24 August 2015 Development of the wide field imager for Athena
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Abstract
The WFI (Wide Field Imager) instrument is planned to be one of two complementary focal plane cameras on ESA’s next X-ray observatory Athena. It combines unprecedented survey power through its large field of view of 40 arcmin x 40 arcmin together with excellent count-rate capability (≥ 1 Crab). The energy resolution of the silicon sensor is state-of-the-art in the energy band of interest from 0.2 keV to 15 keV, e.g. the full width at half maximum of a line at 6 keV will be ≤ 150 eV until the end of the nominal mission phase. This performance is accomplished by using DEPFET active pixel sensors with a pixel size of 130 μm x 130 μm well suited to the on-axis angular resolution of 5 arcsec of the mirror system. Each DEPFET pixel is a combined detector-amplifier structure with a MOSFET integrated onto a fully depleted 450 μm thick silicon bulk. Two different types of DEPFET sensors are planned for the WFI instrument: A set of four large-area sensors to cover the physical size of 14 cm x 14 cm in the focal plane and a single smaller gateable DEPFET sensor matrix optimized for high count-rate observations. Here we present the conceptual design of the instrument with focus on the critical subsystems and describe the instrument performance expectations. An outline of the model philosophy and the project organization completes the presentation.
© (2015) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Norbert Meidinger, Norbert Meidinger, Josef Eder, Josef Eder, Maria Fürmetz, Maria Fürmetz, Kirpal Nandra, Kirpal Nandra, Daniel Pietschner, Daniel Pietschner, Markus Plattner, Markus Plattner, Arne Rau, Arne Rau, Jonas Reiffers, Jonas Reiffers, Rafael Strecker, Rafael Strecker, Marco Barbera, Marco Barbera, Thorsten Brand, Thorsten Brand, Jörn Wilms, Jörn Wilms, } "Development of the wide field imager for Athena", Proc. SPIE 9601, UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XIX, 96010H (24 August 2015); doi: 10.1117/12.2187012; https://doi.org/10.1117/12.2187012
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