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

Treis, J.; Hälker, Olaf; Andricek, L.; Herrmann, Sven; Heinzinger, K.; Lauf, T.; Lechner, P.; Lütz, G.; Mas-Hesse, J. M.; Porro, M.; Richter, R.; Juan, J. L. San; Schäller, G.; Schnecke, M.; Schopper, F.; Segneri, G.; Soltau, H.; Stevenson, T.; Strüder, L.; Whitford, C. H.

doi:10.1117/12.787582

Cited by 6 publications

(2 citation statements)

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“…Both optic modules will be iridium coated to increase their effective area. The spectral resolving power is achieved by the use of DEPFET MPDs as sensitive elements in the focal plane assembly (FPA) [20]. For the sake of simplicity, both of MIXS channels are equipped with identical FPAs with one MPD each.…”

Section: The Mixs Focal Plane Assembly On Bepicolombomentioning

confidence: 99%

Pixel detectors for x-ray imaging spectroscopy in space

et al. 2009

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Pixelated semiconductor detectors for X-ray imaging spectroscopy are foreseen as key components of the payload of various future space missions exploring the x-ray sky. Located on the platform of the new Spectrum-Roentgen-Gamma satellite, the eROSITA (extended Roentgen Survey with an Imaging Telescope Array) instrument will perform an imaging all-sky survey up to an X-ray energy of 10 keV with unprecedented spectral and angular resolution. The instrument will consist of seven parallel oriented mirror modules each having its own pnCCD camera in the focus. The satellite born X-ray observatory SIMBOL-X will be the first mission to use formation-flying techniques to implement an X-ray telescope with an unprecedented focal length of around 20 m. The detector instrumentation consists of separate high-and low energy detectors, a monolithic 128 × 128 DEPFET macropixel array and a pixellated CdZTe detector respectively, making energy

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Section: The Mixs Focal Plane Assembly On Bepicolombomentioning

confidence: 99%

Pixel detectors for x-ray imaging spectroscopy in space

et al. 2009

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“…10 DEPFETs provide good energy resolution (∼130 eV at 1 keV at the beginning of operations and ∼200 eV at the end of the mission) but are more radiation hard than MOS CCDs. CCDs are read out by clocking charge from pixel to pixel, and eventually into an output register.…”

Section: Instrument Overviewmentioning

confidence: 99%

The Mercury Imaging X-ray Spectrometer: instrument overview

et al. 2009

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We report progress in the design of the BepiColombo Mercury Imaging X-ray Spectrometer (MIXS). This instrument consists of two modules; a Wolter I soft X-ray telescope based on radially packed microchannel plate optics (MIXS-T) and a profiled collimator which uses a square pore square packed microchannel plate array to restrict its field of view (MIXS-C). Both instrument modules have identical focal planes (DEPFET macropixel array) providing an energy resolution of better than 200 eV FWHM throughout the mission.The primary science goal of MIXS is to perform X-ray fluorescence spectroscopy of the Hermean surface with unprecedented spatial and energy resolution. This allows discrimination between different regolith types, and by combining with data from other instruments, between competing models of crustal evolution and planetary formation. MIXS will also probe the complex coupling between the planet's surface, exosphere and magnetosphere by observing Particle Induced X-ray Emission (PIXE).

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