COSMOLOGICAL CONSTRAINTS FROM SUNYAEV-ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg2 OF THE SOUTH POLE TELESCOPE SURVEY

被引：206

作者：

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

de Haan, T. ^{[3
]}

Dudley, J. P. ^{[3
]}

Reichardt, C. L. ^{[4
]}

Aird, K. A.

Andersson, K. ^{[5
,6
]}

Armstrong, R. ^{[7
]}

Ashby, M. L. N. ^{[8
]}

Bautz, M. ^{[6
]}

Bayliss, M. ^{[9
]}

Bazin, G. ^{[5
,10
]}

Bleem, L. E. ^{[1
,11
]}

Brodwin, M. ^{[12
]}

Carlstrom, J. E. ^{[1
,2
,11
,13
,14
,24
]}

Chang, C. L. ^{[1
,2
,14
]}

Cho, H. M. ^{[15
]}

Clocchiatti, A. ^{[16
]}

Crawford, T. M. ^{[1
,13
,24
]}

Crites, A. T. ^{[1
,13
,24
]}

Desai, S. ^{[5
,10
]}

Dobbs, M. A. ^{[3
]}

Foley, R. J. ^{[8
]}

Forman, W. R. ^{[8
]}

George, E. M. ^{[4
]}

Gladders, M. D. ^{[1
,13
,24
]}

Gonzalez, A. H. ^{[17
]}

Halverson, N. W. ^{[18
,19
]}

Harrington, N. ^{[4
]}

High, F. W. ^{[1
,13
,24
]}

Holder, G. P. ^{[3
]}

Holzapfel, W. L. ^{[4
]}

Hoover, S. ^{[1
,2
]}

Hrubes, J. D.

Jones, C. ^{[8
]}

Joy, M. ^{[20
]}

Keisler, R. ^{[1
,11
]}

Knox, L. ^{[21
]}

Lee, A. T. ^{[4
,22
]}

Leitch, E. M. ^{[1
,13
,24
]}

Liu, J. ^{[5
,10
]}

Lueker, M. ^{[4
,23
]}

Luong-Van, D.

Mantz, A. ^{[1
]}

Marrone, D. P. ^{[13
,24
]}

McDonald, M. ^{[6
]}

McMahon, J. J. ^{[1
,2
,25
]}

Mehl, J. ^{[1
,13
,24
]}

Meyer, S. S. ^{[1
,2
,11
,13
,24
]}

Mocanu, L. ^{[1
,13
,24
]}

Mohr, J. J. ^{[5
,10
,26
]}

机构：

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

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

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

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

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

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

[7] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA

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

[9] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA

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

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

[12] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA

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

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

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

[16] PUC, Dept Astron & Astrofs, Santiago 22, Chile

[17] Univ Florida, Dept Astron, Gainesville, FL 32611 USA

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

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

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

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

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

[23] CALTECH, Pasadena, CA 91125 USA

[24] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

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

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

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

[28] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA

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

[30] Space Telescope Sci Inst, Baltimore, MD 21218 USA

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

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

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 763卷 / 02期

基金：

美国国家科学基金会;

关键词：

cosmic background radiation; cosmology: observations; galaxies: clusters: general; large-scale structure of universe; MASSIVE GALAXY CLUSTERS; MICROWAVE BACKGROUND ANISOTROPIES; HUBBLE-SPACE-TELESCOPE; WEAK-LENSING MASSES; OBSERVED GROWTH; STAR-FORMATION; SIMULATIONS; PRECISION; EVOLUTION; ENERGY;

D O I：

10.1088/0004-637X/763/2/147

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We usemeasurements from the South Pole Telescope (SPT) Sunyaev-Zel'dovich (SZ) cluster survey in combination with X-ray measurements to constrain cosmological parameters. We present a statistical method that fits for the scaling relations of the SZ and X-ray cluster observables with mass while jointly fitting for cosmology. The method is generalizable to multiple cluster observables, and self-consistently accounts for the effects of the cluster selection and uncertainties in cluster mass calibration on the derived cosmological constraints. We apply this method to a data set consisting of an SZ-selected catalog of 18 galaxy clusters at z > 0.3 from the first 178 deg(2) of the 2500 deg(2) SPT-SZ survey, with 14 clusters having X-ray observations from either Chandra or XMM-Newton. Assuming a spatially flat Lambda CDM cosmological model, we find the SPT cluster sample constrains sigma(8)(Omega(m)/0.25)(0.30) = 0.785 +/- 0.037. In combination with measurements of the cosmic microwave background (CMB) power spectrum from the SPT and the seven-year Wilkinson Microwave Anisotropy Probe data, the SPT cluster sample constrains sigma(8) = 0.795 +/- 0.016 and Omega(m) = 0.255 +/- 0.016, a factor of 1.5 improvement on each parameter over the CMB data alone. We consider several extensions beyond the Lambda CDM model by including the following as free parameters: the dark energy equation of state (w), the sum of the neutrino masses (Sigma m(nu)), the effective number of relativistic species (N-eff), and a primordial non-Gaussianity (f(NL)). We find that adding the SPT cluster data significantly improves the constraints on w and Sigma m(nu) beyond those found when using measurements of the CMB, supernovae, baryon acoustic oscillations, and the Hubble constant. Considering each extension independently, we best constrain w = -0.973 +/- 0.063 and the sum of neutrino masses Sigma m(nu) < 0.28 eV at 95% confidence, a factor of 1.25 and 1.4 improvement, respectively, over the constraints without clusters. Assuming a Lambda CDM model with a free N-eff and Sigma m(nu), we measure N-eff = 3.91 +/- 0.42 and constrain Sigma m(nu) < 0.63 eV at 95% confidence. We also use the SPT cluster sample to constrain f(NL) = -220 +/- 317, consistent with zero primordial non-Gaussianity. Finally, we discuss the current systematic limitations due to the cluster mass calibration, and future improvements for the recently completed 2500 deg(2) SPT-SZ survey. The survey has detected similar to 500 clusters with a median redshift of similar to 0.5 and a median mass of similar to 2.3 x 10(14) M-circle dot h(-1) and, when combined with an improved cluster mass calibration and existing external cosmological data sets will significantly improve constraints on w.

引用

页数：21

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