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Proceedings Paper

SPIDER: a new balloon-borne experiment to measure CMB polarization on large angular scales
Author(s): T. E. Montroy; P. A. R. Ade; R. Bihary; J. J. Bock; J. R. Bond; J. Brevick; C. R. Contaldi; B. P. Crill; A. Crites; O. Doré; L. Duband; S. R. Golwala; M. Halpern; G. Hilton; W. Holmes; V. V. Hristov; K. Irwin; W. C. Jones; C. L. Kuo; A. E. Lange; C. J. MacTavish; P. Mason; J. Mulder; C. B. Netterfield; E. Pascale; J. E. Ruhl; A. Trangsrud; C. Tucker; A. Turner; M. Viero
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Paper Abstract

We describe SPIDER, a novel balloon-borne experiment designed to measure the polarization of the Cosmic Microwave Background (CMB) on large angular scales. The primary goal of SPIDER is to detect the faint signature of inflationary gravitational waves in the CMB polarization. The payload consists of six telescopes, each operating in a single frequency band and cooled to 4 K by a common LN/LHe cryostat. The primary optic for each telescope is a 25 cm diameter lens cooled to 4 K. Each telescope feeds an array of antenna coupled, polarization sensitive sub-Kelvin bolometers that covers a 20 degree diameter FOV with diffraction limited resolution. The six focal planes span 70 to 300 GHz in a manner optimized to separate polarized galactic emission from CMB polarization, and together contain over 2300 detectors. Polarization modulation is achieved by rotating a cryogenic half-wave plate in front of the primary optic of each telescope. The cryogenic system is designed for 30 days of operation. Observations will be conducted during the night portions of a mid-latitude, long duration balloon flight which will circumnavigate the globe from Australia. By spinning the payload at 1 rpm with the six telescopes fixed in elevation, SPIDER will map approximately half of the sky at each frequency on each night of the flight.

Paper Details

Date Published: 12 July 2006
PDF: 16 pages
Proc. SPIE 6267, Ground-based and Airborne Telescopes, 62670R (12 July 2006); doi: 10.1117/12.670339
Show Author Affiliations
T. E. Montroy, Case Western Reserve Univ. (United States)
P. A. R. Ade, Cardiff Univ. (United Kingdom)
R. Bihary, Case Western Reserve Univ. (United States)
J. J. Bock, NASA, Jet Propulsion Lab. (United States)
J. R. Bond, Univ. of Toronto (Canada)
J. Brevick, California Institute of Technology (United States)
C. R. Contaldi, Imperial College London (United Kingdom)
B. P. Crill, California Institute of Technology (United States)
A. Crites, California Institute of Technology (United States)
O. Doré, Univ. of Toronto (Canada)
L. Duband, Commissariat à l'Energie Atomique (France)
S. R. Golwala, California Institute of Technology (United States)
M. Halpern, Univ. of British Columbia (Canada)
G. Hilton, National Institute of Standards and Technology (United States)
W. Holmes, NASA, Jet Propulsion Lab. (United States)
V. V. Hristov, California Institute of Technology (United States)
K. Irwin, National Institute of Standards and Technology (United States)
W. C. Jones, California Institute of Technology (United States)
C. L. Kuo, California Institute of Technology (United States)
A. E. Lange, California Institute of Technology (United States)
C. J. MacTavish, Univ. of Toronto (Canada)
P. Mason, California Institute of Technology (United States)
J. Mulder, NASA, Jet Propulsion Lab. (United States)
C. B. Netterfield, Univ. of Toronto (Canada)
E. Pascale, Univ. of Toronto (Canada)
J. E. Ruhl, Case Western Reserve Univ. (United States)
A. Trangsrud, California Institute of Technology (United States)
C. Tucker, Cardiff Univ. (United Kingdom)
A. Turner, NASA, Jet Propulsion Lab. (United States)
M. Viero, Univ. of Toronto (Canada)


Published in SPIE Proceedings Vol. 6267:
Ground-based and Airborne Telescopes
Larry M. Stepp, Editor(s)

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