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Design and performance of the SPIDER instrument.

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Title: Design and performance of the SPIDER instrument.
Author: Amiri, Mandana; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew
Issue Date: 2010
Publicly Available in cIRcle 2011-09-13
Publisher Society of Photo-Optical Instrumentation Engineers
Citation: Runyan, Marcus C.; Ade, Peter A. R.; Amiri, Mandana; Benton, Steven J.; Bihary, Richard; Bock, James J.; Bond, J. Richard; Bonetti, Joseph A.; Bryan, Sean A.; Chiang, H. Cynthia; Contaldi, Carlo R.; Crill, Brendan P.; Dore, Olivier; O'Dea, Daniel T.; , Farhang, Marzieh; Filippini, Jeffrey P.; Fissel, Laura M.; Gandilo, Natalie N.; Golwala, Sunil R.; Gudmundsson, Jon E.; Hasselfield, Matthew; Halpern, Mark; Hilton, Gene C.; Holmes, Warren; Hristov, Viktor V.; Irwin, Kent D.; Jones, William C; Kuo, Chao Lin; MacTavish, Carrie J.; Mason, Peter V.; Morford, Tracy A.; Montory, Thomas E.; Netterfield, C. Barth; Rahlin, Alexandra S.; Reintsema, Carl D.; Ruhl, John E.; Schenker, Matthew A.; Shariff, Jamil A.; Soler, J. D.; Trangsrud, Amy R.; Tucker, Rebecca S.; Tucker, Carole E.; Turner, Anthony D. Design and performance of the SPIDER instrument. Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V, edited by Wayne S. Holland, Jonas Zmuidzinas, Proceedings of SPIE Volume 7741, 77411O, 2010. http://dx.doi.org/10.1117/12.857715
Abstract: Here we describe the design and performance of the SPIDER instrument. SPIDER is a balloon-borne cosmic microwave background polarization imager that will map part of the sky at 90, 145, and 280 GHz with subdegree resolution and high sensitivity. This paper discusses the general design principles of the instrument inserts, mechanical structures, optics, focal plane architecture, thermal architecture, and magnetic shielding of the TES sensors and SQUID multiplexer. We also describe the optical, noise, and magnetic shielding performance of the 145 GHz prototype instrument insert. Copyright 2010 Society of Photo-Optical Instrumentation Engineers. One print or electronic copy may be made for personal use only. Systematic reproduction and distribution, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited.
Affiliation: Science, Faculty ofPhysics and Astronomy, Department of
URI: http://hdl.handle.net/2429/37254
Peer Review Status: Reviewed
Scholarly Level: Faculty

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