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NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-pot-full.xml
| ... | ... | @@ -5,14 +5,29 @@ |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-pot-full</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | 7 | <ResourceName>0.2 sec (full)</ResourceName> |
| 8 | - <AlternateName>Cluster 1 Prime Parameter EFW Data</AlternateName> | |
| 9 | - <ReleaseDate>2015-10-16T11:32:44Z</ReleaseDate> | |
| 10 | - <Description>The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440-29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1-700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1-100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1-100/cm. There is also a frequency counter covering the range 10-200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Spherical Probe Electric Field and Waves experiment for the Cluster Mission, by G. Gustafsson et al., from which this information was obtained.</Description> | |
| 11 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 8 | + <AlternateName>Cluster 1 Spacecraft Potential (L2)</AlternateName> | |
| 9 | + <ReleaseDate>2016-10-16T11:32:44Z</ReleaseDate> | |
| 10 | + <Description>L2 Spacecraft potential (0.2 sec) | |
| 11 | + is normally the average potential of all available probes, measured relative to | |
| 12 | + the spacecraft. If all four probes are available, the average is done over all 4 probes. If only two | |
| 13 | + or three probes are available, the average is done over 2 opposing probes ( P1 and | |
| 14 | + P, or P3 and P4). If only two non-opposing probes are available (e.g. P2 and P3), this quantity is the | |
| 15 | + value of one of the probes. If only one probe is available, this quantity is the value of that | |
| 16 | + probe. The probes used are given by the parameter P_probes. When moderate high-bias | |
| 17 | + saturation is detected on one of the probes (indicated by bit 14 in the P_bitmask), the average | |
| 18 | + over 4 seconds is replaced by a maximum over 4 seconds to avoid errors resulting from the | |
| 19 | + resulting spikes; also the data quality is lowered for such intervals. The | |
| 20 | + individual probe potentials are available in the ancillary data</Description> | |
| 21 | + <Acknowledgement>PrincipalInvestigator: Prof. Mats Andre</Acknowledgement> | |
| 12 | 22 | <Contact> |
| 13 | - <PersonID>spase://SMWG/Person/Elena.Budnik</PersonID> | |
| 14 | - <Role>TechnicalContact</Role> | |
| 15 | - </Contact> | |
| 23 | + <PersonID>spase://SMWG/Person/Mats.Andre</PersonID> | |
| 24 | + <Role>PrincipalInvestigator</Role> | |
| 25 | + </Contact> | |
| 26 | + <InformationURL> | |
| 27 | + <Name>ESA web page</Name> | |
| 28 | + <URL>http://www.cosmos.esa.int/web/csa/documentation</URL> | |
| 29 | + <Description>This site contains EFW documentation</Description> | |
| 30 | + </InformationURL> | |
| 16 | 31 | <InformationURL> |
| 17 | 32 | <Name>NSSDC Master Catalog listing for Cluster II Rumba Electric Field and Waves (EFW)</Name> |
| 18 | 33 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| ... | ... | @@ -33,11 +48,10 @@ |
| 33 | 48 | <URL>http://amda.cdpp.eu</URL> |
| 34 | 49 | </AccessURL> |
| 35 | 50 | <Format>NetCDF</Format> |
| 36 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 37 | 51 | </AccessInformation> |
| 38 | 52 | <ProviderName>CSA</ProviderName> |
| 39 | 53 | <ProcessingLevel>Calibrated</ProcessingLevel> |
| 40 | - <ProviderResourceName>Cluster II Rumba Prime Parameter Electric Field and Waves (EFW) Data</ProviderResourceName> | |
| 54 | + <ProviderResourceName>C1_CP_EFW_L2_P</ProviderResourceName> | |
| 41 | 55 | <ProviderProcessingLevel>Calibrated</ProviderProcessingLevel> |
| 42 | 56 | <InstrumentID>spase://CDPP/Instrument/AMDA/Cluster-Rumba/EFW</InstrumentID> |
| 43 | 57 | <MeasurementType>ElectricField</MeasurementType> |
| ... | ... | @@ -75,7 +89,7 @@ |
| 75 | 89 | <Name>s/c pot</Name> |
| 76 | 90 | <ParameterKey>c1_potfull</ParameterKey> |
| 77 | 91 | <Description> |
| 78 | - Cluster II Rumba Prime Parameter Electric Field and Waves probe potential at spin time resolution | |
| 92 | + Probe potential, Relative to Spacecraft at full resolution (0.2s) | |
| 79 | 93 | </Description> |
| 80 | 94 | <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> |
| 81 | 95 | <Cadence>PT0.2S</Cadence> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-pot-spin.xml
| ... | ... | @@ -5,15 +5,31 @@ |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster1/EFW/clust1-pot-spin</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | 7 | <ResourceName>4 sec (spin)</ResourceName> |
| 8 | - <AlternateName>Cluster 1 Prime Parameter EFW Data</AlternateName> | |
| 9 | - <ReleaseDate>2015-10-16T11:41:44Z</ReleaseDate> | |
| 10 | - <Description>The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440-29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1-700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1-100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1-100/cm. There is also a frequency counter covering the range 10-200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Spherical Probe Electric Field and Waves experiment for the Cluster Mission, by G. Gustafsson et al., from which this information was obtained.</Description> | |
