Detector electronics sub-system development for the NewAthena Wide Field Imager

Andreas Lederhuber; Jonas Reiffers; Benjamin Mican; Jaroslav Laifr; Samuel Pliego; Aysun Sönmez; Thomas Schanz; Francisco Javier Veredas; Olaf Hälker; Chris Tenzer; Sebastian Albrecht; Hermine Schnetler

doi:10.1117/12.3019653

21 August 2024 Detector electronics sub-system development for the NewAthena Wide Field Imager

Andreas Lederhuber, Jonas Reiffers, Benjamin Mican, Jaroslav Laifr, Samuel Pliego, Aysun Sönmez, Thomas Schanz, Francisco Javier Veredas, Olaf Hälker, Chris Tenzer, Sebastian Albrecht, Hermine Schnetler

Author Affiliations +

Proceedings Volume 13093, Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray; 130934E (2024) https://doi.org/10.1117/12.3019653
Event: SPIE Astronomical Telescopes + Instrumentation, 2024, Yokohama, Japan

Conference Poster

Abstract

The Wide Field Imager (WFI) is one of the two instruments of the NewAthena X-ray mission selected by ESA. Five DEPFET detector modules are implemented in WFI that detect energy, spatial distribution and incidence time of incoming X-ray photons within the energy range of 0.2 keV up to 15 keV. The WFI instrument successfully completed the Instrument System Requirement Review (I-SRR) in March 2022. NewAthena had undergone a mission redefinition, and on February 2024 the mission restarted again. On the road to NewAthena launch, an Engineering Model (EM) as well as a Structural and Thermal Model (STM) of the WFI Detector Electronics Sub-System (DES) is developed. In this paper we present the current status of the DES development. Each DES consists of three modules: Galvanic Isolation Module (GIM), Power Conditioning Module (PCM) and Frame Processing Module (FPM). The function of the FPM is to control the readout Front End Electronic ASICs of its corresponding detector module. The FPM digitizes the analog output signals of the CH and performs an on-board preprocessing. The preprocessing and the control signal generation is done by the FPGA-based Frame Processor (FP). The GIM provides the primary to secondary power conversion, generating all the low voltages required for the operation of the DES, as well as the back-contact high-voltage (up to -200 V) required for the detector operation. It is composed of custom-designed DC-DC converters. Another task of the DES is to provide all the regulated power lines to the CH. More than twenty independent power lines are supplied from the DES to the detectors and have to be switched on and off in a specified sequence. This function is implemented within the PCM.

(2024) Published by SPIE. Downloading of the abstract is permitted for personal use only.

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Andreas Lederhuber, Jonas Reiffers, Benjamin Mican, Jaroslav Laifr, Samuel Pliego, Aysun Sönmez, Thomas Schanz, Francisco Javier Veredas, Olaf Hälker, Chris Tenzer, Sebastian Albrecht, and Hermine Schnetler "Detector electronics sub-system development for the NewAthena Wide Field Imager", Proc. SPIE 13093, Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, 130934E (21 August 2024); https://doi.org/10.1117/12.3019653

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