A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING SOUTH POLE TELESCOPE DATA

被引：205

作者：

van Engelen, A. ^{[1
]}

Keisler, R. ^{[2
,3
]}

Zahn, O. ^{[4
,5
]}

Aird, K. A.

Benson, B. A. ^{[2
,6
]}

Bleem, L. E. ^{[2
,3
]}

Carlstrom, E. ^{[2
,3
,6
,7
,8
]}

Chang, C. L. ^{[2
,6
,8
]}

Cho, H. M. ^{[9
]}

Crawford, T. M. ^{[2
,7
]}

Crites, A. T. ^{[2
,7
]}

de Haan, T. ^{[1
]}

Dobbs, M. A. ^{[1
]}

Dudley, J. ^{[1
]}

George, E. M. ^{[10
]}

Halverson, N. W. ^{[11
,12
]}

Holder, G. P. ^{[1
]}

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

Hoover, S. ^{[2
,3
]}

Hou, Z. ^{[13
]}

Hrubes, D.

Joy, M. ^{[14
]}

Knox, L. ^{[13
]}

Lee, A. T. ^{[10
,15
]}

Leitch, E. M. ^{[2
,7
]}

Lueker, M. ^{[16
]}

Luong-Van, D.

McMahon, J. J. ^{[17
]}

Mehl, J. ^{[2
]}

Meyer, S. S. ^{[2
,3
,6
,7
]}

Millea, M. ^{[13
]}

Mohr, J. J. ^{[18
,19
,20
]}

Montroy, T. E. ^{[21
]}

Natoli, T. ^{[2
,3
]}

Padin, S. ^{[2
,7
,16
]}

Plagge, T. ^{[2
,7
]}

Pryke, C. ^{[22
]}

Reichardt, C. L. ^{[10
]}

Ruhl, J. E. ^{[21
]}

Sayre, J. T. ^{[21
]}

Schaffer, K. K. ^{[2
,6
,23
]}

Shaw, L. ^{[24
]}

Shirokoff, E. ^{[9
]}

Spieler, H. G. ^{[15
]}

Staniszewski, Z. ^{[21
]}

Stark, A. A. ^{[25
]}

Story, K. ^{[2
,3
]}

Vanderlinde, K. ^{[1
]}

Vieira, J. D. ^{[16
]}

Williamson, R. ^{[2
,7
]}

机构：

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

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

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

[4] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA

[5] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA

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

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

[8] Argonne Natl Lab, Argonne, IL 60439 USA

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

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

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

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

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

[14] NASA Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA

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

[16] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[17] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[18] Univ Munich, Dept Phys, D-81679 Munich, Germany

[19] Excellence Cluster Universe, D-85748 Garching, Germany

[20] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[21] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA

[22] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA

[23] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA

[24] Yale Univ, Dept Phys, New Haven, CT 06520 USA

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

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 756卷 / 02期

基金：

美国国家科学基金会;

关键词：

cosmic background radiation; cosmological parameters; cosmology: observations; gravitational lensing: weak; large-scale structure of universe; ATACAMA COSMOLOGY TELESCOPE; PROBE WMAP OBSERVATIONS; POWER SPECTRUM; GALAXY CLUSTERS; DARK-MATTER; CMB; ANISOTROPIES; TEMPERATURE; RECONSTRUCTION; POLARIZATION;

D O I：

10.1088/0004-637X/756/2/142

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use South Pole Telescope data from 2008 and 2009 to detect the non-Gaussian signature in the cosmic microwave background (CMB) produced by gravitational lensing and to measure the power spectrum of the projected gravitational potential. We constrain the ratio of the measured amplitude of the lensing signal to that expected in a fiducial Lambda CDM cosmological model to be 0.86 +/- 0.16, with no lensing disfavored at 6.3 sigma. Marginalizing over Lambda CDM cosmological models allowed by the Wilkinson Microwave Anisotropy Probe (WMAP7) results in a measurement of A(lens) = 0.90 +/- 0.19, indicating that the amplitude of matter fluctuations over the redshift range 0.5 less than or similar to z less than or similar to 5 probed by CMB lensing is in good agreement with predictions. We present the results of several consistency checks. These include a clear detection of the lensing signature in CMB maps filtered to have no overlap in Fourier space, as well as a "curl" diagnostic that is consistent with the signal expected for Lambda CDM. We perform a detailed study of bias in the measurement due to noise, foregrounds, and other effects and determine that these contributions are relatively small compared to the statistical uncertainty in the measurement. We combine this lensing measurement with results from WMAP7 to improve constraints on cosmological parameters when compared to those from WMAP7 alone: we find a factor of 3.9 improvement in the measurement of the spatial curvature of the universe, Omega(k) = -0.0014 +/- 0.0172; a 10% improvement in the amplitude of matter fluctuations within Lambda CDM, sigma(8) = 0.810 +/- 0.026; and a 5% improvement in the dark energy equation of state, w = -1.04 +/- 0.40. When compared with the measurement of w provided by the combination of WMAP7 and external constraints on the Hubble parameter, the addition of the lensing data improves the measurement of w by 15% to give w = -1.087 +/- 0.096.

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