| 11 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 8 | + <AlternateName>Cluster 1 Spacecraft Potential (L3)</AlternateName> | |
| 9 | + <ReleaseDate>2016-10-16T11:41:44Z</ReleaseDate> | |
| 10 | + <Description> | |
| 11 | + L3 Spacecraft potential (4 sec resolution) | |
| 12 | + is normally the average potential of all available probes, measured relative to | |
| 13 | + the spacecraft. If all four probes are available, the average is done over all 4 probes. If only two | |
| 14 | + or three probes are available, the average is done over 2 opposing probes ( P1 and | |
| 15 | + P, or P3 and P4). If only two non-opposing probes are available (e.g. P2 and P3), this quantity is the | |
| 16 | + value of one of the probes. If only one probe is available, this quantity is the value of that | |
| 17 | + probe. The probes used are given by the parameter P_probes. When moderate high-bias | |
| 18 | + saturation is detected on one of the probes (indicated by bit 14 in the P_bitmask), the average | |
| 19 | + over 4 seconds is replaced by a maximum over 4 seconds to avoid errors resulting from the | |
| 20 | + resulting spikes; also the data quality is lowered for such intervals. The | |
| 21 | + individual probe potentials are available in the ancillary data</Description> | |
| 22 | + <Acknowledgement>PrincipalInvestigator: Prof. Mats Andre</Acknowledgement> | |
| 12 | 23 | <Contact> |
| 13 | - <PersonID>spase://SMWG/Person/Elena.Budnik</PersonID> | |
| 14 | - <Role>TechnicalContact</Role> | |
| 24 | + <PersonID>spase://SMWG/Person/Mats.Andre</PersonID> | |
| 25 | + <Role>PrincipalInvestigator</Role> | |
| 15 | 26 | </Contact> |
| 16 | 27 | <InformationURL> |
| 28 | + <Name>ESA web page</Name> | |
| 29 | + <URL>http://www.cosmos.esa.int/web/csa/documentation</URL> | |
| 30 | + <Description>This site contains EFW documentation</Description> | |
| 31 | + </InformationURL> | |
| 32 | + <InformationURL> | |
| 17 | 33 | <Name>NSSDC Master Catalog listing for Cluster II Rumba Electric Field and Waves (EFW)</Name> |
| 18 | 34 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| 19 | 35 | <Description>This site provides information concerning the Cluster II Rumba Electric Field and Waves Instrument.</Description> |
| ... | ... | @@ -32,12 +48,11 @@ |
| 32 | 48 | <Name>AMDA at CDPP</Name> |
| 33 | 49 | <URL>http://amda.cdpp.eu</URL> |
| 34 | 50 | </AccessURL> |
| 35 | - <Format>NetCDF</Format> | |
| 36 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 51 | + <Format>NetCDF</Format> | |
| 37 | 52 | </AccessInformation> |
| 38 | 53 | <ProviderName>CSA</ProviderName> |
| 39 | 54 | <ProcessingLevel>Calibrated</ProcessingLevel> |
| 40 | - <ProviderResourceName>Cluster II Rumba Prime Parameter Electric Field and Waves (EFW) Data</ProviderResourceName> | |
| 55 | + <ProviderResourceName>C1_CP_EFW_L3_P</ProviderResourceName> | |
| 41 | 56 | <ProviderProcessingLevel>Calibrated</ProviderProcessingLevel> |
| 42 | 57 | <InstrumentID>spase://CDPP/Instrument/AMDA/Cluster-Rumba/EFW</InstrumentID> |
| 43 | 58 | <MeasurementType>ElectricField</MeasurementType> |
| ... | ... | @@ -75,10 +90,10 @@ |
| 75 | 90 | <Name>s/c pot</Name> |
| 76 | 91 | <ParameterKey>c1_potspin</ParameterKey> |
| 77 | 92 | <Description> |
| 78 | - Cluster II Rumba Prime Parameter Electric Field and Waves probe potential at spin time resolution | |
| 93 | + Probe potential, Relative to Spacecraft at spin time resolution (4s) | |
| 79 | 94 | </Description> |
| 80 | 95 | <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> |
| 81 | - <Cadence>PT5S</Cadence> | |
| 96 | + <Cadence>PT4S</Cadence> | |
| 82 | 97 | <Units>V</Units> |
| 83 | 98 | <UnitsConversion>1.0>V</UnitsConversion> |
| 84 | 99 | <RenderingHints> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster2/EFW/clust2-pot-full.xml
| ... | ... | @@ -5,14 +5,29 @@ |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster2/EFW/clust2-pot-full</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | 7 | <ResourceName>0.2 sec (full)</ResourceName> |
| 8 | - <AlternateName>Cluster 2 Prime Parameter EFW Data</AlternateName> | |
| 9 | - <ReleaseDate>2015-10-19T15:51:44Z</ReleaseDate> | |
| 10 | - <Description>The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440-29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1-700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1-100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1-100/cm. There is also a frequency counter covering the range 10-200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Spherical Probe Electric Field and Waves experiment for the Cluster Mission, by G. Gustafsson et al., from which this information was obtained.</Description> | |
| 11 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 8 | + <AlternateName>Cluster 2 Spacecraft Potential (L2)</AlternateName> | |
| 9 | + <ReleaseDate>2016-10-16T11:32:44Z</ReleaseDate> | |
| 10 | + <Description>L2 Spacecraft potential (0.2 sec) | |
