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

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. ElleflotJ. 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

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › peer-review

26 Scopus citations

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.

Original language	English
Title of host publication	Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII
Editors	Jonas Zmuidzinas, Wayne S. Holland
Publisher	SPIE
ISBN (Electronic)	9781510602076
DOIs	https://doi.org/10.1117/12.2233103
State	Published - 2016
Event	Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII - Edinburgh, United Kingdom Duration: 28 Jun 2016 → 1 Jul 2016

Publication series

Name	Proceedings of SPIE - The International Society for Optical Engineering
Volume	9914
ISSN (Print)	0277-786X
ISSN (Electronic)	1996-756X

Conference

Conference	Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII
Country/Territory	United Kingdom
City	Edinburgh
Period	28/06/16 → 1/07/16

Keywords

Cosmic microwave background radiation
Dark matter
Gark energy
Gravitational lensing
Inflation
Neutrinos
Polarimeters
Polarization

Access to Document

10.1117/12.2233103

Cite this

Stebor, N., Ade, P., Akiba, Y., Aleman, C., Arnold, K., Baccigalupi, C., Barch, B., Barron, D., Beckman, S., Bender, A., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Cukierman, A., De Haan, T., Dobbs, M., Ducout, A., Dunner, R., ... Zahn, O. (2016). The Simons Array CMB polarization experiment. In J. Zmuidzinas, & W. S. Holland (Eds.), Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII Article 99141H (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 9914). SPIE. https://doi.org/10.1117/12.2233103

@inproceedings{14dc60ac2b1247018165a2c7e6183076,

title = "The Simons Array CMB polarization experiment",

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.",

keywords = "Cosmic microwave background radiation, Dark matter, Gark energy, Gravitational lensing, Inflation, Neutrinos, Polarimeters, Polarization",

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

note = "Publisher Copyright: {\textcopyright} 2016 SPIE.; Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII ; Conference date: 28-06-2016 Through 01-07-2016",

year = "2016",

doi = "10.1117/12.2233103",

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series = "Proceedings of SPIE - The International Society for Optical Engineering",

publisher = "SPIE",

editor = "Jonas Zmuidzinas and Holland, {Wayne S.}",

booktitle = "Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII",

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Stebor, N, Ade, P, Akiba, Y, Aleman, C, Arnold, K, Baccigalupi, C, Barch, B, Barron, D, Beckman, S, Bender, A, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Cukierman, A, De Haan, T, Dobbs, M, Ducout, A, Dunner, R, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Fuller, G, Gilbert, AJ, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hattori, K, Hazumi, M, Hill, C, Holzapfel, WL, Hori, Y, Howe, L, Inoue, Y, Irie, F, Jaehnig, G, Jaffe, A, Jeong, O, Katayama, N, Kaufman, JP, Kazemzadeh, K, Keating, BG, Kermish, Z, Keskitalo, R, Kisner, T, Kusaka, A, Le Jeune, M, Lee, AT, Leon, D, Linder, EV, Lowry, L, Matsuda, F, Matsumura, T, Miller, N, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Poletti, D, Puglisi, G, Raum, CR, Rebeiz, GM, Reichardt, CL, Richards, PL, Ross, C, Rotermund, KM, Segawa, Y, Sherwin, BD, Shirley, I, Siritanasak, P, Steinmetz, L, Stompor, R, Suzuki, A, Tajima, O, Takada, S, Takatori, S, Teply, GP, Tikhomirov, A, Tomaru, T, Westbrook, B, Whitehorn, N, Zahn, A & Zahn, O 2016, The Simons Array CMB polarization experiment. in J Zmuidzinas & WS Holland (eds), Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII., 99141H, Proceedings of SPIE - The International Society for Optical Engineering, vol. 9914, SPIE, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, Edinburgh, United Kingdom, 28/06/16. https://doi.org/10.1117/12.2233103

The Simons Array CMB polarization experiment. / Stebor, N.; Ade, P.; Akiba, Y. et al.
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII. ed. / Jonas Zmuidzinas; Wayne S. Holland. SPIE, 2016. 99141H (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 9914).

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › peer-review

TY - GEN

T1 - The Simons Array CMB polarization experiment

AU - Stebor, N.

AU - Ade, P.

AU - Akiba, Y.

AU - Aleman, C.

AU - Arnold, K.

AU - Baccigalupi, C.

AU - Barch, B.

AU - Barron, D.

AU - Beckman, S.

AU - Bender, A.

AU - Boettger, D.

AU - Borrill, J.

AU - Chapman, S.

AU - Chinone, Y.

AU - Cukierman, A.

AU - De Haan, T.

AU - Dobbs, M.

AU - Ducout, A.

AU - Dunner, R.

AU - Elleflot, T.

AU - Errard, J.

AU - Fabbian, G.

AU - Feeney, S.

AU - Feng, C.

AU - Fujino, T.

AU - Fuller, G.

AU - Gilbert, A. J.

AU - Goeckner-Wald, N.

AU - Groh, J.

AU - Hall, G.

AU - Halverson, N.

AU - Hamada, T.

AU - Hasegawa, M.

AU - Hattori, K.

AU - Hazumi, M.

AU - Hill, C.

AU - Holzapfel, W. L.

AU - Hori, Y.

AU - Howe, L.

AU - Inoue, Y.

AU - Irie, F.

AU - Jaehnig, G.

AU - Jaffe, A.

AU - Jeong, O.

AU - Katayama, N.

AU - Kaufman, J. P.

AU - Kazemzadeh, K.

AU - Keating, B. G.

AU - Kermish, Z.

AU - Keskitalo, R.

AU - Kisner, T.

AU - Kusaka, A.

AU - Le Jeune, M.

AU - Lee, A. T.

AU - Leon, D.

AU - Linder, E. V.

AU - Lowry, L.

AU - Matsuda, F.

AU - Matsumura, T.

AU - Miller, N.

AU - Montgomery, J.

AU - Navaroli, M.

AU - Nishino, H.

AU - Paar, H.

AU - Peloton, J.

AU - Poletti, D.

AU - Puglisi, G.

AU - Raum, C. R.

AU - Rebeiz, G. M.

AU - Reichardt, C. L.

AU - Richards, P. L.

AU - Ross, C.

AU - Rotermund, K. M.

AU - Segawa, Y.

AU - Sherwin, B. D.

AU - Shirley, I.

AU - Siritanasak, P.

AU - Steinmetz, L.

AU - Stompor, R.

AU - Suzuki, A.

AU - Tajima, O.

AU - Takada, S.

AU - Takatori, S.

AU - Teply, G. P.

AU - Tikhomirov, A.

AU - Tomaru, T.

AU - Westbrook, B.

AU - Whitehorn, N.

AU - Zahn, A.

AU - Zahn, O.

PY - 2016

Y1 - 2016

N2 - 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.

AB - 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.

KW - Cosmic microwave background radiation

KW - Dark matter

KW - Gark energy

KW - Gravitational lensing

KW - Inflation

KW - Neutrinos

KW - Polarimeters

KW - Polarization

UR - http://www.scopus.com/inward/record.url?scp=85015047537&partnerID=8YFLogxK

U2 - 10.1117/12.2233103

DO - 10.1117/12.2233103

M3 - 會議論文篇章

AN - SCOPUS:85015047537

T3 - Proceedings of SPIE - The International Society for Optical Engineering

BT - Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII

A2 - Zmuidzinas, Jonas

A2 - Holland, Wayne S.

PB - SPIE

T2 - Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII

Y2 - 28 June 2016 through 1 July 2016

ER -

The Simons Array CMB polarization experiment

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Publication series

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Keywords

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