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Proceedings Paper

The Simons Array CMB polarization experiment
Author(s): N. Stebor; P. Ade; Y. Akiba; C. Aleman; K. Arnold; C. Baccigalupi; B. Barch; D. Barron; S. Beckman; A. Bender; D. Boettger; J. Borrill; S. Chapman; Y. Chinone; A. Cukierman; T. de Haan; M. Dobbs; A. Ducout; R. Dunner; T. Elleflot; J. Errard; G. Fabbian; S. Feeney; C. Feng; T. Fujino; G. Fuller; A. J. Gilbert; N. Goeckner-Wald; J. Groh; G. Hall; N. Halverson; T. Hamada; M. Hasegawa; K. Hattori; M. Hazumi; C. Hill; W. L. Holzapfel; Y. Hori; L. Howe; Y. Inoue; F. Irie; G. Jaehnig; A. Jaffe; O. Jeong; N. Katayama; J. P. Kaufman; K. Kazemzadeh; B. G. Keating; Z. Kermish; R. Keskitalo; T. Kisner; A. Kusaka; M. Le Jeune; A. T. Lee; D. Leon; E. V. Linder; L. Lowry; F. Matsuda; T. Matsumura; N. Miller; J. Montgomery; M. Navaroli; H. Nishino; H. Paar; J. Peloton; D. Poletti; G. Puglisi; C. R. Raum; G. M. Rebeiz; C. L. Reichardt; P. L. Richards; C. Ross; K. M. Rotermund; Y. Segawa; B. D. Sherwin; I. Shirley; P. Siritanasak; L. Steinmetz; R. Stompor; A. Suzuki; O. Tajima; S. Takada; S. Takatori; G. P. Teply; A. Tikhomirov; T. Tomaru; B. Westbrook; N. Whitehorn; A. Zahn; O. Zahn
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Paper Abstract

The Simons Array is a next generation cosmic microwave background (CMB) polarization experiment whose science target is a precision measurement of the B-mode polarization pattern produced both by inflation and by gravitational lensing. As a continuation and extension of the successful POLARBEAR experimental program, the Simons Array will consist of three cryogenic receivers each featuring multichroic bolometer arrays mounted onto separate 3.5m telescopes. The first of these, also called POLARBEAR-2A, will be the first to deploy in late 2016 and has a large diameter focal plane consisting of dual-polarization dichroic pixels sensitive at 95 GHz and 150 GHz. The POLARBEAR-2A focal plane will utilize 7,588 antenna-coupled superconducting transition edge sensor (TES) bolometers read out with SQUID amplifiers using frequency domain multiplexing techniques. The next two receivers that will make up the Simons Array will be nearly identical in overall design but will feature extended frequency capability. The combination of high sensitivity, multichroic frequency coverage and large sky area available from our mid-latitude Chilean observatory will allow Simons Array to produce high quality polarization sky maps over a wide range of angular scales and to separate out the CMB B-modes from other astrophysical sources with high fidelity. After accounting for galactic foreground separation, the Simons Array will detect the primordial gravitational wave B-mode signal to r > 0.01 with a significance of > 5σ and will constrain the sum of neutrino masses to 40 meV (1σ) when cross-correlated with galaxy surveys. We present the current status of this funded experiment, its future, and discuss its projected science return.