| 11 | + is normally the average potential of all available probes, measured relative to | |
| 12 | + the spacecraft. If all four probes are available, the average is done over all 4 probes. If only two | |
| 13 | + or three probes are available, the average is done over 2 opposing probes ( P1 and | |
| 14 | + P, or P3 and P4). If only two non-opposing probes are available (e.g. P2 and P3), this quantity is the | |
| 15 | + value of one of the probes. If only one probe is available, this quantity is the value of that | |
| 16 | + probe. The probes used are given by the parameter P_probes. When moderate high-bias | |
| 17 | + saturation is detected on one of the probes (indicated by bit 14 in the P_bitmask), the average | |
| 18 | + over 4 seconds is replaced by a maximum over 4 seconds to avoid errors resulting from the | |
| 19 | + resulting spikes; also the data quality is lowered for such intervals. The | |
| 20 | + individual probe potentials are available in the ancillary data</Description> | |
| 21 | + <Acknowledgement>PrincipalInvestigator: Prof. Mats Andre</Acknowledgement> | |
| 12 | 22 | <Contact> |
| 13 | - <PersonID>spase://SMWG/Person/Elena.Budnik</PersonID> | |
| 14 | - <Role>TechnicalContact</Role> | |
| 15 | - </Contact> | |
| 23 | + <PersonID>spase://SMWG/Person/Mats.Andre</PersonID> | |
| 24 | + <Role>PrincipalInvestigator</Role> | |
| 25 | + </Contact> | |
| 26 | + <InformationURL> | |
| 27 | + <Name>ESA web page</Name> | |
| 28 | + <URL>http://www.cosmos.esa.int/web/csa/documentation</URL> | |
| 29 | + <Description>This site contains EFW documentation</Description> | |
| 30 | + </InformationURL> | |
| 16 | 31 | <InformationURL> |
| 17 | 32 | <Name>NSSDC Master Catalog listing for Cluster II Salsa Electric Field and Waves (EFW)</Name> |
| 18 | 33 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| ... | ... | @@ -22,7 +37,7 @@ |
| 22 | 37 | <AssociationID>c2-efw-pot</AssociationID> |
| 23 | 38 | <AssociationType>PartOf</AssociationType> |
| 24 | 39 | <Note>s/c potential</Note> |
| 25 | - </Association> | |
| 40 | + </Association> | |
| 26 | 41 | </ResourceHeader> |
| 27 | 42 | <AccessInformation> |
| 28 | 43 | <RepositoryID>spase://SMWG/Repository/CDPP/AMDA</RepositoryID> |
| ... | ... | @@ -33,11 +48,10 @@ |
| 33 | 48 | <URL>http://amda.cdpp.eu</URL> |
| 34 | 49 | </AccessURL> |
| 35 | 50 | <Format>NetCDF</Format> |
| 36 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 37 | 51 | </AccessInformation> |
| 38 | 52 | <ProviderName>CSA</ProviderName> |
| 39 | 53 | <ProcessingLevel>Calibrated</ProcessingLevel> |
| 40 | - <ProviderResourceName>Cluster II Salsa Prime Parameter Electric Field and Waves (EFW) Data</ProviderResourceName> | |
| 54 | + <ProviderResourceName>C2_CP_EFW_L2_P</ProviderResourceName> | |
| 41 | 55 | <ProviderProcessingLevel>Calibrated</ProviderProcessingLevel> |
| 42 | 56 | <InstrumentID>spase://CDPP/Instrument/AMDA/Cluster-Salsa/EFW</InstrumentID> |
| 43 | 57 | <MeasurementType>ElectricField</MeasurementType> |
| ... | ... | @@ -75,7 +89,7 @@ |
| 75 | 89 | <Name>s/c pot</Name> |
| 76 | 90 | <ParameterKey>c2_potfull</ParameterKey> |
| 77 | 91 | <Description> |
| 78 | - Cluster II Salsa Prime Parameter Electric Field and Waves probe potential at spin time resolution | |
| 92 | + Probe potential, Relative to Spacecraft at full resolution (0.2s) | |
| 79 | 93 | </Description> |
| 80 | 94 | <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> |
| 81 | 95 | <Cadence>PT0.2S</Cadence> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster2/EFW/clust2-pot-spin.xml
| ... | ... | @@ -4,16 +4,32 @@ |
| 4 | 4 | <NumericalData> |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster2/EFW/clust2-pot-spin</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | - <ResourceName> 4 sec (spin)</ResourceName> | |
| 8 | - <AlternateName>Cluster 2 Prime Parameter EFW Data</AlternateName> | |
| 9 | - <ReleaseDate>2015-10-19T15:51:44Z</ReleaseDate> | |
| 10 | - <Description>The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440-29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1-700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1-100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1-100/cm. There is also a frequency counter covering the range 10-200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Spherical Probe Electric Field and Waves experiment for the Cluster Mission, by G. Gustafsson et al., from which this information was obtained.</Description> | |
| 11 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 7 | + <ResourceName>4 sec (spin)</ResourceName> | |
| 8 | + <AlternateName>Cluster 2 Spacecraft Potential (L3)</AlternateName> | |
| 9 | + <ReleaseDate>2016-10-16T11:41:44Z</ReleaseDate> | |
| 10 | + <Description> | |
| 11 | + L3 Spacecraft potential (4 sec resolution) | |
| 12 | + is normally the average potential of all available probes, measured relative to | |
| 13 | + the spacecraft. If all four probes are available, the average is done over all 4 probes. If only two | |
| 14 | + or three probes are available, the average is done over 2 opposing probes ( P1 and | |
