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Proceedings Paper

Pre-flight integration and characterization of the SPIDER balloon-borne telescope
Author(s): A. S. Rahlin; P. A. R. Ade; M. Amiri; S. J. Benton; J. J. Bock; J. R. Bond; S. A. Bryan; Hsin C. Chiang; C. R. Contaldi; B. P. Crill; O. Doré; M. Farhang; J. P. Filippini; L. M. Fissel; A. A. Fraisse; A. E. Gambrel; N. N. Gandilo; S. Golwala; Jon E. Gudmundsson; M. Halpern; M. F. Hasselfield; G. Hilton; W. A. Holmes; V. V. Hristov; K. D. Irwin; William C. Jones; Zigmund D. Kermish; C. L. Kuo; C. J. MacTavish; P. V. Mason; K. Megerian; L. Moncelsi; T. A. Morford; J. M. Nagy; C. B. Netterfield; R. O'Brient; C. Reintsema; J. E. Ruhl; M. C. Runyan; J. A. Shariff; J. D. Soler; A. Trangsrud; C. Tucker; R. S. Tucker; A. D. Turner; A. C. Weber; D. V. Wiebe; E. Y. Young
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Paper Abstract

We present the results of integration and characterization of the Spider instrument after the 2013 pre-flight campaign. Spider is a balloon-borne polarimeter designed to probe the primordial gravitational wave signal in the degree-scale B-mode polarization of the cosmic microwave background. With six independent telescopes housing over 2000 detectors in the 94 GHz and 150 GHz frequency bands, Spider will map 7.5% of the sky with a depth of 11 to 14 μK•arcmin at each frequency, which is a factor of ~5 improvement over Planck. We discuss the integration of the pointing, cryogenic, electronics, and power sub-systems, as well as pre-flight characterization of the detectors and optical systems. Spider is well prepared for a December 2014 flight from Antarctica, and is expected to be limited by astrophysical foreground emission, and not instrumental sensitivity, over the survey region.

Paper Details

Date Published: 23 July 2014
PDF: 25 pages
Proc. SPIE 9153, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, 915313 (23 July 2014); doi: 10.1117/12.2055683
Show Author Affiliations
A. S. Rahlin, Princeton Univ. (United States)
P. A. R. Ade, Cardiff Univ. (United Kingdom)
M. Amiri, The Univ. of British Columbia (Canada)
S. J. Benton, Univ. of Toronto (Canada)
J. J. Bock, California Institute of Technology (United States)
Jet Propulsion Lab. (United States)
J. R. Bond, Canadian Institute for Theoretical Astrophysics, Inc., Univ. of Toronto (Canada)
S. A. Bryan, Case Western Reserve Univ. (United States)
Hsin C. Chiang, Univ. of KwaZulu-Natal (South Africa)
C. R. Contaldi, Imperial College London (United Kingdom)
B. P. Crill, California Institute of Technology (United States)
Jet Propulsion Lab. (United States)
O. Doré, California Institute of Technology (United States)
Jet Propulsion Lab. (United States)
M. Farhang, Canadian Institute for Theoretical Astrophysics, Inc., Univ. of Toronto (Canada)
Univ. of Toronto (Canada)
J. P. Filippini, California Institute of Technology (United States)
L. M. Fissel, Univ. of Toronto (Canada)
Northwestern Univ. (United States)
A. A. Fraisse, Princeton Univ. (United States)
A. E. Gambrel, Princeton Univ. (United States)
N. N. Gandilo, Univ. of Toronto (Canada)
S. Golwala, California Institute of Technology (United States)
Jon E. Gudmundsson, Princeton Univ. (United States)
M. Halpern, The Univ. of British Columbia (Canada)
M. F. Hasselfield, Princeton Univ. (United States)
The Univ. of British Columbia (Canada)
G. Hilton, National Institute of Standards and Technology (United States)
W. A. Holmes, Jet Propulsion Lab. (United States)
V. V. Hristov, California Institute of Technology (United States)
K. D. Irwin, Stanford Univ. (United States)
Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Lab. (United States)
National Institute of Standards and Technology (United States)
William C. Jones, Princeton Univ. (United States)
Zigmund D. Kermish, Princeton Univ. (United States)
C. L. Kuo, Stanford Univ. (United States)
SLAC National Accelerator Lab., Kavli Institute for Particle Astrophysics and Cosmology (United States)
C. J. MacTavish, Kavli Institute for Cosmological Physics, Univ. of Cambridge (United Kingdom)
P. V. Mason, California Institute of Technology (United States)
K. Megerian, Jet Propulsion Lab. (United States)
L. Moncelsi, California Institute of Technology (United States)
T. A. Morford, California Institute of Technology (United States)
J. M. Nagy, Case Western Reserve Univ. (United States)
C. B. Netterfield, Univ. of Toronto (Canada)
Canadian Institute for Advanced Research (Canada)
R. O'Brient, California Institute of Technology (United States)
Jet Propulsion Lab. (United States)
C. Reintsema, National Institute of Standards and Technology (United States)
J. E. Ruhl, Case Western Reserve Univ. (United States)
M. C. Runyan, Jet Propulsion Lab. (United States)
J. A. Shariff, Univ. of Toronto (Canada)
J. D. Soler, Institut d'Astrophysique Spatiale, CNRS, Univ. Paris Sud (France)
Univ. of Toronto (Canada)
A. Trangsrud, California Institute of Technology (United States)
C. Tucker, Cardiff Univ. (United Kingdom)
R. S. Tucker, California Institute of Technology (United States)
A. D. Turner, Jet Propulsion Lab. (United States)
A. C. Weber, Jet Propulsion Lab. (United States)
D. V. Wiebe, The Univ. of British Columbia (Canada)
E. Y. Young, Princeton Univ. (United States)


Published in SPIE Proceedings Vol. 9153:
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII
Wayne S. Holland; Jonas Zmuidzinas, Editor(s)

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