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BepiColombo Science R equirements

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BepiColombo Science R equirements

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  1. The Mercury Imaging X-ray Spectrometer (MIXS): Lessons learned for the ATHENA Wide Field Imager (WFI)GW Fraser, A Martindale and C ThomasSpace Research Centre, Department of Physics and Astronomy, University of Leicester, UKOn behalf of the BepiColombo MIXS Team1. BepiColombo ESA/JAXA mission to Mercury, launch July,2016, arrival 20222. MIXS – first true imaging X-ray telescope for planetary XRF3. Enabling technologies - low mass MCP optics and DEPFET arrays4. DEPFET advantages include: radiation tolerance and high-temp operation5. MIXS Flight Model delivery scheduled for Q3/20146. MIXS as a “pathfinder” for the Wide Field Imager?

  2. BepiColombo Science Requirements for the mapping of the elemental composition of Mercury on global, intermediate and local scales dictate two complementary X-ray channels Wide field-of-view – Non-Imaging Collimator MIXS-C Narrow field-of-view – Imaging Telescope MIXS-T Common detector format – 64 x64 pixel, 300 x 300 micron DEPFET APS

  3. QM MIXS

  4. MIXSFunctionalSchematic MEB MIXS Electronics Box 1660 g FPA Focal Plane Assembly 1330g FEE Front End Electronics 248g DPA Detector Plane Array

  5. Detector Assembly

  6. MIXS Electronic Block Diagram

  7. ATHENA WFI Electronic Block Diagram (Figure 6 of Rau et al.)

  8. MIXS-C LM6 room temperature switch-on (not gain calibrated  3 peaks) Increase of energy with time at start of observation is caused by the MEB tracking the offsets to their operating level after switch on. Offset tracking

  9. MIXS-C QM operating at room temperature Noisy pixel identified by OBSW and turned off Events per bin Time ( arb. And non linear) Noisy pixel identified by OBSW and turned off Energy (arb.) The noisy pixel in the QM is only visible at room temperature and is turned off by the OBSW after it is identified by autonomous algorithms Offset tracking Energy (arb.)

  10. Gain, Offset and Noise

  11. X-ray calibration of MIXS FM

  12. Carbon and Oxygen band response

  13. Titanium Self-fluorescence

  14. Stainless steel target

  15. Conclusions • The BepiColombo MIXS DEPFET focal plane array provides a direct technical precursor, in FM build for an ESA Cornerstone mission, for the ATHENA WFI • Sensor control, communication and internal calibration have been implemented in a rad-hard FPGA • Split pixel, hot pixel.. Corrections have been implemented in OBSW • Front End Electronics have been implemented in low-mass, hybrid components • MIXS DEPFET detectors have been subjected to environmental test and detailed X-ray calibration and provide a basis for power and mass estimates for the WFI • TRL 6 now

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