| 15 | + P, or P3 and P4). If only two non-opposing probes are available (e.g. P2 and P3), this quantity is the | |
| 16 | + value of one of the probes. If only one probe is available, this quantity is the value of that | |
| 17 | + probe. The probes used are given by the parameter P_probes. When moderate high-bias | |
| 18 | + saturation is detected on one of the probes (indicated by bit 14 in the P_bitmask), the average | |
| 19 | + over 4 seconds is replaced by a maximum over 4 seconds to avoid errors resulting from the | |
| 20 | + resulting spikes; also the data quality is lowered for such intervals. The | |
| 21 | + individual probe potentials are available in the ancillary data</Description> | |
| 22 | + <Acknowledgement>PrincipalInvestigator: Prof. Mats Andre</Acknowledgement> | |
| 12 | 23 | <Contact> |
| 13 | - <PersonID>spase://SMWG/Person/Elena.Budnik</PersonID> | |
| 14 | - <Role>TechnicalContact</Role> | |
| 24 | + <PersonID>spase://SMWG/Person/Mats.Andre</PersonID> | |
| 25 | + <Role>PrincipalInvestigator</Role> | |
| 15 | 26 | </Contact> |
| 16 | 27 | <InformationURL> |
| 28 | + <Name>ESA web page</Name> | |
| 29 | + <URL>http://www.cosmos.esa.int/web/csa/documentation</URL> | |
| 30 | + <Description>This site contains EFW documentation</Description> | |
| 31 | + </InformationURL> | |
| 32 | + <InformationURL> | |
| 17 | 33 | <Name>NSSDC Master Catalog listing for Cluster II Salsa Electric Field and Waves (EFW)</Name> |
| 18 | 34 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| 19 | 35 | <Description>This site provides information concerning the Cluster II Salsa Electric Field and Waves Instrument.</Description> |
| ... | ... | @@ -32,12 +48,11 @@ |
| 32 | 48 | <Name>AMDA at CDPP</Name> |
| 33 | 49 | <URL>http://amda.cdpp.eu</URL> |
| 34 | 50 | </AccessURL> |
| 35 | - <Format>NetCDF</Format> | |
| 36 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 51 | + <Format>NetCDF</Format> | |
| 37 | 52 | </AccessInformation> |
| 38 | 53 | <ProviderName>CSA</ProviderName> |
| 39 | 54 | <ProcessingLevel>Calibrated</ProcessingLevel> |
| 40 | - <ProviderResourceName>Cluster II Salsa Prime Parameter Electric Field and Waves (EFW) Data</ProviderResourceName> | |
| 55 | + <ProviderResourceName>C2_CP_EFW_L3_P</ProviderResourceName> | |
| 41 | 56 | <ProviderProcessingLevel>Calibrated</ProviderProcessingLevel> |
| 42 | 57 | <InstrumentID>spase://CDPP/Instrument/AMDA/Cluster-Salsa/EFW</InstrumentID> |
| 43 | 58 | <MeasurementType>ElectricField</MeasurementType> |
| ... | ... | @@ -75,10 +90,10 @@ |
| 75 | 90 | <Name>s/c pot</Name> |
| 76 | 91 | <ParameterKey>c2_potspin</ParameterKey> |
| 77 | 92 | <Description> |
| 78 | - Cluster II Salsa Prime Parameter Electric Field and Waves probe potential at spin time resolution | |
| 93 | + Probe potential, Relative to Spacecraft at spin time resolution (4s) | |
| 79 | 94 | </Description> |
| 80 | 95 | <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> |
| 81 | - <Cadence>PT5S</Cadence> | |
| 96 | + <Cadence>PT4S</Cadence> | |
| 82 | 97 | <Units>V</Units> |
| 83 | 98 | <UnitsConversion>1.0>V</UnitsConversion> |
| 84 | 99 | <RenderingHints> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster3/EFW/clust3-efw-sr2.xml
| ... | ... | @@ -12,6 +12,13 @@ |
| 12 | 12 | The EFW instrument measures the electric field only in the spacecraft |
| 13 | 13 | spin plane, therefore a spin-plane oriented coordinate system is best suited for scientific studies involving the electric field. The ISR2 (Inverted Spin Reference) system, also known as DSI (Despun System Inverted), is such a system. The X and Y axes are in the spin plane, with X pointing as near sunward as possible and Y perpendicular to the sunward direction, positive towards dusk. The Z-axis is along the (negative) spacecraft spin axis, towards the north ecliptic. The coordinate system is called Inverted because the actual spin axis of Cluster is pointing towards the south ecliptic. The difference between ISR2 (DSI) and the GSE (Geocentric Solar Ecliptic) is a tilt of 2ยฐ to 7ยฐ of the Z-axis performed in order |
| 14 | 14 | to avoid shading of the EFW probes by the spacecraft. |
| 15 | + Note | |
| 16 | + : The ISR2 and GSE systems differ substantially on C3 during the May 2008 | |
| 17 | + tilt campaign (between 09:00 UT on 2008-04-25 and 08:24 UT on 2008-05-30), | |
| 18 | + when the spin axis of C3 was deliberately tilted by up to 45 degrees about the x | |
| 19 | + axis. | |
| 20 | + | |
| 21 | + | |
| 15 | 22 | Data quality description : |
| 16 | 23 | * 4 : Excellent data which have received special treatment |
| 17 | 24 | * 3 : Good for publication, subject to PI approval |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster3/EFW/clust3-pot-full.xml
| ... | ... | @@ -5,14 +5,29 @@ |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster3/EFW/clust3-pot-full</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | 7 | <ResourceName>0.2 sec (full)</ResourceName> |
| 8 | - <AlternateName>Cluster 3 Prime Parameter EFW Data</AlternateName> | |
| 9 | - <ReleaseDate>2015-10-19T15:51:44Z</ReleaseDate> | |
