CDPP / CNES

Commit e6385f90ebec7f26eb7ff9bcdc6794cfea26ecc6

Authored by Benjamin Renard
1 parent 3e551342
Exists in juice_jdc and in 3 other branches amdadev, cleanup_registry_master, cleanup_registry_merged

Add PSP FIELDS RFS/LFR SQTN (#9965)

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Instrument/CDPP-AMDA/PSP/LFR.xml 0 → 100644
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  1 +<?xml version="1.0" encoding="UTF-8" standalone="yes"?>
  2 +<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://www.spase-group.org/data/schema/spase-2_3_1.xsd" lang="en">
  3 + <Version>2.3.1</Version>
  4 + <Instrument>
  5 + <ResourceID>spase://CNES/Instrument/CDPP-AMDA/PSP/LFR</ResourceID>
  6 + <ResourceHeader>
  7 + <ResourceName>FIELDS RFS/LFR</ResourceName>
  8 + <AlternateName>Solar Probe Plus, SPP, FIELDS Suite, Radio Frequency Spectrometer, Low Frequency Receiver, RFS/LFR, Instrument</AlternateName>
  9 + <ReleaseDate>2022-05-11T09:00:00.000Z</ReleaseDate>
  10 + <Description>The Radio Frequency Spectrometer, RFS, is a dual channel digital spectrometer, designed for both remote sensing of radio waves and in situ measurement of electrostatic fluctuations. The RFS receives inputs from the V1, V2, V3, and V4 electric field antennas, using the high frequency output of the FIELDS electric field preamplifiers. Both RFS channels are digitally sampled simultaneously, allowing for calculations of auto spectra for each channel and cross spectra between the two channels. Using multiplexers to select antennas, each RFS channel can use as input either the difference between any two antennas, dipole mode, or the difference between any antenna and spacecraft ground, monopole mode. In addition to the electric field antennas, the single axis medium frequency, MF, winding from the search coil may also used as an input to the RFS. The RFS analog electronics are physically located on an isolated segment of the FIELDS Digital Control Board, DCB. RFS digital signal processing, DSP, is handled by the DCB FPGA and the DCB flight software.
  11 +
  12 +The nominal length of a RFS sample is 32,768 samples. Using an 8 tap PFB, this results in a 4,096 point time series for the fast Fourier transform, FFT, which in turn yields 2048 positive frequencies. The full resolution spectra would be too large to store and telemeter, and so select frequencies are extracted from the full resolution spectra and stored in memory for downlink. Both autocorrelation and cross correlation measurements are produced from the selected bins of the spectra.
  13 +
  14 +The RFS operational frequency range spans from approximately 10 kHz to 19.2 MHz. This frequency range is subdivided into the Low Frequency Range, LFR, from about 10 kHz to 2.4 MHz, and High Frequency Range, HFR, about 1.6 kHz to 19.2 MHz. The primary science of the LFR consists of in situ quasi-thermal noise, QTN, spectrum measurements. The HFR will focus primarily on remote sensing. The LFR sampling cadence is reduced from 38.4 MHz to fs equal to 4.8 MHz, using a Cascade Integrator Comb, CIC, filter to anti-alias and downsample by a factor of eight. Because the frequency resolution of FFT algorithms is equal to fs/N, the lower fs allows for better frequency resolution at the LFR frequencies while using an identical DSP signal chain. For both the LFR and HFR, the chosen frequencies allow for a relative frequency spacing &#916;f/f of approximately 4.5% throughout their respective frequency ranges.</Description>
  15 + <Acknowledgement>Please acknowledge NASA, Stuart D. Bale, the PSP FIELDS Instrument Suite Principal Investigator, and Nicola J. Fox, the PSP Project Scientist.</Acknowledgement>
  16 + <Contact>
  17 + <PersonID>spase://SMWG/Person/Nicola.J.Fox</PersonID>
  18 + <Role>ProjectScientist</Role>
  19 + </Contact>
