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The SEIS experiment on INSIGHT Discovery mission to Mars IPPW- 10, June 18th 2013, San José

Rene Perez , SEIS instrument manager, CNES Ph. Lognonné , S. Deraucourt , IPGP D. Mimoun, ISAE K. Hurst, JPL and the SEIS Team. The SEIS experiment on INSIGHT Discovery mission to Mars IPPW- 10, June 18th 2013, San José.

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The SEIS experiment on INSIGHT Discovery mission to Mars IPPW- 10, June 18th 2013, San José

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  1. Rene Perez, SEIS instrument manager, CNES Ph. Lognonné, S. Deraucourt, IPGP D. Mimoun, ISAE K. Hurst, JPL and the SEIS Team The SEIS experiment on INSIGHT Discovery mission to MarsIPPW-10, June 18th 2013, San José

  2. Afundamental contribution to understanding the early evolution of the terrestrial planets through investigations of the Mars interior 1

  3. Why bother about planetary interiors ? • The interior of a planet retains the signature of its origin and subsequent evolution. • The interior structure provides the boundary conditions that can constraint our understanding of both accretion composition and conditions • The interior structure reveals the signature of early differentiation processes Crust Crust Core Crust Crust Core Core Crust Mantle Mantle Mantle Mantle Mantle

  4. Seismology on Mars: a long story... 1976: Viking 3 months of (accumulated) seismicdata 1996: Mars 96 Failedatlaunch 2016: Insight Will provide1 martianyear of data (or more?)

  5. Scientific objectives: • Understand the formation and evolution of terrestrial planets through investigation of the interior structure and processes of Mars • Determine the present level of tectonic activity and impact flux on Mars Objectives translated in Threshold Science Requirements for SEIS: • Rayleigh wave group velocitydispersion • P and S arrivaltimes • Phobostideamplitude a few/yr M~5.5 Global ~ 10/yr M~4.5 Global to regional M~3.5 ~100/yr Regional 4.6 6 2.6 3.3 Magnitudes

  6. Use or disclosure of information contained on this sheet is subject to the restriction on the title page of this document. The InSight Payload: SEIS RISE HP3

  7. 3 VBBs-Long period axis (IPGP) The SEIS experiment overview: On Lander Mars surface APSS: Wind sensors (CAB) Pressure sensors (JPL) and Magnetometer (UCLA) WTS: Wind and Thermal shield (JPL) E-Box(ETHZ) Tether /Tether box (JPL) 3 SP sensors (IC)short period Earth Ground segment SEIS operational (CNES) and data center (IPGP) LVL: Leveling system (MPS) SEISManagement (CNES)

  8. Wake-up Wake-up Wake-up TBD hrs TBD hrs C&DH t SEIS communication session E-Box NVmemory usage SEIS Operation Concept • The instrument is always ON and keeps on acquiring raw data • SW (and C&DH) wakes up ~every TBD hours during about ten of minutes • In routine one daily DSN pass for data downlink

  9. The Sphere VBB (long period sensors)

  10. Sphere VBB development history: InSight PDR 16 years old...

  11. Performance Validation Plan: • Phobos tide calibration : • end-to-end performance test done on Earth • SP performances • end-to-end performance test done on Earth • VBB performances (S/N): end-to-end test not doable on Earth: • VBBs performance cannot be measured on Earth without a compensation mass (so, not in Mars configuration) • Only reduced functional tests can be performed on flight VBBs (due to the difference in gravity) • Planning will be incompatible in long term (e.g. ~month) tests in low noise sites with temperature comparable to Martian condition (e.g. Antarctica) • Final performance is demonstrated by Tests and Modeling: • Early model (VBB5) extensively tested for performance, providing elements for last tuning of flight models • Measure the instrument self noise, and correct with the Performance Model • Measure sensitivity to external environment parameters • Test in Martian environment when possible (e.g. temperature, pressure capsule noise) • Simulate, when tests are not possible, to derive SEIS performance in Martian environment (Magnetic field, Pressure)

  12. SEIS successtree (example) + Sci. Temp. performance (IPGP) Validation of Thermal noise allocation (CNES) (CNES) Mars Temperature Model (Oxford) (Oxford) Convection Model Ground Inside/payload skin Exterior skin

  13. Performances budget: VBB noise budget (Velocity output):

  14. Performance Validation: VBB5 first results … Thermal environment tests done (and to be continued): • Thermal sensitivity • Behavior under cold environment (recentering, transfer function …) • Full characterization @ cold Ambient Noise@StMaur des Fossés (0.1-1Hz) 2013/05/21 M7.4 Earthquake Tonga 2013/05/23 @St Maur des Fossés (0.1-1Hz) Early model, but highly representative design under tests.

  15. Seismic Vault • VBB (one axis) + reference seismometer installed on the same pillar. • Axes in vacuum chamber + µ-metal shielding • Recombine reference seismometer axes to fit VBB’s sensitivity axis, then compare measurements both in time and frequency domain

  16. Low noise test in lownoise site? • Unique way to detect noise issues at ng/Hz1/2 on fully integrated instrument • This test has been done last summer (BFO) with a previous instrument configuration (significant gain on the results!) • It’s worth to be repeated with VBB5, but challenging for planning • Could be attempted in // with ATLO (2015...)? BFO or Antartica?...

  17. Thanks for your attention!

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