| 10 | - <Description>The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440-29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1-700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1-100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1-100/cm. There is also a frequency counter covering the range 10-200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Spherical Probe Electric Field and Waves experiment for the Cluster Mission, by G. Gustafsson et al., from which this information was obtained.</Description> | |
| 11 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 8 | + <AlternateName>Cluster 3 Spacecraft Potential (L2)</AlternateName> | |
| 9 | + <ReleaseDate>2016-10-16T11:32:44Z</ReleaseDate> | |
| 10 | + <Description>L2 Spacecraft potential (0.2 sec) | |
| 11 | + is normally the average potential of all available probes, measured relative to | |
| 12 | + the spacecraft. If all four probes are available, the average is done over all 4 probes. If only two | |
| 13 | + or three probes are available, the average is done over 2 opposing probes ( P1 and | |
| 14 | + P, or P3 and P4). If only two non-opposing probes are available (e.g. P2 and P3), this quantity is the | |
| 15 | + value of one of the probes. If only one probe is available, this quantity is the value of that | |
| 16 | + probe. The probes used are given by the parameter P_probes. When moderate high-bias | |
| 17 | + saturation is detected on one of the probes (indicated by bit 14 in the P_bitmask), the average | |
| 18 | + over 4 seconds is replaced by a maximum over 4 seconds to avoid errors resulting from the | |
| 19 | + resulting spikes; also the data quality is lowered for such intervals. The | |
| 20 | + individual probe potentials are available in the ancillary data</Description> | |
| 21 | + <Acknowledgement>PrincipalInvestigator: Prof. Mats Andre</Acknowledgement> | |
| 12 | 22 | <Contact> |
| 13 | - <PersonID>spase://SMWG/Person/Elena.Budnik</PersonID> | |
| 14 | - <Role>TechnicalContact</Role> | |
| 15 | - </Contact> | |
| 23 | + <PersonID>spase://SMWG/Person/Mats.Andre</PersonID> | |
| 24 | + <Role>PrincipalInvestigator</Role> | |
| 25 | + </Contact> | |
| 26 | + <InformationURL> | |
| 27 | + <Name>ESA web page</Name> | |
| 28 | + <URL>http://www.cosmos.esa.int/web/csa/documentation</URL> | |
| 29 | + <Description>This site contains EFW documentation</Description> | |
| 30 | + </InformationURL> | |
| 16 | 31 | <InformationURL> |
| 17 | 32 | <Name>NSSDC Master Catalog listing for Cluster II Samba Electric Field and Waves (EFW)</Name> |
| 18 | 33 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| ... | ... | @@ -33,11 +48,10 @@ |
| 33 | 48 | <URL>http://amda.cdpp.eu</URL> |
| 34 | 49 | </AccessURL> |
| 35 | 50 | <Format>NetCDF</Format> |
| 36 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 37 | 51 | </AccessInformation> |
| 38 | 52 | <ProviderName>CSA</ProviderName> |
| 39 | 53 | <ProcessingLevel>Calibrated</ProcessingLevel> |
| 40 | - <ProviderResourceName>Cluster II Samba Prime Parameter Electric Field and Waves (EFW) Data</ProviderResourceName> | |
| 54 | + <ProviderResourceName>C3_CP_EFW_L2_P</ProviderResourceName> | |
| 41 | 55 | <ProviderProcessingLevel>Calibrated</ProviderProcessingLevel> |
| 42 | 56 | <InstrumentID>spase://CDPP/Instrument/AMDA/Cluster-Samba/EFW</InstrumentID> |
| 43 | 57 | <MeasurementType>ElectricField</MeasurementType> |
| ... | ... | @@ -75,7 +89,7 @@ |
| 75 | 89 | <Name>s/c pot</Name> |
| 76 | 90 | <ParameterKey>c3_potfull</ParameterKey> |
| 77 | 91 | <Description> |
| 78 | - Cluster II Samba Prime Parameter Electric Field and Waves probe potential at spin time resolution | |
| 92 | + Probe potential, Relative to Spacecraft at full resolution (0.2s) | |
| 79 | 93 | </Description> |
| 80 | 94 | <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> |
| 81 | 95 | <Cadence>PT0.2S</Cadence> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster3/EFW/clust3-pot-spin.xml
| ... | ... | @@ -5,15 +5,31 @@ |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster3/EFW/clust3-pot-spin</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | 7 | <ResourceName>4 sec (spin)</ResourceName> |
| 8 | - <AlternateName>Cluster 3 Prime Parameter EFW Data</AlternateName> | |
| 9 | - <ReleaseDate>2015-10-19T15:51:44Z</ReleaseDate> | |
| 10 | - <Description>The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440-29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1-700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1-100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1-100/cm. There is also a frequency counter covering the range 10-200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Spherical Probe Electric Field and Waves experiment for the Cluster Mission, by G. Gustafsson et al., from which this information was obtained.</Description> | |
| 11 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 8 | + <AlternateName>Cluster 3 Spacecraft Potential (L3)</AlternateName> | |
| 9 | + <ReleaseDate>2016-10-16T11:41:44Z</ReleaseDate> | |
| 10 | + <Description> | |
| 11 | + L3 Spacecraft potential (4 sec resolution) | |
