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SCM team Laboratoire de Physique des Plasmas (formerly CETP),

THEMIS End of Prime Mission (EOPM). SCM team Laboratoire de Physique des Plasmas (formerly CETP), CNRS/Ecole Polytechnique/UPMC/P11, Palaiseau, France Co-i’s: A. Roux, O. Le Contel Software, calibration, science: P. Robert Technical Manager: C. Coillot Lead Engineer: A. Bouabdellah

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SCM team Laboratoire de Physique des Plasmas (formerly CETP),

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  1. THEMIS End of Prime Mission (EOPM) SCM team Laboratoire de Physique des Plasmas (formerly CETP), CNRS/Ecole Polytechnique/UPMC/P11, Palaiseau, France Co-i’s: A. Roux, O. Le Contel Software, calibration, science: P. Robert Technical Manager: C. Coillot Lead Engineer: A. Bouabdellah Technician: D. Alison

  2. SCM sensitivity at laboratory IN.SCM-3. The SCM sensitivity shall be better than 1pT/Hz^1/2 @10Hz , and 0.1 pT/Hz^1/2 @1 kHz. requirements

  3. In flight SCM sensitivity In flight sensitivity before cleanup 100 32 Hz 8 Hz NEMI (pT/sqrt(Hz)) SCM ground sensitivities are recovered after cleanup processing although spurious noises are still present 0.001 In flight sensitivity after cleanup 100 requirements NEMI (pT/sqrt(Hz)) 0.001 From wave burst mode data (8192 S/s)

  4. On orbit performance vs time No modification of the SCM sensitivity even during and after the longest eclipse (no temperature drift): TH-B/P1 flew through its longest eclipse on March 11, 2009 between 0558 and 1017 UT SCW spectra on THB performed after this long shadow period March 15 10:09:40-10:09:48 UT March 11, 09:34:14-09:34:22 UT 4 days after Shadow period

  5. Scientific assessment of data products • Thanks to onboard triggering SCM waveforms are available during substorm onsets and have allowed to study the role of the electromagnetic waves or structures: • Fast survey range (0.1-4 Hz) which covers the ion cyclotron frequency corresponding to the current disruption process • Particle burst (0.1-64 Hz) which allows to detect the “whistler” mode emissions and the lower hydrid drift instability • Wave burst (0.1-4 kHz) unique mode allowing the detection of the non linear coherent structures so called “electron holes”. First detection of the parallel magnetic field component. • Onboard FFT of SCM data indicated that these are no magnetic fluctuations above the electron cyclotron frequency

  6. SCM data history Issue on SCM & EFI waveforms in wave burst mode (Dec. 2007 to April 2008) due to data packetizing Fixed by the Berkeley team (J. Lewis).  the SCW data base has been re-processed in July 2008. Issue on SCM&EFI FBK data due to a compression problem (Oct-Dec 2008) Fixed by the Berkeley team (implementation of a patch IDPU FSW v5.1 successively on each probe) in beginning of March 2009

  7. All L1 SCM data are available on line (using THEMIS software) Calibration with or without noise data reduction can be performed by any user thanks to the THEMIS software (cf. Le Contel et al., SSR, 2009) Errors are minimized due to precise ground calibrations which demonstrated that 15 SCM transfer functions corresponding to the 5 SCM tri-axis are almost identical with less of 1dB of difference (cf. Roux et al. SSR 2009) SCM data accessibility, calibration and error Table 1e - Sensibility of FM5

  8. Publication history NB: Only SCM L1 data are available for now 2008: 8 papers with SCM CoI as coauthors (4 SSR+3 GRL+1 JGR) 2009: 7 papers with SCM CoI as coauthors (2 JGR+ 1 AG+ 2 PRL+1GRL+1 Science)

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