  20 + <Contact>
  21 + <PersonID>spase://SMWG/Person/Stuart.D.Bale</PersonID>
  22 + <Role>PrincipalInvestigator</Role>
  23 + </Contact>
  24 + <InformationURL>
  25 + <Name>The Solar Probe Plus Radio Frequency Spectrometer: Measurement requirements, analog design, and digital signal processing</Name>
  26 + <URL>https://doi.org/10.1002/2016JA023345</URL>
  27 + <Description>Pulupa, M., et al. (2017), The Solar Probe Plus Radio Frequency Spectrometer: Measurement requirements, analog design, and digital signal processing, J. Geophys. Res. Space Physics, 122, 2836– 2854</Description>
  28 + </InformationURL>
  29 + </ResourceHeader>
  30 + <InstrumentType>SpectralPowerReceiver</InstrumentType>
  31 + <InvestigationName>FIELDS</InvestigationName>
  32 + <OperatingSpan>
  33 + <StartDate>2018-08-12T07:31:00.000Z</StartDate>
  34 + </OperatingSpan>
  35 + <ObservatoryID>spase://CNES/Observatory/CDPP-AMDA/PSP</ObservatoryID>
  36 + </Instrument>
  37 +</Spase>
NumericalData/CDPP-AMDA/PSP/LFR/psp-rfs-sqtn.xml 0 → 100644
  Diff comments   View file @e6385f9
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  1 +<?xml version="1.0" encoding="UTF-8"?>
  2 +<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">
  3 + <Version>2.3.0</Version>
  4 + <NumericalData>
  5 + <ResourceID>spase://CNES/NumericalData/CDPP-AMDA/PSP/LFR/psp-rfs-sqtn</ResourceID>
  6 + <ResourceHeader>
  7 + <ResourceName>L3 - SQTN</ResourceName>
  8 + <AlternateName>Simplified Quasi-Thermal Noise</AlternateName>
  9 + <ReleaseDate>2022-05-11T09:00:00Z</ReleaseDate>
  10 + <Description>These data are derived from power spectra (10.5 kHz to 1.7 MHz) acquired by the low-frequency receiver (LFR) of the Radio Frequency Spectrometer (RFS), part of the FIELDS instrument suite on PSP.
  11 +
  12 +The technique of QTN spectroscopy consists of using the power spectrum of the voltage induced on an electric antenna by the particle quasi-thermal motion, measured by a radio receiver connected to an electric antenna. The signature of the electrons is a line at the electron plasma frequency, which leads to the total electron density (proportionnal to the square of electron plasma frequency), whereas the shape of the line reveals the electron kinetic temperature, as well as its themral (core) and suprathermal components.
  13 +
  14 +For more information on the QTN spectroscopy, please see : Moncuquet, M. et al. (2020), First in-situ measurements electron density and temperature from quasi-thermal noise spectroscopy with Parker Solar Probe/FIELDS, The Astrophysical Journal Supplement Series, Volume 246, p.44, doi:10.3847/1538-4365/ab5a84/
  15 +
  16 +For more information on the FIELDS instruments and datasets, please see: FIELDS Data Center
  17 + </Description>
  18 + <Acknowledgement>In publications, we recommend to add the following sentence in the acknowledgments: 'The authors acknowledge LESIA (Laboratoire d Etudes Spatiales et Instrumentation en Astrophysique), Observatoire de PARIS, CNRS (Centre National de la Recherche Scientifique) and CNES (Centre National d'Etudes Spatiales) for support for production of these data and CDPP (Centre de Donnees de la Physique des Plasmas) for their archiving and provision'.
  19 + </Acknowledgement>
  20 + <Contact>
  21 + <PersonID>spase://CNES/Person/M.Moncuquet</PersonID>
  22 + <Role>DataProducer</Role>
  23 + </Contact>
  24 + <InformationURL>
  25 + <Name>First In Situ Measurements of Electron Density and Temperature from Quasi-thermal Noise Spectroscopy with Parker Solar Probe/FIELDS</Name>
  26 + <URL>https://doi.org/10.3847/1538-4365/ab5a84</URL>
  27 + <Description>Moncuquet, M. et al. (2020), First in-situ measurements electron density and temperature from quasi-thermal noise spectroscopy with Parker Solar Probe/FIELDS, The Astrophysical Journal Supplement Series, Volume 246, p.44, doi:10.3847/1538-4365/ab5a84/
