2.0.1 spase://vspo/numericalData/P_CLUSTER_HDR_PEACE_DATA Cluster PEACE Digital Data 2007-06-01T00:00:00 Cluster PEACE digital data; password needed spase://SMWG/Person/Andrew.N.Fazakerley PrincipalInvestigator spase://SMWG/Person/Joey.Mukherjee GeneralContact spase://SMWG/Repository/SWRI Online Restricted PEACE site at SWRI http://cluster2.space.swri.edu/ Binary CALIBRATED spase://SMWG/Instrument/Cluster2-Rumba/PEACE spase://SMWG/Instrument/Cluster2-Salsa/PEACE spase://SMWG/Instrument/Cluster2-Samba/PEACE spase://SMWG/Instrument/Cluster2-Tango/PEACE ThermalPlasma EnergeticParticles 2001-01-09T00:00:00 -P3D Data are within a few days of current. Earth.Magnetosphere spase://SMWG/Observatory/Cluster2-Rumba Cluster 2/FM5 (Rumba) 2000-045A FM5 Rumba Cluster-1 2009-05-20T20:00:12Z This Cluster II spacecraft, FM5 (Rumba), is also known as Phoenix, after a mythical Arabian bird which was burnt on a funeral pile and then rose from the ashes to live again. The original Cluster of four spacecraft experienced a launch failure in 1996. (NSSDC will carry the name "Cluster96" in its information files to designate the unsuccessful 1996 four-spacecraft Ariane 5 launch.) Phoenix was approved in July 1996 as a replacement for the lost four-spacecraft group. It was later (April 1997) agreed that the potential science return from a full Cluster reflight was so important that a further three near-replicas of the original spacecraft would also be built. This Cluster II spacecraft, FM5 (Rumba), was launched together with FM8 (Tango) by a Soyuz-Fregat rocket from Baikonur. The four similar spacecraft of the Cluster II mission are part of ESA's and NASA's Solar-Terrestrial Science Program (STSP). The purpose of the Cluster II mission is to study small-scale structures in three dimensions in the Earth's plasma environment, such as those involved in the interaction between the solar wind and the magnetospheric plasma, in global magnetotail dynamics, in cross-tail currents, and in the formation and dynamics of the neutral line and of plasmoids. The four Cluster II spacecraft will orbit in a tetrahedral formation in near-polar orbits of nominally 4 x 19.6 Earth radii, with period about 57 hours, and inclination about 90.7 degrees. Relative distances between the spacecraft will be adjusted in the course of the mission, depending on the spatial scales of the structures to be studied, varying from a few hundred km to a few Earth radii. The tetrahedral formation is essential for making three-dimensional measurements and for determining the curl of vectorial quantities such as the magnetic field. The orbits of all four spacecraft will be frequently maneuvered so as to achieve the targeted investigations. See http://jsoc1.bnsc.rl.ac.uk/pub/PlanningData.html for ongoing updates of orbital information and other status. Each spacecraft will be spin-stabilized, normally at around 15 rpm, and will be cylindrical in shape, with a 2.9-m diameter and 1.3-m length. It will have two rigid 5-m radial experiment booms, four 50-m experiment wire booms, and two axial telecommunications antenna booms. Telemetry downlink bit rate will be 2 to 262 kbit/s. Each spacecraft will have AC and DC magnetometers, an electric fields and waves sensor, an electron emitter/detector, an electron density sounder, electron and ion plasma analysers, an energetic particle detector, an ion emitter, and a data processing unit. Cluster operations will be performed by ESOC in Darmstadt, Germany, with support from NASA's Deep Space Network. Cluster is also an IACG mission. The scientific data are distributed by ESOC using CD-ROM as a medium to the Principal Investigators, Co-Investigators and the network of eight national data centres (6 in Europe, 1 in USA and 1 in China) that form the Cluster Science Data System (CSDS). There are approximately 80 recipients world-wide. Science operations are carried out by the Joint Science Operations Centre, co-located with the UK data centre at RAL, Didcot. A wide scientific community will have differing rights of access to the Cluster data. Scientists wishing to access Cluster data should contact their national Data Centres. The Cluster Summary Parameters are publicly