The DCU: the detector control unit of the SAFARI instrument onboard SPICA

A. Clénet; L. Ravera; B. Bertrand; A. Cros; R. Hou; B. D. Jackson; B. J. van Leeuwen; D. Van Loon; Y. Parot; E. Pointecouteau; A. Sournac; N. Ta

doi:10.1117/12.925380

24 September 2012 The DCU: the detector control unit of the SAFARI instrument onboard SPICA

A. Clénet, L. Ravera, B. Bertrand, A. Cros, R. Hou, B. D. Jackson, B. J. van Leeuwen, D. Van Loon, Y. Parot, E. Pointecouteau, A. Sournac, N. Ta

Author Affiliations +

Proceedings Volume 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI; 84521V (2012) https://doi.org/10.1117/12.925380
Event: SPIE Astronomical Telescopes + Instrumentation, 2012, Amsterdam, Netherlands

Abstract

The SpicA FAR infrared Instrument (SAFARI) is a European instrument for the infrared domain telescope SPICA, a JAXA space mission. The SAFARI detectors are Transistor Edge Sensors (TES) arranged in 3 matrixes. The TES front end electronic is based on Superconducting Quantum Interference Devices (SQUIDs) and it does the readout of the 3500 detectors with Frequency Division Multiplexing (FDM) type architecture. The Detector Control Unit (DCU), contributed by IRAP, manages the readout of the TES by computing and providing the AC-bias signals (1 - 3 MHz) to the TES and by computing the demodulation of the returning signals. The SQUID being highly non-linear, the DCU has also to provide a feedback signal to increase the SQUID dynamic. Because of the propagation delay in the cables and the processing time, a classic feedback will not be stable for AC-bias frequencies up to 3 MHz. The DCU uses a specific technique to compensate for those delays: the BaseBand FeedBack (BBFB). This digital data processing is done for the 3500 pixels in parallel. Thus, to keep the DCU power budget within its allocation we have to specifically optimize the architecture of the digital circuit with respect to the power consumption. In this paper we will mainly present the DCU architecture. We will particularly focus on the BBFB technique used to linearize the SQUID and on the optimization done to reduce the power consumption of the digital processing circuit.

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A. Clénet, L. Ravera, B. Bertrand, A. Cros, R. Hou, B. D. Jackson, B. J. van Leeuwen, D. Van Loon, Y. Parot, E. Pointecouteau, A. Sournac, and N. Ta "The DCU: the detector control unit of the SAFARI instrument onboard SPICA", Proc. SPIE 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 84521V (24 September 2012); https://doi.org/10.1117/12.925380

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KEYWORDS

Sensors

Filtering (signal processing)

Digital electronics

Space telescopes

Telescopes

Electronic filtering

Signal processing

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