| 12 | + is normally the average potential of all available probes, measured relative to | |
| 13 | + the spacecraft. If all four probes are available, the average is done over all 4 probes. If only two | |
| 14 | + or three probes are available, the average is done over 2 opposing probes ( P1 and | |
| 15 | + P, or P3 and P4). If only two non-opposing probes are available (e.g. P2 and P3), this quantity is the | |
| 16 | + value of one of the probes. If only one probe is available, this quantity is the value of that | |
| 17 | + probe. The probes used are given by the parameter P_probes. When moderate high-bias | |
| 18 | + saturation is detected on one of the probes (indicated by bit 14 in the P_bitmask), the average | |
| 19 | + over 4 seconds is replaced by a maximum over 4 seconds to avoid errors resulting from the | |
| 20 | + resulting spikes; also the data quality is lowered for such intervals. The | |
| 21 | + individual probe potentials are available in the ancillary data</Description> | |
| 22 | + <Acknowledgement>PrincipalInvestigator: Prof. Mats Andre</Acknowledgement> | |
| 12 | 23 | <Contact> |
| 13 | - <PersonID>spase://SMWG/Person/Elena.Budnik</PersonID> | |
| 14 | - <Role>TechnicalContact</Role> | |
| 24 | + <PersonID>spase://SMWG/Person/Mats.Andre</PersonID> | |
| 25 | + <Role>PrincipalInvestigator</Role> | |
| 15 | 26 | </Contact> |
| 16 | 27 | <InformationURL> |
| 28 | + <Name>ESA web page</Name> | |
| 29 | + <URL>http://www.cosmos.esa.int/web/csa/documentation</URL> | |
| 30 | + <Description>This site contains EFW documentation</Description> | |
| 31 | + </InformationURL> | |
| 32 | + <InformationURL> | |
| 17 | 33 | <Name>NSSDC Master Catalog listing for Cluster II Samba Electric Field and Waves (EFW)</Name> |
| 18 | 34 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| 19 | 35 | <Description>This site provides information concerning the Cluster II Samba Electric Field and Waves Instrument.</Description> |
| ... | ... | @@ -32,12 +48,11 @@ |
| 32 | 48 | <Name>AMDA at CDPP</Name> |
| 33 | 49 | <URL>http://amda.cdpp.eu</URL> |
| 34 | 50 | </AccessURL> |
| 35 | - <Format>NetCDF</Format> | |
| 36 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 51 | + <Format>NetCDF</Format> | |
| 37 | 52 | </AccessInformation> |
| 38 | 53 | <ProviderName>CSA</ProviderName> |
| 39 | 54 | <ProcessingLevel>Calibrated</ProcessingLevel> |
| 40 | - <ProviderResourceName>Cluster II Samba Prime Parameter Electric Field and Waves (EFW) Data</ProviderResourceName> | |
| 55 | + <ProviderResourceName>C3_CP_EFW_L3_P</ProviderResourceName> | |
| 41 | 56 | <ProviderProcessingLevel>Calibrated</ProviderProcessingLevel> |
| 42 | 57 | <InstrumentID>spase://CDPP/Instrument/AMDA/Cluster-Samba/EFW</InstrumentID> |
| 43 | 58 | <MeasurementType>ElectricField</MeasurementType> |
| ... | ... | @@ -75,7 +90,7 @@ |
| 75 | 90 | <Name>s/c pot</Name> |
| 76 | 91 | <ParameterKey>c3_potspin</ParameterKey> |
| 77 | 92 | <Description> |
| 78 | - Cluster II Samba Prime Parameter Electric Field and Waves probe potential at spin time resolution | |
| 93 | + Probe potential, Relative to Spacecraft at spin time resolution (4s) | |
| 79 | 94 | </Description> |
| 80 | 95 | <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> |
| 81 | 96 | <Cadence>PT5S</Cadence> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster4/EFW/clust4-pot-full.xml
| ... | ... | @@ -5,14 +5,29 @@ |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster4/EFW/clust4-pot-full</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | 7 | <ResourceName>0.2 sec (full)</ResourceName> |
| 8 | - <AlternateName>Cluster 4 Prime Parameter EFW Data</AlternateName> | |
| 9 | - <ReleaseDate>2015-10-16T16:51:44Z</ReleaseDate> | |
| 10 | - <Description>The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440-29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1-700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1-100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1-100/cm. There is also a frequency counter covering the range 10-200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Spherical Probe Electric Field and Waves experiment for the Cluster Mission, by G. Gustafsson et al., from which this information was obtained.</Description> | |
| 11 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 8 | + <AlternateName>Cluster 4 Spacecraft Potential (L2)</AlternateName> | |
| 9 | + <ReleaseDate>2016-10-16T11:32:44Z</ReleaseDate> | |
| 10 | + <Description>L2 Spacecraft potential (0.2 sec) | |
| 11 | + is normally the average potential of all available probes, measured relative to | |
| 12 | + the spacecraft. If all four probes are available, the average is done over all 4 probes. If only two | |
| 13 | + or three probes are available, the average is done over 2 opposing probes ( P1 and | |
| 14 | + P, or P3 and P4). If only two non-opposing probes are available (e.g. P2 and P3), this quantity is the | |
| 15 | + value of one of the probes. If only one probe is available, this quantity is the value of that | |