available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public and the Prime Parameters are available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/ to project personnel (password-protected). See the Cluster II WWW site at http://sci.esa.int/cluster/ for more information, including spacecraft and exprient status. An article on 'The Resurrection of the Cluster Scientific Mission' was published in ESA Bulletin no. 91 (August 1997). A complete overview of the original mission, written before the loss with Ariane-5, was given in a series of articles in ESA Bulletin no. 84 (November 1995). ESA SP-1159, Paris, March 1993 is entitled "Cluster: Mission, Payload and Supporting Activities." spase://SMWG/Person/Melvyn.L.Goldstein ProjectScientist NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-045A Information about the Cluster 2/FM5 (Rumba) mission CLUSTER Heliosphere.NearEarth spase://SMWG/Observatory/Cluster2-Salsa Cluster 2/FM6 (Salsa) 2000-041B FM6 Salsa Cluster-2 2009-05-20T20:00:12Z This Cluster II spacecraft, FM6 (Salsa), was launched together with FM7 (Samba) by a Soyuz-Fregat rocket from Baikonur. The four similar spacecraft of the Cluster II mission are part of ESA's and NASA's Solar-Terrestrial Science Program (STSP). The current Cluster II mission is a near-replica of the original four-spacecraft mission lost at launch in 1996. (NSSDC will carry the name "Cluster96" in its information files to designate the unsuccessful 1996 four-spacecraft Ariane 5 launch.) The purpose of the Cluster II mission is to study small-scale structures in three dimensions in the Earth's plasma environment, such as those involved in the interaction between the solar wind and the magnetospheric plasma, in global magnetotail dynamics, in cross-tail currents, and in the formation and dynamics of the neutral line and of plasmoids. The four Cluster II spacecraft will orbit in a tetrahedral formation in near-polar orbits of nominally 4 x 19.6 Earth radii, with period about 57 hours, and inclination about 90.7 degrees. Relative distances between the spacecraft will be adjusted in the course of the mission, depending on the spatial scales of the structures to be studied, varying from a few hundred km to a few Earth radii. The tetrahedral formation is essential for making three-dimensional measurements and for determining the curl of vectorial quantities such as the magnetic field. The orbits of all four spacecraft will be frequently maneuvered so as to achieve the targeted investigations. See http://jsoc1.bnsc.rl.ac.uk/pub/PlanningData.html for ongoing updates of orbital information and other status. Each spacecraft will be spin-stabilized, normally at around 15 rpm, and will be cylindrical in shape, with a 2.9-m diameter and 1.3-m length. It will have two rigid 5-m radial experiment booms, four 50-m experiment wire booms, and two axial telecommunications antenna booms. Telemetry downlink bit rate will be 2 to 262 kbit/s. Each spacecraft will have AC and DC magnetometers, an electric fields and waves sensor, an electron emitter/detector, an electron density sounder, electron and ion plasma analysers, an energetic particle detector, an ion emitter, and a data processing unit. Cluster operations will be performed by ESOC in Darmstadt, Germany, with support from NASA's Deep Space Network. Cluster is also an IACG mission. The scientific data are distributed by ESOC using CD-ROM as a medium to the Principal Investigators, Co-Investigators and the network of eight national data centres (6 in Europe, 1 in USA and 1 in China) that form the Cluster Science Data System (CSDS). There are approximately 80 recipients world-wide. Science operations are carried out by the Joint Science Operations Centre, co-located with the UK data centre at RAL, Didcot. A wide scientific community will have differing rights of access to the Cluster data. Scientists wishing to access Cluster data should contact their national Data Centres. The Cluster Summary Parameters are publicly available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public and the Prime Parameters are available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/ to project personnel (password-protected). See the