The Simons Array CMB polarization experiment

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

doi:10.1117/12.2233103

20 July 2016 The Simons Array CMB polarization experiment

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

Author Affiliations +

Proceedings Volume 9914, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII; 99141H (2016) https://doi.org/10.1117/12.2233103
Event: SPIE Astronomical Telescopes + Instrumentation, 2016, Edinburgh, United Kingdom

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.

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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, and O. Zahn "The Simons Array CMB polarization experiment", Proc. SPIE 9914, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, 99141H (20 July 2016); https://doi.org/10.1117/12.2233103

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