The Simons Array: expanding POLARBEAR to three multi-chroic telescopes

被引：29

作者：

Arnold, K. ^{[11
]}

Stebor, N. ^{[11
]}

Ade, P. A. R. ^{[23
]}

Akiba, Y. ^{[26
]}

Anthony, A. E. ^{[2
,5
]}

Atlas, M. ^{[11
]}

Barron, D. ^{[11
]}

Bender, A. ^{[21
]}

Boettger, D. ^{[11
]}

Borrill, J. ^{[3
,25
]}

Chapman, S. ^{[7
]}

Chinone, Y. ^{[10
,13
]}

Cukierman, A. ^{[10
]}

Dobbs, M. ^{[21
]}

Elleflot, T. ^{[11
]}

Errard, J. ^{[3
,25
]}

Fabbian, G. ^{[1
,15
]}

Feng, C. ^{[11
]}

Gilbert, A. ^{[21
]}

Goeckner-Wald, N. ^{[10
]}

Halverson, N. W. ^{[2
,5
,12
]}

Hasegawa, M. ^{[13
,26
]}

Hattori, K.

Hazumi, M. ^{[13
,17
,26
]}

Holzapfel, W. L. ^{[10
]}

Hori, Y. ^{[13
]}

Inoue, Y. ^{[26
]}

Jaehnig, G. C. ^{[2
,12
]}

Jaffe, A. H. ^{[8
]}

Katayama, N. ^{[17
]}

Keating, B. ^{[11
]}

Kermish, Z. ^{[9
]}

Keskitalo, R. ^{[3
]}

Kisner, T. ^{[3
,25
]}

Le Jeune, M. ^{[1
]}

Lee, A. T. ^{[10
,22
]}

Leitch, E. M. ^{[4
,16
]}

Linder, E. ^{[22
]}

Matsuda, F. ^{[11
]}

Matsumura, T. ^{[14
]}

Meng, X. ^{[10
]}

Miller, N. J. ^{[12
]}

Morii, H. ^{[13
]}

Myers, M. J. ^{[10
]}

Navaroli, M. ^{[11
]}

Nishino, H. ^{[17
]}

Okamura, T. ^{[13
]}

Paar, H. ^{[11
]}

Peloton, J. ^{[1
]}

Poletti, D. ^{[1
]}

机构：

[1] Univ Paris Diderot, AstroParticule & Cosmol, CNRS IN2P3, CEA Irfu,Obs Paris,Sorbonne Paris Cite, Paris, France

[2] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA

[3] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[4] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[5] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[6] Univ Calif San Diego, Dept Elect & Comp Engn, San Diego, CA 92093 USA

[7] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada

[8] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England

[9] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA

[10] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[11] Univ Calif San Diego, Dept Phys, San Diego, CA 92093 USA

[12] Univ Colorado, Dept Phys, Boulder, CO 80309 USA

[13] KEK, High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan

[14] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan

[15] Int Sch Adv Studies SISSA, I-34014 Trieste, Italy

[16] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[17] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan

[18] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA

[19] Natl Inst Nat Sci, Natl Inst Fus Sci, Toki, Gifu 5095292, Japan

[20] Osaka Univ, Toyonaka, Osaka 5600043, Japan

[21] McGill Univ, Dept Phys, Montreal, PQ H3A 0G4, Canada

[22] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA

[23] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, S Glam, Wales

[24] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia

[25] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[26] Grad Univ Adv Studies, Hayama, Kanagawa 2400115, Japan

[27] Three Speed Log Inc, Vancouver, BC V6A 2J8, Canada

来源：

MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY VII | 2014年 / 9153卷

关键词：

cosmic background radiation; polarimeters; inflation; dark matter; neutrinos; dark energy;

D O I：

10.1117/12.2057332

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Simons Array is an expansion of the POLARBEAR cosmic microwave background (CMB) polarization experiment currently observing from the Atacama Desert in Northern Chile. This expansion will create an array of three 3.5 m telescopes each coupled to a multichroic bolometric receiver. The Simons Array will have the sensitivity to produce a > 5 sigma detection of inflationary gravitational waves with a tensor-to-scalar ratio r > 0.01, detect the known minimum 58 meV sum of the neutrino masses with 3 sigma confidence when combined with a next-generation baryon acoustic oscillation measurement, and make a lensing map of large-scale structure over the 80% of the sky available from its Chilean site. These goals require high sensitivity and the ability to extract the CMB signal from contaminating astrophysical foregrounds; these requirements are met by coupling the three high-throughput telescopes to novel multichroic lenslet-coupled pixels each measuring CMB photons in both linear polarization states over multiple spectral bands. We present the status of this instrument already under construction, and an analysis of its capabilities.

引用

页数：8

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