GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV-ZEL'DOVICH EFFECT IN THE FIRST 720 SQUARE DEGREES OF THE SOUTH POLE TELESCOPE SURVEY

被引：241

作者：

Reichardt, C. L. ^{[32
]}

Stalder, B. ^{[1
]}

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

Montroy, T. E. ^{[4
]}

Aird, K. A.

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

Armstrong, R. ^{[7
]}

Ashby, M. L. N. ^{[1
]}

Bautz, M. ^{[6
]}

Bayliss, M. ^{[8
]}

Bazin, G. ^{[5
,9
]}

Benson, B. A. ^{[2
,10
]}

Brodwin, M. ^{[11
]}

Carlstrom, J. E. ^{[2
,3
,10
,12
,13
]}

Chang, C. L. ^{[2
,10
,13
]}

Cho, H. M. ^{[14
]}

Clocchiatti, A. ^{[15
]}

Crawford, T. M. ^{[2
,12
]}

Crites, A. T. ^{[2
,12
]}

de Haan, T. ^{[16
]}

Desai, S. ^{[5
,9
]}

Dobbs, M. A. ^{[16
]}

Dudley, J. P. ^{[16
]}

Foley, R. J. ^{[1
]}

Forman, W. R. ^{[1
]}

George, E. M.

Gladders, M. D. ^{[2
,12
]}

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

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

Harrington, N. L.

High, F. W. ^{[2
,12
]}

Holder, G. P. ^{[16
]}

Holzapfel, W. L.

Hoover, S. ^{[2
,10
]}

Hrubes, J. D.

Jones, C. ^{[1
]}

Joy, M. ^{[20
]}

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

Knox, L. ^{[21
]}

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

Leitch, E. M. ^{[2
,12
]}

Liu, J. ^{[5
,9
]}

Lueker, M. ^{[23
]}

Luong-Van, D.

Mantz, A. ^{[2
]}

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

McDonald, M. ^{[6
]}

McMahon, J. J. ^{[2
,10
,25
]}

Mehl, J. ^{[2
,12
]}

Meyer, S. S. ^{[2
,3
,10
,12
]}

机构：

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

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

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

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

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

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

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

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

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

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

[11] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA

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

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

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

[15] PUC, Dept Astron & Astrofis, Santiago 22, Chile

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

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

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

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

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

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

[32] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 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: individual; large-scale structure of universe; MICROWAVE BACKGROUND ANISOTROPIES; ALL-SKY SURVEY; BLANCO COSMOLOGY SURVEY; HUBBLE-SPACE-TELESCOPE; RICH CLUSTERS; DATA RELEASE; CATALOG; CONSTRAINTS; REDSHIFTS; SAMPLE;

D O I：

10.1088/0004-637X/763/2/127

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a catalog of galaxy cluster candidates, selected through their Sunyaev-Zel'dovich (SZ) effect signature in the first 720 deg(2) of the South Pole Telescope (SPT) survey. This area was mapped with the SPT in the 2008 and 2009 austral winters to a depth of similar to 18 mu K-CMB-arcmin at 150 GHz; 550 deg(2) of it was also mapped to similar to 44 mu K-CMB-arcmin at 95 GHz. Based on optical imaging of all 224 candidates and near-infrared imaging of the majority of candidates, we have found optical and/or infrared counterparts for 158, which we then classify as confirmed galaxy clusters. Of these 158 clusters, 135 were first identified as clusters in SPT data, including 117 new discoveries reported in this work. This catalog triples the number of confirmed galaxy clusters discovered through the SZ effect. We report photometrically derived (and in some cases spectroscopic) redshifts for confirmed clusters and redshift lower limits for the remaining candidates. The catalog extends to high redshift with a median redshift of z = 0.55 and maximum confirmed redshift of z = 1.37. Forty-five of the clusters have counterparts in the ROSAT bright or faint source catalogs from which we estimate X-ray fluxes. Based on simulations, we expect the catalog to be nearly 100% complete above M-500 approximate to 5 x 10(14) M-circle dot h(70)(-1) at z greater than or similar to 0.6. There are 121 candidates detected at signal-to-noise ratio greater than five, at which the catalog purity is measured to be 95%. From this high-purity subsample, we exclude the z < 0.3 clusters and use the remaining 100 candidates to improve cosmological constraints following the method presented by Benson et al. Adding the cluster data to CMB + BAO + H-0 data leads to a preference for non-zero neutrino masses while only slightly reducing the upper limit on the sum of neutrino masses to Sigma m(nu) < 0.38 eV (95% CL). For a spatially flat wCDM cosmological model, the addition of this catalog to the CMB + BAO + H-0 + SNe results yields sigma(8) = 0.807 +/- 0.027 and w = -1.010 +/- 0.058, improving the constraints on these parameters by a factor of 1.4 and 1.3, respectively. The larger cluster catalog presented in this work leads to slight improvements in cosmological constraints from those presented by Benson et al. These cosmological constraints are currently limited by uncertainty in the cluster mass calibration, not the size or quality of the cluster catalog. A multi-wavelength observation program to improve the cluster mass calibration will make it possible to realize the full potential of the final 2500 deg(2) SPT cluster catalog to constrain cosmology.

引用

页数：20

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