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Proceedings Paper

SPTpol: an instrument for CMB polarization measurements with the South Pole Telescope
Author(s): J. E. Austermann; K. A. Aird; J. A. Beall; D. Becker; A. Bender; B. A. Benson; L. E. Bleem; J. Britton; J. E. Carlstrom; C. L. Chang; H. C. Chiang; H.-M. Cho; T. M. Crawford; A. T. Crites; A. Datesman; T. de Haan; M. A. Dobbs; E. M. George; N. W. Halverson; N. Harrington; J. W. Henning; G. C. Hilton; G. P. Holder; W. L. Holzapfel; S. Hoover; N. Huang; J. Hubmayr; K. D. Irwin; R. Keisler; J. Kennedy; L. Knox; A. T. Lee; E. Leitch; D. Li; M. Lueker; D. P. Marrone; J. J. McMahon; J. Mehl; S. S. Meyer; T. E. Montroy; T. Natoli; J. P. Nibarger; M. D. Niemack; V. Novosad; S. Padin; C. Pryke; C. L. Reichardt; J. E. Ruhl; B. R. Saliwanchik; J. T. Sayre; K. K. Schaffer; E. Shirokoff; A. A. Stark; K. Story; K. Vanderlinde; J. D. Vieira; G. Wang; R. Williamson; V. Yefremenko; K. W. Yoon; O. Zahn
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Paper Abstract

SPTpol is a dual-frequency polarization-sensitive camera that was deployed on the 10-meter South Pole Telescope in January 2012. SPTpol will measure the polarization anisotropy of the cosmic microwave background (CMB) on angular scales spanning an arcminute to several degrees. The polarization sensitivity of SPTpol will enable a detection of the CMB “B-mode” polarization from the detection of the gravitational lensing of the CMB by large scale structure, and a detection or improved upper limit on a primordial signal due to inationary gravity waves. The two measurements can be used to constrain the sum of the neutrino masses and the energy scale of ination. These science goals can be achieved through the polarization sensitivity of the SPTpol camera and careful control of systematics. The SPTpol camera consists of 768 pixels, each containing two transition-edge sensor (TES) bolometers coupled to orthogonal polarizations, and a total of 1536 bolometers. The pixels are sensitive to light in one of two frequency bands centered at 90 and 150 GHz, with 180 pixels at 90 GHz and 588 pixels at 150 GHz. The SPTpol design has several features designed to control polarization systematics, including: singlemoded feedhorns with low cross-polarization, bolometer pairs well-matched to dfference atmospheric signals, an improved ground shield design based on far-sidelobe measurements of the SPT, and a small beam to reduce temperature to polarization leakage. We present an overview of the SPTpol instrument design, project status, and science projections.

Paper Details

Date Published: 27 September 2012
PDF: 18 pages
Proc. SPIE 8452, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 84521E (27 September 2012); doi: 10.1117/12.927286
Show Author Affiliations
J. E. Austermann, Univ. of Colorado at Boulder (United States)
K. A. Aird, Univ. of Chicago (United States)
J. A. Beall, National Institute of Standards and Technology (United States)
D. Becker, National Institute of Standards and Technology (United States)
A. Bender, McGill Univ. (Canada)
B. A. Benson, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
L. E. Bleem, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
J. Britton, National Institute of Standards and Technology (United States)
J. E. Carlstrom, Kavli Institute for Cosmological Physics (United States)
Argonne National Lab. (United States)
Univ. of Chicago (United States)
C. L. Chang, Kavli Institute for Cosmological Physics (United States)
Argonne National Lab. (United States)
Univ. of Chicago (United States)
H. C. Chiang, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
H.-M. Cho, National Institute of Standards and Technology (United States)
T. M. Crawford, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
A. T. Crites, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
A. Datesman, Argonne National Lab. (United States)
T. de Haan, McGill Univ. (Canada)
M. A. Dobbs, McGill Univ. (Canada)
E. M. George, Univ. of California, Berkeley (United States)
N. W. Halverson, Univ. of Colorado at Boulder (United States)
N. Harrington, Univ. of California, Berkeley (United States)
J. W. Henning, Univ. of Colorado at Boulder (United States)
G. C. Hilton, National Institute of Standards and Technology (United States)
G. P. Holder, McGill Univ. (Canada)
W. L. Holzapfel, Univ. of California, Berkeley (United States)
S. Hoover, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
N. Huang, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
J. Hubmayr, National Institute of Standards and Technology (United States)
K. D. Irwin, National Institute of Standards and Technology (United States)
R. Keisler, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
J. Kennedy, McGill Univ. (Canada)
L. Knox, Univ. of California, Davis (United States)
A. T. Lee, Univ. of California, Berkeley (United States)
E. Leitch, Kavli Institute for Cosmological Physics (United States)
D. Li, National Institute of Standards and Technology (United States)
M. Lueker, California Institute of Technology (United States)
D. P. Marrone, The Univ. of Arizona (United States)
J. J. McMahon, Univ. of Michigan (United States)
J. Mehl, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
S. S. Meyer, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
T. E. Montroy, Case Western Reserve Univ. (United States)
T. Natoli, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
J. P. Nibarger, National Institute of Standards and Technology (United States)
M. D. Niemack, National Institute of Standards and Technology (United States)
V. Novosad, Argonne National Lab. (United States)
S. Padin, Kavli Institute for Cosmological Physics (United States)
C. Pryke, Univ. of Minnesota (United States)
C. L. Reichardt, Univ. of California, Berkeley (United States)
J. E. Ruhl, Case Western Reserve Univ. (United States)
B. R. Saliwanchik, Case Western Reserve Univ. (United States)
J. T. Sayre, Case Western Reserve Univ. (United States)
K. K. Schaffer, The School of the Art Institute of Chicago (United States)
E. Shirokoff, California Institute of Technology (United States)
A. A. Stark, Harvard-Smithsonian Ctr. for Astrophysics (United States)
K. Story, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
K. Vanderlinde, McGill Univ. (Canada)
J. D. Vieira, California Institute of Technology (United States)
G. Wang, Argonne National Lab. (United States)
R. Williamson, Kavli Institute for Cosmological Physics (United States)
Univ. of Chicago (United States)
V. Yefremenko, Argonne National Lab. (United States)
K. W. Yoon, National Institute of Standards and Technology (United States)
O. Zahn, Univ. of California, Berkeley (United States)


Published in SPIE Proceedings Vol. 8452:
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI
Wayne S. Holland, Editor(s)

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