SPICA sub-Kelvin cryogenic chains |
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| Authors: | L. Duband J.M. Duval N. Luchier T. Prouve |
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| Affiliation: | 1. CEA/INAC/Service des Basses Températures, Grenoble 38054, France;2. California Institute of Technology, Pasadena, CA 91125, USA;1. NASA Kennedy Space Center, M/S: NE-F6 Kennedy Space Center, FL, USA, 32899;2. NASA Marshall Space Flight Center, M/S:ER-24 Huntsville, AL, USA, 35812;1. Laboratory of Physical Chemistry of the Solid State, Faculty of Sciences, University of Sfax, BP 1171, 3000, Sfax, Tunisia;2. Institut de Chimie de la Matière Condensée de Bordeaux, Centre National de la Recherche Scientifique, University of Bordeaux, 87 avenue du Dr A. Schweitzer, 33608, Pessac, Bordeaux, France;3. Laboratory of Applied Physics, Faculty of Sciences, University of Sfax, BP 1171, 3000, Sfax, Tunisia;1. Université de Nice Sophia-Antipolis, INLN, CNRS, 06560 Valbonne, France;2. Institut-Lorentz, Universiteit Leiden, P.O. Box 9506, 2300 RA Leiden, The Netherlands;3. Aix Marseille Université, CNRS, CPT, UMR 7332, 13288 Marseille, France;4. Université de Toulon, CNRS, CPT, UMR 7332, 83957 La Garde, France;1. Shanghai Institute of Applied Physics, Chinese Academy of Science, Shanghai 201800, China;2. Department of Engineering Physics, Tsinghua University, Beijing 100084, China;3. Shanghai Key Laboratory of Cryogenics & Superconducting RF Technology, Shanghai 201800, China;4. Shanghai Science Research Center, Chinese Academy of Science, Shanghai 201204, China;1. Laboratoire d’Ingénierie et Sciences des Matériaux (LISM EA 4695), Université de Reims Champagne-Ardenne, UFR Sciences et Naturelles, Bat. 6, Moulin de la Housse, BP 1039, 51687 Reims Cedex 2, France;2. Department of Materials Science (MTM), KU Leuven, Kasteelpark Arenberg 44, 3001 Haverlee (Leuven), Belgium;3. Laboratory of Physical Chemistry and Electrochemistry, Faculty of Non-Ferrous Metals, AGH University of Science and Technology, al. A. Mickiewicza 30, 30059 Krakow, Poland;4. Key Laboratory of Electromagnetic Processing of Materials (Ministry of Education), Northeastern University, 314 Box, 110004 Shenyang, China;5. Department of Electronics, AGH University of Science and Technology, al. A. Mickiewicza 30, 30059 Krakow, Poland |
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| Abstract: | SPICA, a Japanese led mission, is part of the JAXA future science program and is planned for launch in 2018. SPICA will perform imaging and spectroscopic observations in the mid- and far-IR waveband, and is developing instrumentation spanning the 5–400 μm range. The SPICA payload features several candidate instruments, some of them requiring temperature down to 50 mK. This is currently the case for SAFARI, a core instrument developed by a European-based consortium, and BLISS proposed by CALTECH/JPL in the US.SPICA’s distinctive feature is to actively cool its telescope to below 6 K. In addition, SPICA is a liquid cryogen free satellite and all the cooling will be provided by radiative cooling (L2 orbit) down to 30 K and by mechanical coolers for lower temperatures. The satellite will launch warm and slowly equilibrate to its operating temperatures once in orbit. This warm launch approach makes it possible to eliminate a large liquid cryogen tank and to use the mass saved to launch a large diameter telescope (3.2 m). This 4 K cooled telescope significantly reduces its own thermal radiation, offering superior sensitivity in the infrared region.The cryogenic system that enables this warm launch/cooled telescope concept is a key issue of the mission. This cryogenic chain features a number of cooling stages comprising passive radiators, Stirling coolers and several Joule Thomson loops, offering cooling powers at typically 20, 4.5, 2.5 and 1.7 K. The SAFARI and BLISS detectors require cooling to temperatures as low as 50 mK. The instrument coolers will be operated from these heat sinks. They are composed of a small demagnetization refrigerator (ADR) pre cooled by either a single or a double sorption cooler, respectively for SAFARI and BLISS. The BLISS cooler maintains continuous cooling at 300 mK and thus suppresses the thermal equilibrium time constant of the large focal plane.These hybrid architectures allow designing low weight coolers able to reach 50 mK. Because the sorption cooler has extremely low mass for a sub-Kelvin cooler, it allows the stringent mass budget to be met. These concepts are discussed in this paper. |
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