SPT-3G: A Next-Generation Cosmic Microwave Background Polarization Experiment on the South Pole Telescope

被引：381

作者：

Benson, B. A. ^{[1
,2
]}

Ade, P. A. R. ^{[3
]}

Ahmed, Z. ^{[4
,5
,6
]}

Allen, S. W. ^{[4
,5
,6
]}

Arnold, K. ^{[7
]}

Austermann, J. E. ^{[8
]}

Bender, A. N. ^{[9
]}

Bleem, L. E. ^{[1
,10
]}

Carlstrom, J. E. ^{[1
,2
,10
,11
,12
]}

Chang, C. L. ^{[1
,2
,10
]}

Cho, H. M. ^{[6
]}

Cliche, J. F. ^{[9
]}

Crawford, T. M. ^{[1
,2
]}

Cukierman, A. ^{[13
]}

de Haan, T. ^{[9
]}

Dobbs, M. A. ^{[9
,14
]}

Dutcher, D. ^{[1
,12
]}

Everett, W. ^{[8
]}

Gilbert, A. ^{[9
]}

Halverson, N. W. ^{[8
,15
]}

Hanson, D. ^{[9
]}

Harrington, N. L. ^{[13
]}

Hattori, K. ^{[16
]}

Henning, J. W. ^{[8
]}

Hilton, G. C. ^{[17
]}

Holder, G. P. ^{[9
,14
]}

Holzapfel, W. L. ^{[13
]}

Irwin, K. D. ^{[4
,5
,6
]}

Keisler, R. ^{[4
,5
]}

Knox, L. ^{[18
]}

Kubik, D.

Kuo, C. L. ^{[4
,5
,6
]}

Lee, A. T. ^{[13
,19
]}

Leitch, E. M. ^{[1
,2
]}

Li, D. ^{[17
]}

McDonald, M. ^{[20
]}

Meyer, S. S. ^{[1
,2
,11
,12
]}

Montgomery, J. ^{[9
]}

Myers, M. ^{[13
]}

Natoli, T. ^{[1
,12
]}

Nguyen, H.

Novosad, V. ^{[21
]}

Padin, S. ^{[22
]}

Pan, Z. ^{[1
,12
]}

Pearson, J. ^{[21
]}

Reichardt, C. L. ^{[13
,23
]}

Ruhl, J. E. ^{[24
]}

Saliwanchik, B. R. ^{[24
]}

Simard, G. ^{[9
]}

Smecher, G. ^{[25
]}

机构：

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

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

[3] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, Wales

[4] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA

[5] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[6] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

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

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

[9] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

[10] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA

[11] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA

[12] Univ Chicago, Dept Phys, Chicago, IL 60637 USA

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

[14] Canadian Inst Adv Res, CIFAR Program Cosmol & Grav, Toronto, ON M5G 1Z8, Canada

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

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

[17] NIST, Quantum Devices Grp, Boulder, CO 80305 USA

[18] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

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

[20] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[21] Argonne Natl Lab, Div Mat Sci, Argonne, IL 60439 USA

[22] CALTECH, Pasadena, CA 91125 USA

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

[24] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA

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

[26] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[27] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M55 3H4, Canada

[28] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M55 3H4, Canada

[29] Univ Illinois, Dept Astron, Urbana, IL 61801 USA

[30] Univ Illinois, Dept Phys, Urbana, IL 61801 USA

来源：

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

关键词：

B-modes; cosmic microwave background; cryogenics; inflation; gravitational lensing; neutrino mass; optical design; polarization; transition-edge sensors; GALAXY CLUSTERS; DAMPING TAIL; DEG(2); CMB; ANISOTROPIES; MULTIPLEXER; CONSTRAINTS; STATISTICS; ESTIMATORS; CATALOG;

D O I：

10.1117/12.2057305

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We describe the design of a new polarization sensitive receiver, SPT-3G, for the 10-meter South Pole Telescope (sPT). The SPT-3G receiver will deliver a factor of similar to 20 improvement in mapping speed over the current receiver, SPT-POL. The sensitivity of the SPT-3G receiver will enable the advance from statistical detection of B-mode polarization anisotropy power to high signal-to-noise measurements of the individual modes, i.e., maps. This will lead to precise (similar to 0.06 eV) constraints on the sum of neutrino masses with the potential to directly address the neutrino mass hierarchy. It will allow a separation of the lensing and inflationary B-mode power spectra, improving constraints on the amplitude and shape of the primordial signal, either through SPT-3G data alone or in combination with BICEP2/KECK, which is observing the same area of sky. The measurement of small-scale temperature anisotropy will provide new constraints on the epoch of reionization. Additional science from the SPT-3G survey will be significantly enhanced by the synergy with the ongoing optical Dark Energy Survey (DES), including: a 1% constraint on the bias of optical tracers of large-scale structure, a measurement of the differential Doppler signal from pairs of galaxy clusters that will test General Relativity on similar to 200 Mpc scales, and improved cosmological constraints from the abundance of clusters of galaxies.

引用

页数：21

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