| 16 | + probe. The probes used are given by the parameter P_probes. When moderate high-bias | |
| 17 | + saturation is detected on one of the probes (indicated by bit 14 in the P_bitmask), the average | |
| 18 | + over 4 seconds is replaced by a maximum over 4 seconds to avoid errors resulting from the | |
| 19 | + resulting spikes; also the data quality is lowered for such intervals. The | |
| 20 | + individual probe potentials are available in the ancillary data</Description> | |
| 21 | + <Acknowledgement>PrincipalInvestigator: Prof. Mats Andre</Acknowledgement> | |
| 12 | 22 | <Contact> |
| 13 | - <PersonID>spase://SMWG/Person/Elena.Budnik</PersonID> | |
| 14 | - <Role>TechnicalContact</Role> | |
| 15 | - </Contact> | |
| 23 | + <PersonID>spase://SMWG/Person/Mats.Andre</PersonID> | |
| 24 | + <Role>PrincipalInvestigator</Role> | |
| 25 | + </Contact> | |
| 26 | + <InformationURL> | |
| 27 | + <Name>ESA web page</Name> | |
| 28 | + <URL>http://www.cosmos.esa.int/web/csa/documentation</URL> | |
| 29 | + <Description>This site contains EFW documentation</Description> | |
| 30 | + </InformationURL> | |
| 16 | 31 | <InformationURL> |
| 17 | 32 | <Name>NSSDC Master Catalog listing for Cluster II Tango Electric Field and Waves (EFW)</Name> |
| 18 | 33 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| ... | ... | @@ -33,11 +48,10 @@ |
| 33 | 48 | <URL>http://amda.cdpp.eu</URL> |
| 34 | 49 | </AccessURL> |
| 35 | 50 | <Format>NetCDF</Format> |
| 36 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 37 | 51 | </AccessInformation> |
| 38 | 52 | <ProviderName>CSA</ProviderName> |
| 39 | 53 | <ProcessingLevel>Calibrated</ProcessingLevel> |
| 40 | - <ProviderResourceName>Cluster II Tango Prime Parameter Electric Field and Waves (EFW) Data</ProviderResourceName> | |
| 54 | + <ProviderResourceName>C4_CP_EFW_L2_P</ProviderResourceName> | |
| 41 | 55 | <ProviderProcessingLevel>Calibrated</ProviderProcessingLevel> |
| 42 | 56 | <InstrumentID>spase://CDPP/Instrument/AMDA/Cluster-Tango/EFW</InstrumentID> |
| 43 | 57 | <MeasurementType>ElectricField</MeasurementType> |
| ... | ... | @@ -75,9 +89,9 @@ |
| 75 | 89 | <Name>s/c pot</Name> |
| 76 | 90 | <ParameterKey>c4_potfull</ParameterKey> |
| 77 | 91 | <Description> |
| 78 | - Cluster II Tango Prime Parameter Electric Field and Waves probe potential at spin time resolution | |
| 92 | + Probe potential, Relative to Spacecraft at full resolution (0.2s) | |
| 79 | 93 | </Description> |
| 80 | - <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> | |
| 94 | + <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> | |
| 81 | 95 | <Cadence>PT0.2S</Cadence> |
| 82 | 96 | <Units>V</Units> |
| 83 | 97 | <UnitsConversion>1.0>V</UnitsConversion> |
| ... | ... |
NumericalData/AMDA/Cluster/Cluster4/EFW/clust4-pot-spin.xml
| ... | ... | @@ -5,18 +5,34 @@ |
| 5 | 5 | <ResourceID>spase://CDPP/NumericalData/AMDA/Cluster/Cluster4/EFW/clust4-pot-spin</ResourceID> |
| 6 | 6 | <ResourceHeader> |
| 7 | 7 | <ResourceName>4 sec (spin)</ResourceName> |
| 8 | - <AlternateName>Cluster 4 Prime Parameter EFW Data</AlternateName> | |
| 9 | - <ReleaseDate>2015-10-16T16:51:44Z</ReleaseDate> | |
| 10 | - <Description>The EFW (Electric Field and Waves) instrument consists of four orthogonal spherical sensors deployed from 50 m cable booms in the spin plane of the spacecraft, plus four deployment units and a main electronics unit. Each deployment unit deploys a multiconductor cable and tip-mounted spherical sensor. Each opposing pair of cables will be symmetrically deployed to a tip-to-tip distance of approximately 100 m, except for about a week at the beginning of the mission when 70 m will be used for one boom pair (the Z-booms) and 100 m for the other pair. The potentials of the spherical sensor and nearby conductors are controlled by the microprocessor to minimize errors associated with photoelectron fluxes to and from the spheres. Output signals from the sensor preamplifiers are provided to the wave instruments for analysis of high frequency wave phenomena. There is a 1 MB burst memory and tow fast A/D conversion circuits for recording electric field wave forms for time resolutions of up to 36,000 samples/s. Data gathered in the burst memory will be played back through the telemetry stream allocated to the instrument by pre-empting a portion of the real-time data. Incoming data are continuously monitored by algorithms in the software to determine whether to trigger the burst-playback mode. A large number of sampling modes is possible, yielding four possible telemetry rates from 1.440-29.440 Kbps. This data stream is transferred via the DWP instrument. The main measured quantities will be, in various modes: (1) the instantaneous spin-plane components of the electric field vector, from 0.1-700 V/Km, with time resolution down to 0.1 ms, in four frequency ranges from DC to upper limits of 10 Hz, 180 Hz, 4 KHz, or 32 KHz; (2) the AC electric field components from 10 Hz to 8 KHz, within the dynamic range of ~3 mV/Km to 10 V/Km; (3) plasma density fluctuations within the range of 1-100/cm and in three frequency ranges from 0 Hz to upper limits of 10 Hz, 180 Hz, or 4 