Paper Details

Date Published: 20 July 2016
PDF: 9 pages
Proc. SPIE 9914, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, 99141H (20 July 2016); doi: 10.1117/12.2233103
Show Author Affiliations
N. Stebor, Univ. of California, San Diego (United States)
P. Ade, Cardiff Univ. (United Kingdom)
Y. Akiba, The Graduate Univ. for Advanced Studies (Japan)
C. Aleman, Univ. of California, San Diego (United States)
K. Arnold, Univ. of Wisconsin-Madison (United States)
C. Baccigalupi, Scuola Internazionale Superiore di Studi Avanzati (Italy)
B. Barch, Univ. of California, Berkeley (United States)
D. Barron, Univ. of California, Berkeley (United States)
S. Beckman, Univ. of California, Berkeley (United States)
A. Bender, Argonne National Lab. (United States)
Univ. of California, San Diego (United States)
D. Boettger, Pontificia Univ. Católica de Chile (Chile)
J. Borrill, Lawrence Berkeley National Lab. (United States)
Space Sciences Lab., Univ. of California, Berkeley (United States)
S. Chapman, Dalhousie Univ. (Canada)
Y. Chinone, Univ. of California, Berkeley (United States)
The Univ. of Tokyo (Japan)
A. Cukierman, Univ. of California, Berkeley (United States)
T. de Haan, Univ. of California, Berkeley (United States)
M. Dobbs, McGill Univ. (Canada)
A. Ducout, Imperial College London (United Kingdom)
R. Dunner, Pontificia Univ. Católica de Chile (Chile)
T. Elleflot, Univ. of California, San Diego (United States)
J. Errard, Institut Lagrange de Paris (France)
G. Fabbian, Scuola Internazionale Superiore di Studi Avanzati (Italy)
S. Feeney, Imperial College London (United Kingdom)
C. Feng, Univ. of California, Irvine (United States)
T. Fujino, The Univ. of Tokyo (Japan)
Yokohama National Univ. (Japan)
G. Fuller, Univ. of California, San Diego (United States)
A. J. Gilbert, McGill Univ. (Canada)
N. Goeckner-Wald, Univ. of California, Berkeley (United States)
J. Groh, Univ. of California, Berkeley (United States)
G. Hall, Univ. of California, Berkeley (United States)
N. Halverson, Univ. of Colorado at Boulder (United States)
T. Hamada, High Energy Accelerator Research Organization, KEK (Japan)
M. Hasegawa, High Energy Accelerator Research Organization, KEK (Japan)
The Graduate Institute for Advanced Studies (Japan)
K. Hattori, High Energy Accelerator Research Organization, KEK (Japan)
M. Hazumi, High Energy Accelerator Research Organization, KEK (Japan)
The Graduate Univ. for Advanced Studies (Japan)
Kavli Institute for the Physics and Mathematics of the Universe (Japan)
C. Hill, Univ. of California, Berkeley (United States)
W. L. Holzapfel, Univ. of California, Berkeley (United States)
Y. Hori, Univ. of California, Berkeley (United States)
L. Howe, Univ. of California, San Diego (United States)
Y. Inoue, The Graduate Univ. for Advanced Studies (Japan)
High Energy Accelerator Research Organization, KEK (Japan)
F. Irie, Kavli Institute for the Physics and Mathematics of the Universe (Japan)
Yokohama National Univ. (Japan)
G. Jaehnig, Univ. of Colorado at Boulder (United States)
A. Jaffe, Imperial College London (United Kingdom)
O. Jeong, Univ. of California, Berkeley (United States)
N. Katayama, Kavli Institute for the Physics and Mathematics of the Universe (Japan)
J. P. Kaufman, Univ. of California, San Diego (United States)
K. Kazemzadeh, Univ. of California, San Diego (United States)
B. G. Keating, Univ. of California, San Diego (United States)
Z. Kermish, Princeton Univ. (United States)
R. Keskitalo, Lawrence Berkeley National Lab. (United States)
Univ. of California, Berkeley (United States)
T. Kisner, Lawrence Berkeley National Lab. (United States)
Space Sciences Laboratory, Univ. of California, Berkeley (United States)
A. Kusaka, Lawrence Berkeley National Lab. (United States)
M. Le Jeune, AstroParticule et Cosmologie, Univ. Paris Diderot, CNRS (France)
A. T. Lee, Univ. of California, Berkeley (United States)
Lawrence Berkeley National Lab. (United States)
D. Leon, Univ. of California, San Diego (United States)
E. V. Linder, Lawrence Berkeley National Lab. (United States)
L. Lowry, Univ. of California, San Diego (United States)
F. Matsuda, Univ. of California, San Diego (United States)
T. Matsumura, Japan Aerospace Exploration Agency (Japan)
N. Miller, NASA Goddard Space Flight Ctr. (United States)
J. Montgomery, McGill Univ. (Canada)
M. Navaroli, Univ. of California, San Diego (United States)
H. Nishino, High Energy Accelerator Research Organization, KEK (Japan)
H. Paar, Univ. of California, San Diego (United States)
J. Peloton, Univ. of Sussex (United Kingdom)
D. Poletti, AstroParticule et Cosmologie, Univ. Paris Diderot, CNRS (France)
G. Puglisi, Scuola Internazionale Superiore di Studi Avanzati (Italy)
C. R. Raum, Univ. of California, Berkeley (United States)
G. M. Rebeiz, Univ. of California, San Diego (United States)
C. L. Reichardt, The Univ. of Melbourne (Australia)
P. L. Richards, Univ. of California, Berkeley (United States)
C. Ross, Dalhousie Univ. (Canada)
K. M. Rotermund, Dalhousie Univ. (Canada)
Y. Segawa, High Energy Accelerator Research Organization, KEK (Japan)
The Graduate Univ. for Advanced Studies (Japan)
B. D. Sherwin, Univ. of California, Berkeley (United States)
I. Shirley, Univ. of California, Berkeley (United States)
P. Siritanasak, Univ. of California, San Diego (United States)
L. Steinmetz, Univ. of California, Berkeley (United States)
R. Stompor, AstroParticule et Cosmologie, Univ. Paris Diderot, CNRS (France)
A. Suzuki, Univ. of California, Berkeley (United States)
Space Sciences Lab. (United States)
O. Tajima, High Energy Accelerator Research Organization, KEK (Japan)
The Graduate Univ. for Advanced Studies (Japan)
S. Takada, National Institute for Fusion Science (Japan)
S. Takatori, High Energy Accelerator Research Organization, KEK (Japan)
The Graduate Univ. for Advanced Studies (Japan)
G. P. Teply, Univ. of California, San Diego (United States)
A. Tikhomirov, Dalhousie Univ. (Canada)
T. Tomaru, High Energy Accelerator Research Organization, KEK (Japan)
B. Westbrook, Univ. of California, Berkeley (United States)
Space Sciences Lab. (United States)
N. Whitehorn, Univ. of California, Berkeley (United States)
A. Zahn, Univ. of California, San Diego (United States)
Univ. of Wisconsin, Madison (United States)
O. Zahn, Univ. of California, Berkeley (United States)


Published in SPIE Proceedings Vol. 9914:
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII
Wayne S. Holland; Jonas Zmuidzinas, Editor(s)

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