Cluster II WWW site at http://sci.esa.int/cluster/ for more information, iincluding status of spacecraft and instruments. An article on 'The Resurrection of the Cluster Scientific Mission' was published in ESA Bulletin no. 91 (August 1997). A complete overview of the original mission, written before the loss with Ariane-5, was given in a series of articles in ESA Bulletin no. 84 (November 1995). ESA SP-1159, Paris, March 1993 is entitled "Cluster: Mission, Payload and Supporting Activities." spase://SMWG/Person/Melvyn.L.Goldstein ProjectScientist NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-041B Information about the Cluster 2/FM6 (Salsa) mission CLUSTER Earth.Magnetosheath Earth.Magnetosphere.Main Earth.Magnetosphere.Polar spase://SMWG/Observatory/Cluster2-Samba Cluster 2/FM7 (Samba) 2000-041A FM7 Samba Cluster-3 2009-05-20T20:00:12Z This Cluster II spacecraft, FM7 (Samba), was launched together with FM6 (Salsa) by a Soyuz-Fregat rocket from Baikonur. The four similar spacecraft of the Cluster II mission are part of ESA's and NASA's Solar-Terrestrial Science Program (STSP). The current Cluster II mission is a near-replica of the original four-spacecraft mission lost at launch in 1996. (NSSDC will carry the name "Cluster96" in its information files to designate the unsuccessful 1996 four-spacecraft Ariane 5 launch.) The purpose of the Cluster II mission is to study small-scale structures in three dimensions in the Earth's plasma environment, such as those involved in the interaction between the solar wind and the magnetospheric plasma, in global magnetotail dynamics, in cross-tail currents, and in the formation and dynamics of the neutral line and of plasmoids. The four Cluster II spacecraft will orbit in a tetrahedral formation in near-polar orbits of nominally 4 x 19.6 Earth radii, with period about 57 hours, and inclination about 90.7 degrees.. Relative distances between the spacecraft will be adjusted in the course of the mission, depending on the spatial scales of the structures to be studied, varying from a few hundred km to a few Earth radii. The tetrahedral formation is essential for making three-dimensional measurements and for determining the curl of vectorial quantities such as the magnetic field. The orbits of all four spacecraft will be frequently maneuvered so as to achieve the targeted investigations. See http://jsoc1.bnsc.rl.ac.uk/pub/PlanningData.html for ongoing updates of orbital information and other status. Each spacecraft will be spin-stabilized, normally at around 15 rpm, and will be cylindrical in shape, with a 2.9-m diameter and 1.3-m length. It will have two rigid 5-m radial experiment booms, four 50-m experiment wire booms, and two axial telecommunications antenna booms. Telemetry downlink bit rate will be 2 to 262 kbit/s. Each spacecraft will have AC and DC magnetometers, an electric fields and waves sensor, an electron emitter/detector, an electron density sounder, electron and ion plasma analysers, an energetic particle detector, an ion emitter, and a data processing unit. Cluster operations will be performed by ESOC in Darmstadt, Germany, with support from NASA's Deep Space Network. Cluster is also an IACG mission. The scientific data are distributed by ESOC using CD-ROM as a medium to the Principal Investigators, Co-Investigators and the network of eight national data centres (6 in Europe, 1 in USA and 1 in China) that form the Cluster Science Data System (CSDS). There are approximately 80 recipients world-wide. Science operations are carried out by the Joint Science Operations Centre, co-located with the UK data centre at RAL, Didcot. A wide scientific community will have differing rights of access to the Cluster data. Scientists wishing to access Cluster data should contact their national Data Centres. The Cluster Summary Parameters are publicly available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public and the Prime Parameters are available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/ to project personnel (password-protected). See the Cluster II WWW site at http://sci.esa.int/cluster/ for more information, including status of the spacecraft and instruments. An article on 'The