KHz; and, (4) density and temperature (in Langmuir sweeps) in the eV range, with a dynamic range of 1-100/cm. There is also a frequency counter covering the range 10-200 KHz. On-board calculations of least-square fits to the electric field data over one spacecraft spin period (4 s) will provide a baseline of high-quality two-dimensional electric field components that are present in the telemetry stream, except for periods when three or four sensors are in current mode. The spacecraft potential is calculated and transmitted via DWP to other instruments on board. The three components from the search coil instrument (WHISPER) are also available in EFW with a bandwidth of 4 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article The Spherical Probe Electric Field and Waves experiment for the Cluster Mission, by G. Gustafsson et al., from which this information was obtained.</Description> | |
| 11 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 8 | + <AlternateName>Cluster 4 Spacecraft Potential (L3)</AlternateName> | |
| 9 | + <ReleaseDate>2016-10-16T11:41:44Z</ReleaseDate> | |
| 10 | + <Description> | |
| 11 | + L3 Spacecraft potential (4 sec resolution) | |
| 12 | + is normally the average potential of all available probes, measured relative to | |
| 13 | + the spacecraft. If all four probes are available, the average is done over all 4 probes. If only two | |
| 14 | + or three probes are available, the average is done over 2 opposing probes ( P1 and | |
| 15 | + P, or P3 and P4). If only two non-opposing probes are available (e.g. P2 and P3), this quantity is the | |
| 16 | + value of one of the probes. If only one probe is available, this quantity is the value of that | |
| 17 | + probe. The probes used are given by the parameter P_probes. When moderate high-bias | |
| 18 | + saturation is detected on one of the probes (indicated by bit 14 in the P_bitmask), the average | |
| 19 | + over 4 seconds is replaced by a maximum over 4 seconds to avoid errors resulting from the | |
| 20 | + resulting spikes; also the data quality is lowered for such intervals. The | |
| 21 | + individual probe potentials are available in the ancillary data</Description> | |
| 22 | + <Acknowledgement>PrincipalInvestigator: Prof. Mats Andre</Acknowledgement> | |
| 12 | 23 | <Contact> |
| 13 | - <PersonID>spase://SMWG/Person/Elena.Budnik</PersonID> | |
| 14 | - <Role>TechnicalContact</Role> | |
| 24 | + <PersonID>spase://SMWG/Person/Mats.Andre</PersonID> | |
| 25 | + <Role>PrincipalInvestigator</Role> | |
| 15 | 26 | </Contact> |
| 16 | 27 | <InformationURL> |
| 17 | - <Name>NSSDC Master Catalog listing for Cluster II Tango Electric Field and Waves (EFW)</Name> | |
| 28 | + <Name>ESA web page</Name> | |
| 29 | + <URL>http://www.cosmos.esa.int/web/csa/documentation</URL> | |
| 30 | + <Description>This site contains EFW documentation</Description> | |
| 31 | + </InformationURL> | |
| 32 | + <InformationURL> | |
| 33 | + <Name>NSSDC Master Catalog listing for Cluster II Samba Electric Field and Waves (EFW)</Name> | |
| 18 | 34 | <URL>http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=2000-045A-08</URL> |
| 19 | - <Description>This site provides information concerning the Cluster II Tango Electric Field and Waves Instrument.</Description> | |
| 35 | + <Description>This site provides information concerning the Cluster II Samba Electric Field and Waves Instrument.</Description> | |
| 20 | 36 | </InformationURL> |
| 21 | 37 | <Association> |
| 22 | 38 | <AssociationID>c4-efw-pot</AssociationID> |
| ... | ... | @@ -32,12 +48,11 @@ |
| 32 | 48 | <Name>AMDA at CDPP</Name> |
| 33 | 49 | <URL>http://amda.cdpp.eu</URL> |
| 34 | 50 | </AccessURL> |
| 35 | - <Format>NetCDF</Format> | |
| 36 | - <Acknowledgement>NASA, Georg Gustafsson</Acknowledgement> | |
| 51 | + <Format>NetCDF</Format> | |
| 37 | 52 | </AccessInformation> |
| 38 | 53 | <ProviderName>CSA</ProviderName> |
| 39 | 54 | <ProcessingLevel>Calibrated</ProcessingLevel> |
| 40 | - <ProviderResourceName>Cluster II Tango Prime Parameter Electric Field and Waves (EFW) Data</ProviderResourceName> | |
| 55 | + <ProviderResourceName>C4_CP_EFW_L3_P</ProviderResourceName> | |
| 41 | 56 | <ProviderProcessingLevel>Calibrated</ProviderProcessingLevel> |
| 42 | 57 | <InstrumentID>spase://CDPP/Instrument/AMDA/Cluster-Tango/EFW</InstrumentID> |
| 43 | 58 | <MeasurementType>ElectricField</MeasurementType> |
| ... | ... | @@ -75,10 +90,10 @@ |
| 75 | 90 | <Name>s/c pot</Name> |
| 76 | 91 | <ParameterKey>c4_potspin</ParameterKey> |
| 77 | 92 | <Description> |
| 78 | - Cluster II Tango Prime Parameter Electric Field and Waves probe potential at spin time resolution | |
| 93 | + Probe potential, Relative to Spacecraft at spin time resolution (4s) | |
| 79 | 94 | </Description> |
| 80 | - <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> | |
| 81 | - <Cadence>PT5S</Cadence> | |
| 95 | + <Ucd>phys.potential;phys.elecField;instr.obsty</Ucd> | |
| 96 | + <Cadence>PT4S</Cadence> | |
| 82 | 97 | <Units>V</Units> |
| 83 | 98 | <UnitsConversion>1.0>V</UnitsConversion> |
| 84 | 99 | <RenderingHints> |
| ... | ... |