Thermal design of the SPICA/ESI instrument

Douglas K. Griffin; Hiroyuki Sugita; Lionel Duband; Nicolas Luchier; Berend Winter; Peter Hargrave

doi:10.1117/12.672783

27 June 2006 Thermal design of the SPICA/ESI instrument

Douglas K. Griffin, Hiroyuki Sugita, Lionel Duband, Nicolas Luchier, Berend Winter, Peter Hargrave

Proceedings Volume 6275, Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III; 62750E (2006) https://doi.org/10.1117/12.672783
Event: SPIE Astronomical Telescopes + Instrumentation, 2006, Orlando, Florida , United States

Abstract

The ESI instrument (European SPICA Instrument) is a proposed imaging spectrometer for the 30-210μm band for the JAXA SPICA mission. The instrument will have unprecedented spatial resolution and sensitivity due to the large 03.5m telescope aperture, cold fore-optics (~5K) and high sensitivity detectors (NEP~10^-19W/√Hz). One of the key technical challenges of the design of the instrument is the thermal architecture due to the mass and cryogenic heat load constraints and the need for very low temperatures. Two candidate detector technologies have been pre-selected for inclusion in the instrument Phase-A study; Photoconductors and TES Bolometers. An overview of thermal architecture of the SPICA spacecraft is presented in order to explain the thermal interface constraints imposed on the instrument. Proposed thermal architectures for the instrument for both the TES and the Photoconductor options will be outlined including a novel design for a lightweight hybrid cooler for achieving sub 100-mK detector temperatures. This novel cooler architecture utilizes a combination of ADR and sorption coolers. Several design solutions for achieving high thermal isolation generic to both detector options are presented.

Citation Download Citation

Douglas K. Griffin, Hiroyuki Sugita, Lionel Duband, Nicolas Luchier, Berend Winter, and Peter Hargrave "Thermal design of the SPICA/ESI instrument", Proc. SPIE 6275, Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III, 62750E (27 June 2006); https://doi.org/10.1117/12.672783

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