IMPROVED CONSTRAINTS ON COSMIC MICROWAVE BACKGROUND SECONDARY ANISOTROPIES FROM THE COMPLETE 2008 SOUTH POLE TELESCOPE DATA

被引：83

作者：

Shirokoff, E. ^{[1
]}

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

Shaw, L. ^{[2
]}

Millea, M. ^{[3
]}

Ade, P. A. R. ^{[4
]}

Aird, K. A.

Benson, B. A. ^{[1
,5
,6
]}

Bleem, L. E. ^{[5
,7
]}

Carlstrom, J. E. ^{[5
,6
,7
,8
]}

Chang, C. L. ^{[5
,6
]}

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

Crawford, T. M. ^{[5
,8
]}

Crites, A. T. ^{[5
,8
]}

de Haan, T. ^{[10
]}

Dobbs, M. A. ^{[10
]}

Dudley, J. ^{[10
]}

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

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

Holder, G. P. ^{[10
]}

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

Hrubes, J. D.

Joy, M. ^{[13
]}

Keisler, R. ^{[5
,7
]}

Knox, L. ^{[3
]}

Lee, A. T. ^{[1
,14
]}

Leitch, E. M. ^{[5
,8
]}

Lueker, M. ^{[15
]}

Luong-Van, D.

McMahon, J. J. ^{[5
,6
,16
]}

Mehl, J. ^{[5
]}

Meyer, S. S. ^{[5
,6
,7
,8
]}

Mohr, J. J. ^{[17
,18
,19
]}

Montroy, T. E. ^{[20
]}

Padin, S. ^{[5
,8
,15
]}

Plagge, T. ^{[5
,8
]}

Pryke, C. ^{[5
,6
,8
]}

Ruhl, J. E. ^{[20
]}

Schaffer, K. K. ^{[5
,6
,21
]}

Spieler, H. G. ^{[14
]}

Staniszewski, Z. ^{[20
]}

Stark, A. A. ^{[22
]}

Story, K. ^{[5
,7
]}

Vanderlinde, K. ^{[10
]}

Vieira, J. D. ^{[15
]}

Williamson, R. ^{[8
]}

Zahn, O. ^{[23
,24
]}

机构：

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[15] CALTECH, Pasadena, CA 91125 USA

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

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

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 736卷 / 01期

基金：

美国国家科学基金会;

关键词：

cosmic background radiation; cosmology: observations; large-scale structure of universe; ATACAMA COSMOLOGY TELESCOPE; ANGULAR POWER SPECTRUM; DUST EMISSION; GAS MOTIONS; PROBE; SIMULATIONS; RADIATION; CLUSTERS; CMB; REIONIZATION;

D O I：

10.1088/0004-637X/736/1/61

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report measurements of the cosmic microwave background (CMB) power spectrum from the complete 2008 South Pole Telescope (SPT) data set. We analyze twice as much data as the first SPT power spectrum analysis, using an improved cosmological parameter estimator which fits multi-frequency models to the SPT 150 and 220 GHz bandpowers. We find an excellent fit to the measured bandpowers with a model that includes lensed primary CMB anisotropy, secondary thermal (tSZ) and kinetic (kSZ) Sunyaev-Zel'dovich anisotropies, unclustered synchrotron point sources, and clustered dusty point sources. In addition to measuring the power spectrum of dusty galaxies at high signal-to-noise, the data primarily constrain a linear combination of the kSZ and tSZ anisotropy contributions at 150 GHz and l = 3000: D-3000(tSZ) + 0.5 D-3000(kSZ) = 4.5 +/- 1.0 mu K-2. The 95% confidence upper limits on secondary anisotropy power are D-3000(tSZ) < 5.3 mu K-2 and D-3000(kSZ) < 6.5 mu K-2. We also consider the potential correlation of dusty and tSZ sources and find it incapable of relaxing the tSZ upper limit. These results increase the significance of the lower than expected tSZ amplitude previously determined from SPT power spectrum measurements. We find that models including non-thermal pressure support in groups and clusters predict tSZ power in better agreement with the SPT data. Combining the tSZ power measurement with primary CMB data halves the statistical uncertainty on sigma(8). However, the preferred value of sigma(8) varies significantly between tSZ models. Improved constraints on cosmological parameters from tSZ power spectrum measurements require continued progress in the modeling of the tSZ power.

引用

页数：21

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