DEPFET based x-ray detectors for the MIXS focal plane on BepiColombo

J. Treis; O. Hälker; L. Andricek; S. Herrmann; K. Heinzinger; T. Lauf; P. Lechner; G. Lutz; J. M. Mas-Hesse; M. Porro; R. H. Richter; J. L. San Juan; G. Schaller; M. Schnecke; F. Schopper; G. Segneri; H. Soltau; T. Stevenson; L. Strüder; C. Whitford

doi:10.1117/12.787582

24 July 2008 DEPFET based x-ray detectors for the MIXS focal plane on BepiColombo

J. Treis, O. Hälker, L. Andricek, S. Herrmann, K. Heinzinger, T. Lauf, P. Lechner, G. Lutz, J. M. Mas-Hesse, M. Porro, R. H. Richter, J. L. San Juan, G. Schaller, M. Schnecke, F. Schopper, G. Segneri, H. Soltau, T. Stevenson, L. Strüder, C. Whitford

Author Affiliations +

Proceedings Volume 7021, High Energy, Optical, and Infrared Detectors for Astronomy III; 70210Z (2008) https://doi.org/10.1117/12.787582
Event: SPIE Astronomical Telescopes + Instrumentation, 2008, Marseille, France

Abstract

DEPFET Macropixel detectors, based on the fusion of the combined Detector-Amplifier structure DEPFET with a silicon drift chamber (SDD) like drift ring structure, combine the excellent properties of the DEPFETs with the advantages of the drift detectors. As both device concepts rely on the principle of sideways depletion, a device entrance window with excellent properties is obtained at full depletion of the detector volume. DEPFET based focal plane arrays have been proposed for the Focal Plane Detectors for the MIXS (Mercury Imaging X-ray Spectrometer) instrument on BepiColombo, ESAs fifth cornerstone mission, with destination Mercury. MIXS uses a lightweight Wolter Type 1 mirror system to focus fluorescent radiation from the Mercury surface on the FPA detector, which yields the spatially resolved relative element abundance in Mercurys crust. In combination with the reference information from the Solar Intensity X-ray Spectrometer (SIXS), the element abundance can be measured quantitatively as well. The FPA needs to have an energy resolution better than 200 eV FWHM @ 1 keV and is required to cover an energy range from 0.5 keV to 10 keV, for a pixel size of 300 x 300 μm². Main challenges for the instrument are the increase in leakage current due to a high level of radiation damage, and the limited cooling resources due to the difficult thermal environment in the mercury orbit. By applying an advanced cooling concept, using all available cooling power for the detector itself, and very high speed readout, the energy resolution requirement can be kept during the entire mission lifetime up to an end-of-life dose of ~ 3 × 10¹⁰ 10 MeV p / cm². The production of the first batch of flight devices has been finished at the MPI semiconductor laboratory, and first prototype modules have been built. The results of the first tests will be presented here.

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J. Treis, O. Hälker, L. Andricek, S. Herrmann, K. Heinzinger, T. Lauf, P. Lechner, G. Lutz, J. M. Mas-Hesse, M. Porro, R. H. Richter, J. L. San Juan, G. Schaller, M. Schnecke, F. Schopper, G. Segneri, H. Soltau, T. Stevenson, L. Strüder, and C. Whitford "DEPFET based x-ray detectors for the MIXS focal plane on BepiColombo", Proc. SPIE 7021, High Energy, Optical, and Infrared Detectors for Astronomy III, 70210Z (24 July 2008); https://doi.org/10.1117/12.787582

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