Presentation on theme: "The Mercury Imaging X-ray Spectrometer (MIXS): Lessons learned for the ATHENA Wide Field Imager (WFI) GW Fraser, A Martindale and C Thomas Space Research."— Presentation transcript:
The Mercury Imaging X-ray Spectrometer (MIXS): Lessons learned for the ATHENA Wide Field Imager (WFI) GW Fraser, A Martindale and C Thomas Space Research Centre, Department of Physics and Astronomy, University of Leicester, UK On behalf of the BepiColombo MIXS Team 1. BepiColombo ESA/JAXA mission to Mercury, launch July,2016, arrival 2022 2. MIXS – first true imaging X-ray telescope for planetary XRF 3. Enabling technologies - low mass MCP optics and DEPFET arrays 4. DEPFET advantages include: radiation tolerance and high-temp operation 5. MIXS Flight Model delivery scheduled for Q3/2014 6. MIXS as a “pathfinder” for the Wide Field Imager?
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
MIXS-C LM6 room temperature switch-on (not gain calibrated 3 peaks) Offset tracking Increase of energy with time at start of observation is caused by the MEB tracking the offsets to their operating level after switch on.
MIXS-C QM operating at room temperature Offset tracking Noisy pixel identified by OBSW and turned off Energy (arb.) Time ( arb. And non linear) Events per bin Noisy pixel identified by OBSW and turned off 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
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