Resurrection of the Cluster Scientific Mission' was published in ESA Bulletin no. 91 (August 1997). A complete overview of the original mission, written before the loss with Ariane-5, was given in a series of articles in ESA Bulletin no. 84 (November 1995). ESA SP-1159, Paris, March 1993 is entitled "Cluster: Mission, Payload and Supporting Activities." spase://SMWG/Person/Melvyn.L.Goldstein ProjectScientist NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-041A Information about the Cluster 2/FM7 (Samba) mission CLUSTER Earth.Magnetosphere.Main Earth.Magnetosheath Earth.Magnetosphere.Polar spase://SMWG/Observatory/Cluster2-Tango Cluster 2/FM8 (Tango) 2000-045B Cluster-4 Tango FM8 2009-05-20T20:00:12Z This Cluster II spacecraft, FM8 (Tango), was launched together with FM5 (Rumba) by a Soyuz-Fregat rocket from Baikonur. The four similar spacecraft of the Cluster II mission are part of ESA's and NASA's Solar-Terrestrial Science Program (STSP). The current Cluster II mission is a near-replica of the original four-spacecraft mission lost at launch in 1996. (NSSDC will carry the name "Cluster96" in its information files to designate the unsuccessful 1996 four-spacecraft Ariane 5 launch.) The purpose of the Cluster II mission is to study small-scale structures in three dimensions in the Earth's plasma environment, such as those involved in the interaction between the solar wind and the magnetospheric plasma, in global magnetotail dynamics, in cross-tail currents, and in the formation and dynamics of the neutral line and of plasmoids. The four Cluster II spacecraft will orbit in a tetrahedral formation in near-polar orbits of nominally 4 x 19.6 Earth radii, with period about 57 hours, and inclination about 90.7 degrees. Relative distances between the spacecraft will be adjusted in the course of the mission, depending on the spatial scales of the structures to be studied, varying from a few hundred km to a few Earth radii. The tetrahedral formation is essential for making three-dimensional measurements and for determining the curl of vectorial quantities such as the magnetic field. The orbits of all four spacecraft will be frequently maneuvered so as to achieve the targeted investigations. See http://jsoc1.bnsc.rl.ac.uk/pub/PlanningData.html for ongoing updates of orbital information and other status. Each spacecraft will be spin-stabilized, normally at around 15 rpm, and will be cylindrical in shape, with a 2.9-m diameter and 1.3-m length. It will have two rigid 5-m radial experiment booms, four 50-m experiment wire booms, and two axial telecommunications antenna booms. Telemetry downlink bit rate will be 2 to 262 kbit/s. Each spacecraft will have AC and DC magnetometers, an electric fields and waves sensor, an electron emitter/detector, an electron density sounder, electron and ion plasma analysers, an energetic particle detector, an ion emitter, and a data processing unit. Cluster operations will be performed by ESOC in Darmstadt, Germany, with support from NASA's Deep Space Network. Cluster is also an IACG mission. The scientific data are distributed by ESOC using CD-ROM as a medium to the Principal Investigators, Co-Investigators and the network of eight national data centres (6 in Europe, 1 in USA and 1 in China) that form the Cluster Science Data System (CSDS). There are approximately 80 recipients world-wide. Science operations are carried out by the Joint Science Operations Centre, co-located with the UK data centre at RAL, Didcot. A wide scientific community will have differing rights of access to the Cluster data. Scientists wishing to access Cluster data should contact their national Data Centres. The Cluster Summary Parameters are publicly available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ and the Prime Parameters are available on CDAWeb at http://cdaweb.gsfc.nasa.gov/cdaweb/ to project personnel (password-protected). See the Cluster II WWW site at http://sci.esa.int/cluster/ for more information. An article on 'The Resurrection of the Cluster Scientific Mission' was published in ESA Bulletin no. 91 (August 1997). A complete overview of the original mission, written before the loss with Ariane-5, was given in a series of