  28 + </Description>
  29 + </InformationURL>
  30 + <InformationURL>
  31 + <Name>CDPP Archive</Name>
  32 + <URL>https://cdpp-archive.cnes.fr</URL>
  33 + <Description>Data archive in CNES</Description>
  34 + </InformationURL>
  35 + </ResourceHeader>
  36 + <AccessInformation>
  37 + <RepositoryID>spase://SMWG/Repository/CNES/CDPP-AMDA</RepositoryID>
  38 + <Availability>Online</Availability>
  39 + <AccessRights>Open</AccessRights>
  40 + <AccessURL>
  41 + <Name>AMDA at CDPP</Name>
  42 + <URL>
  43 + http://amda.cdpp.eu
  44 + </URL>
  45 + </AccessURL>
  46 + <Format>Text</Format>
  47 + <Acknowledgement>
  48 + AMDA is a science analysis system provided by the Centre de Donnees de la
  49 + Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and
  50 + Universite Paul Sabatier, Toulouse
  51 + </Acknowledgement>
  52 + </AccessInformation>
  53 + <ProviderName>CDPP</ProviderName>
  54 + <ProviderResourceName>DA_TC_PARKERSP_FIELDS_RFS_SQTN</ProviderResourceName>
  55 + <InstrumentID>spase://CNES/Instrument/CDPP-AMDA/PSP/LFR</InstrumentID>
  56 + <MeasurementType>ThermalPlasma</MeasurementType>
  57 + <TemporalDescription>
  58 + <TimeSpan>
  59 + <StartDate>2018-10-15T00:00:26Z</StartDate>
  60 + <StopDate>2021-08-19T23:59:48Z</StopDate>
  61 + </TimeSpan>
  62 + <CadenceMin>PT7S</CadenceMin>
  63 + <CadenceMax>PT56S</CadenceMax>
  64 + </TemporalDescription>
  65 + <ObservedRegion>Heliosphere.Inner</ObservedRegion>
  66 + <ObservedRegion>Sun.Corona</ObservedRegion>
  67 + <Parameter>
  68 + <Name>density e-</Name>
  69 + <ParameterKey>psp_sqtn_n</ParameterKey>
  70 + <Description>The electron density is deduced from the automatic detection of the plasma frequency in RFS spectra with SQTN spectroscopy</Description>
  71 + <Ucd>phys.density;phys.electron</Ucd>
  72 + <Units>cm-3</Units>
  73 + <UnitsConversion>1.e-6&gt;m^-3</UnitsConversion>
  74 + <FillValue>-1.0e+31</FillValue>
  75 + <RenderingHints>
  76 + <DisplayType>TimeSeries</DisplayType>
  77 + </RenderingHints>
  78 + <Particle>
  79 + <ParticleType>Electron</ParticleType>
  80 + <ParticleQuantity>NumberDensity</ParticleQuantity>
  81 + </Particle>
  82 + </Parameter>
  83 + <Parameter>
  84 + <Name>density e- : delta</Name>
  85 + <ParameterKey>psp_sqtn_ndelta</ParameterKey>
  86 + <Description>Uncertainty of electron density.</Description>
  87 + <Ucd>phys.density;phys.electron</Ucd>
  88 + <Units>m-3</Units>
  89 + <UnitsConversion>1.e-6&gt;m^-3</UnitsConversion>
  90 + <FillValue>-1.0e+31</FillValue>
  91 + <RenderingHints>
  92 + <DisplayType>TimeSeries</DisplayType>
  93 + </RenderingHints>
  94 + <Structure>
  95 + <Size>2</Size>
  96 + <Element>
  97 + <Name>n_delta_minus</Name>
  98 + <Index>1</Index>
  99 + <ParameterKey>psp_sqtn_ndelta(0)</ParameterKey>
  100 + </Element>
  101 + <Element>
  102 + <Name>n_delta_plus</Name>
  103 + <Index>2</Index>
  104 + <ParameterKey>psp_sqtn_ndelta(1)</ParameterKey>
  105 + </Element>
  106 + </Structure>
  107 + <Support>
  108 + <SupportQuantity>DataQuality</SupportQuantity>
  109 + </Support>
  110 + </Parameter>
  111 + <Parameter>
  112 + <Name>temperature e-</Name>
  113 + <ParameterKey>psp_sqtn_t</ParameterKey>
  114 + <Description>The electron core temperature is deduced from the QTN level below fp in RFS spectra with SQTN spectroscopy</Description>
  115 + <Ucd>phys.temperature;phys.electron</Ucd>
  116 + <Units>eV</Units>
  117 + <FillValue>-1.0e+31</FillValue>
  118 + <RenderingHints>
  119 + <DisplayType>TimeSeries</DisplayType>
  120 + </RenderingHints>
  121 + <Particle>
  122 + <ParticleType>Electron</ParticleType>
  123 + <ParticleQuantity>Temperature</ParticleQuantity>
  124 + </Particle>
  125 + </Parameter>
  126 +</NumericalData>
  127 +</Spase>