CONSTRAINTS ON COSMOLOGY FROM THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM OF THE 2500 deg2 SPT-SZ SURVEY

被引：180

作者：

Hou, Z. ^{[1
]}

Reichardt, C. L. ^{[2
]}

Story, K. T. ^{[3
,4
]}

Follin, B. ^{[1
]}

Keisler, R. ^{[3
,4
]}

Aird, K. A. ^{[5
]}

Benson, B. A. ^{[3
,6
]}

Bleem, L. E. ^{[3
,4
]}

Carlstrom, J. E. ^{[3
,4
,6
,7
,8
]}

Chang, C. L. ^{[3
,6
,8
]}

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

Crawford, T. M. ^{[3
,7
]}

Crites, A. T. ^{[3
,7
]}

De Haan, T. ^{[10
]}

De Putter, R. ^{[11
,12
]}

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

Dodelson, S. ^{[3
,7
,13
]}

Dudley, J. ^{[10
]}

George, E. M. ^{[2
]}

Halverson, N. W. ^{[14
,15
]}

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

Holzapfel, W. L. ^{[2
]}

Hoover, S. ^{[3
,4
]}

Hrubes, J. D. ^{[5
]}

Joy, M. ^{[16
]}

Knox, L. ^{[1
]}

Lee, A. T. ^{[2
,17
]}

Leitch, E. M. ^{[3
,7
]}

Lueker, M. ^{[13
]}

Luong-Van, D. ^{[5
]}

McMahon, J. J. ^{[18
]}

Mehl, J. ^{[3
,8
]}

Meyer, S. S. ^{[3
,4
,6
,7
]}

Millea, M. ^{[1
]}

Mohr, J. J. ^{[19
,20
,21
]}

Montroy, T. E. ^{[22
]}

Padin, S. ^{[3
,4
,7
]}

Plagge, T. ^{[3
,7
]}

Pryke, C. ^{[3
,7
,23
]}

Ruhl, J. E. ^{[22
]}

Sayre, J. T. ^{[22
]}

Schaffer, K. K. ^{[3
,6
,24
]}

Shaw, L. ^{[10
]}

Shirokoff, E. ^{[2
]}

Spieler, H. G. ^{[17
]}

Staniszewski, Z. ^{[22
]}

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

Van Engelen, A. ^{[10
]}

Vanderlinde, K. ^{[10
]}

Vieira, J. D. ^{[13
]}

机构：

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

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

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

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

[5] Univ Chicago, Chicago, IL 60637 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] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

[11] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[12] CALTECH, Pasadena, CA 91125 USA

[13] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA

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

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

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

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

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

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

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

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

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

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

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

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

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

[27] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

来源：

ASTROPHYSICAL JOURNAL | 2014年 / 782卷 / 02期

基金：

美国国家科学基金会;

关键词：

cosmic background radiation; cosmological parameters; early universe; inflation; BARYON ACOUSTIC-OSCILLATIONS; 720 SQUARE DEGREES; PRIMORDIAL NUCLEOSYNTHESIS; PRECISION COSMOLOGY; HELIUM ABUNDANCE; GALAXY CLUSTERS; CENT DISTANCE; DAMPING TAIL; DARK ENERGY; ANISOTROPY;

D O I：

10.1088/0004-637X/782/2/74

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We explore extensions to the Lambda CDM cosmology using measurements of the cosmic microwave background (CMB) from the recent SPT-SZ survey, along with data from WMAP7 and measurements of H-0 and baryon acoustic oscillation (BAO). We check for consistency within Lambda CDM between these data sets, and find some tension. The CMB alone gives weak support to physics beyond Lambda CDM, due to a slight trend relative to Lambda CDM of decreasing power toward smaller angular scales. While it may be due to statistical fluctuation, this trend could also be explained by several extensions. We consider running of the primordial spectral index (dn(s)/d ln k), as well as two extensions that modify the damping tail power (the primordial helium abundance Y-p and the effective number of neutrino species N-eff) and one that modifies the large-scale power due to the integrated Sachs-Wolfe effect (the sum of neutrino masses Sigma m(nu)). These extensions have similar observational consequences and are partially degenerate when considered simultaneously. Of the six one-parameter extensions considered, we find CMB to have the largest preference for dn(s)/d ln k with -0.046 < dn(s)/d lnk < -0.003 at 95% confidence, which strengthens to a 2.7 sigma indication of dn(s)/d lnk < 0 from CMB+BAO+H-0. Detectable dn(s)/d ln k not equal 0 is difficult to explain in the context of single-field, slow-roll inflation models. We find N-eff = 3.62 +/- 0.48 for the CMB, which tightens to N-eff = 3.71 +/- 0.35 from CMB+BAO+H-0. Larger values of N-eff relieve the mild tension between CMB, BAO, and H-0. When the Sunyaev-Zel'dovich selected galaxy cluster abundances (SPTCL) data are also included, we obtain N-eff = 3.29 +/- 0.31. Allowing for Sigma m(nu) gives a 3.0s detection of Sigma m(nu) > 0 from CMB+BAO+H-0 +SPTCL. The median value is (0.32+/-0.11) eV, a factor of six above the lower bound set by neutrino oscillation observations. All data sets except H-0 show some preference for massive neutrinos; data combinations including H-0 favor nonzero masses only if BAO data are also included. We also constrain the two-parameter extensions N-eff + Sigma m(nu) and N-eff + Y-p to explore constraints on additional light species and big bang nucleosynthesis, respectively.

引用

页数：24

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