articles in ESA Bulletin no. 84 (November 1995). ESA SP-1159, Paris, March 1993 is entitled "Cluster: Mission, Payload and Supporting Activities." spase://SMWG/Person/Melvyn.L.Goldstein ProjectScientist NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-045B Information about the Cluster 2/FM8 (Tango) mission CLUSTER Earth.Magnetosheath Earth.Magnetosphere.Main Earth.Magnetosphere.Polar spase://SMWG/Instrument/Cluster2-Samba/PEACE Plasma Electron and Current Experiment (PEACE) PEACE 2009-05-20T21:10:15Z The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7--10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0--180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. 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 ``PEACE: a Plasma Electron and Current Experiment,'' by A. D. Johnstone et al., from which this information was obtained. spase://SMWG/Person/Andrew.N.Fazakerley PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-041A&ex=5 Information about the Plasma Electron and Current Experiment (PEACE) experiment on the Cluster 2/FM7 (Samba) mission. EnergeticParticleInstrument Plasma Electron and Current Experiment (PEACE) on Cluster 2/FM7 (Samba) spase://SMWG/Observatory/Cluster2-Samba spase://SMWG/Instrument/Cluster2-Rumba/PEACE Plasma Electron and Current Experiment (PEACE) PEACE 2009-05-20T21:10:10Z The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7--10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0--180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. 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 ``PEACE: a Plasma Electron and Current Experiment,'' by A. D. Johnstone et al., from which this information was obtained. spase://SMWG/Person/Andrew.N.Fazakerley PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-045A&ex=5 Information about the Plasma Electron and Current Experiment (PEACE) experiment on the Cluster 2/FM5 (Rumba) mission. EnergeticParticleInstrument Plasma Electron and Current Experiment (PEACE) on Cluster 2/FM5 (Rumba) spase://SMWG/Observatory/Cluster2-Rumba spase://SMWG/Instrument/Cluster2-Salsa/PEACE Plasma Electron and Current Experiment (PEACE) PEACE 2009-05-20T21:10:16Z The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7--10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0--180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. 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 ``PEACE: a Plasma Electron and Current Experiment,'' by A. D. Johnstone et al., from which this information was obtained. spase://SMWG/Person/Andrew.N.Fazakerley PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-041B&ex=5 Information about the Plasma Electron and Current Experiment (PEACE) experiment on the Cluster 2/FM6 (Salsa) mission. EnergeticParticleInstrument Plasma Electron and Current Experiment (PEACE) on Cluster 2/FM6 (Salsa) spase://SMWG/Observatory/Cluster2-Salsa spase://SMWG/Instrument/Cluster2-Tango/PEACE Plasma Electron and Current Experiment (PEACE) PEACE 2009-05-20T21:10:13Z The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7--10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0--180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. 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 ``PEACE: a Plasma Electron and Current Experiment,'' by A. D. Johnstone et al., from which this information was obtained. spase://SMWG/Person/Andrew.N.Fazakerley PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=2000-045B&ex=5 Information about the Plasma Electron and Current Experiment (PEACE) experiment on the Cluster 2/FM8 (Tango) mission. EnergeticParticleInstrument Plasma Electron and Current Experiment (PEACE) on Cluster 2/FM8 (Tango) spase://SMWG/Observatory/Cluster2-Tango spase://SMWG/Repository/SWRI SWRI 2008-06-18T18:05:57Z spase://SMWG/Person/UNKNOWN GeneralContact spase://SMWG/Person/Melvyn.L.Goldstein 1999-08-18T00:00:00Z Dr. Melvyn L. Goldstein GSFC-Code 692 melvyn.l.goldstein@nasa.gov +1-301-286-7828 spase://SMWG/Person/Andrew.N.Fazakerley Dr. Andrew N. Fazakerley University College London spase://SMWG/Person/UNKNOWN 1999-01-01T00:00:00Z UNKNOWN UNKNOWN spase://SMWG/Person/Joey.Mukherjee Joey Mukherjee Southwest Research Institute joey@swri.edu