S</CadenceMax>
</TemporalDescription>
<ObservedRegion>Heliosphere.Inner</ObservedRegion>
<ObservedRegion>Sun.Corona</ObservedRegion>
<Caveats>Ions with energies around 500 keV can penetrate the foil and give a signal in the electron
channel. In the presence of high ion flux, there could be a considerable contamination from ions in this product.</Caveats>
<Parameter>
<Name>el flux: total</Name>
<ParameterKey>solo_ept_tot_eflux</ParameterKey>
<Description>Particle flux in foil channel</Description>
<Ucd/>
<Units>1/(s cm^2 sr MeV)</Units>
<UnitsConversion/>
<RenderingHints>
<DisplayType>Spectrogram</DisplayType>
</RenderingHints>
<Structure>
<Size>34</Size>
</Structure>
</Parameter>
</NumericalData>
</Spase>