MEASUREMENTS OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH THE SOUTH POLE TELESCOPE

被引：135

作者：

Lueker, M. ^{[1
]}

Reichardt, C. L. ^{[1
]}

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

Zahn, O. ^{[4
]}

Ade, P. A. R. ^{[5
]}

Aird, K. A.

Benson, B. A. ^{[1
,2
,3
]}

Bleem, L. E. ^{[2
,6
]}

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

Chang, C. L. ^{[2
,3
]}

Cho, H. -M. ^{[1
]}

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

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

de Haan, T. ^{[8
]}

Dobbs, M. A. ^{[8
]}

George, E. M. ^{[1
]}

Hall, N. R. ^{[9
]}

Halverson, N. W. ^{[10
,11
]}

Holder, G. P. ^{[8
]}

Holzapfel, W. L. ^{[1
]}

Hrubes, J. D.

Joy, M. ^{[12
]}

Keisler, R. ^{[2
,6
]}

Knox, L. ^{[9
]}

Lee, A. T. ^{[1
,13
]}

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

McMahon, J. J. ^{[2
,3
,14
]}

Mehl, J. ^{[1
]}

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

Mohr, J. J. ^{[15
,16
,17
]}

Montroy, T. E. ^{[18
]}

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

Plagge, T. ^{[1
]}

Pryke, C. ^{[2
,3
,7
]}

Ruhl, J. E. ^{[18
]}

Shaw, L. ^{[8
,19
]}

Shirokoff, E. ^{[1
]}

Spieler, H. G. ^{[13
]}

Stalder, B. ^{[20
]}

Staniszewski, Z. ^{[18
]}

Stark, A. A. ^{[20
]}

Vanderlinde, K. ^{[8
]}

Vieira, J. D. ^{[2
,6
]}

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

机构：

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

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

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

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

[5] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales

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

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

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

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

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

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

[12] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA

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

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

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

[16] Excellence Cluster Univ, D-85748 Garching, Germany

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 719卷 / 02期

基金：

美国国家科学基金会;

关键词：

cosmic background radiation; cosmological parameters; cosmology: observations; galaxies: clusters: intracluster medium; large-scale structure of universe; ANGULAR POWER SPECTRUM; STAR-FORMING GALAXIES; EXTRAGALACTIC SOURCES; DUST EMISSION; CLUSTERS; PROBE; CMB; SUBMILLIMETER; CAMERA; TEMPERATURE;

D O I：

10.1088/0004-637X/719/2/1045

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report cosmic microwave background (CMB) power-spectrum measurements from the first 100 deg(2) field observed by the South Pole Telescope (SPT) at 150 and 220 GHz. On angular scales where the primary CMB anisotropy is dominant, l less than or similar to 3000, the SPT power spectrum is consistent with the standard Lambda CDM cosmology. On smaller scales, we see strong evidence for a point-source contribution, consistent with a population of dusty, star-forming galaxies. After we mask bright point sources, anisotropy power on angular scales of 3000 < l < 9500 is detected with a signal-to-noise ratio greater than or similar to 50 at both frequencies. We combine the 150 and 220 GHz data to remove the majority of the point-source power and use the point-source-subtracted spectrum to detect Sunyaev-Zel'dovich (SZ) power at 2.6 sigma. At l = 3000, the SZ power in the subtracted bandpowers is 4.2 +/- 1.5 mu K-2, which is significantly lower than the power predicted by a fiducial model using WMAP5 cosmological parameters. This discrepancy may suggest that contemporary galaxy cluster models overestimate the thermal pressure of intracluster gas. Alternatively, this result can be interpreted as evidence for lower values of sigma(8). When combined with an estimate of the kinetic SZ contribution, the measured SZ amplitude shifts sigma(8) from the primary CMB anisotropy derived constraint of 0.794 +/- 0.028 down to 0.773 +/- 0.025. The uncertainty in the constraint on sigma(8) from this analysis is dominated by uncertainties in the theoretical modeling required to predict the amplitude of the SZ power spectrum for a given set of cosmological parameters.

引用

页码：1045 / 1066

页数：22

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