MASS CALIBRATION AND COSMOLOGICAL ANALYSIS OF THE SPT-SZ GALAXY CLUSTER SAMPLE USING VELOCITY DISPERSION σv AND X-RAY YX MEASUREMENTS

被引:130
作者
Bocquet, S. [1 ,2 ]
Saro, A. [1 ]
Mohr, J. J. [1 ,2 ,3 ]
Aird, K. A. [4 ]
Ashby, M. L. N. [5 ]
Bautz, M. [6 ]
Bayliss, M. [5 ,7 ]
Bazin, G. [1 ]
Benson, B. A. [8 ,9 ,10 ]
Bleem, L. E. [9 ,11 ,12 ]
Brodwin, M. [13 ]
Carlstrom, J. E. [9 ,10 ,11 ,12 ,14 ]
Chang, C. L. [9 ,12 ,14 ]
Chiu, I. [1 ]
Cho, H. M. [15 ]
Clocchiatti, A. [16 ]
Crawford, T. M. [9 ,10 ]
Crites, A. T. [9 ,10 ,17 ]
Desai, S. [1 ,2 ]
de Haan, T. [18 ]
Dietrich, J. P. [1 ,2 ]
Dobbs, M. A. [18 ]
Foley, R. J. [5 ,19 ,20 ]
Forman, W. R. [5 ]
Gangkofner, D. [1 ,2 ]
George, E. M. [21 ]
Gladders, M. D. [9 ,10 ]
Gonzalez, A. H. [22 ]
Halverson, N. W. [23 ,24 ]
Hennig, C. [1 ]
Hlavacek-Larrondo, J. [25 ,26 ]
Holder, G. P. [18 ]
Holzapfel, W. L. [21 ]
Hrubes, J. D. [4 ]
Jones, C. [5 ]
Keisler, R. [9 ,11 ]
Knox, L. [27 ]
Lee, A. T. [21 ,28 ]
Leitch, E. M. [9 ,10 ]
Liu, J. [1 ,2 ]
Lueker, M. [17 ,21 ]
Luong-Van, D. [4 ]
Marrone, D. P. [29 ]
McDonald, M. [6 ]
McMahon, J. J. [30 ]
Meyer, S. S. [9 ,10 ,11 ,14 ]
Mocanu, L. [9 ,10 ]
Murray, S. S. [5 ]
Padin, S. [9 ,10 ,17 ]
Pryke, C. [31 ]
机构
[1] Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany
[2] Excellence Cluster Univ, D-85748 Garching, Germany
[3] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany
[4] Univ Chicago, Chicago, IL 60637 USA
[5] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[6] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA
[7] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA
[8] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA
[9] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA
[10] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA
[11] Univ Chicago, Dept Phys, Chicago, IL 60637 USA
[12] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA
[13] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA
[14] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA
[15] NIST, Quantum Devices Grp, Boulder, CO 80305 USA
[16] Pontificia Univ Catolica Chile, Dept Astron & Astrosif, Santiago, Chile
[17] CALTECH, Pasadena, CA 91125 USA
[18] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada
[19] Univ Illinois, Dept Astron, Urbana, IL 61801 USA
[20] Univ Illinois, Dept Phys, Urbana, IL 61801 USA
[21] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[22] Univ Florida, Dept Astron, Gainesville, FL 32611 USA
[23] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA
[24] Univ Colorado, Dept Phys, Boulder, CO 80309 USA
[25] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA
[26] Stanford Univ, Dept Phys, Stanford, CA 94305 USA
[27] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA
[28] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA
[29] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA
[30] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA
[31] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA
[32] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia
[33] Space Telescope Sci Inst, Baltimore, MD 21218 USA
[34] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA
[35] Sch Art, Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA
[36] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA
[37] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada
[38] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada
[39] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA
[40] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA
[41] Cerro Tololo Interamer Observ, La Serena, Chile
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; BARYON ACOUSTIC-OSCILLATIONS; HUBBLE-SPACE-TELESCOPE; 720 SQUARE DEGREES; OBSERVED GROWTH; CONSTRAINTS; RELEASE; CHANDRA; DEG(2); SIMULATIONS; CATALOG;
D O I
10.1088/0004-637X/799/2/214
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present a velocity-dispersion-based mass calibration of the South Pole Telescope Sunyaev-Zel'dovich effect survey (SPT-SZ) galaxy cluster sample. Using a homogeneously selected sample of 100 cluster candidates from 720 deg(2) of the survey along with 63 velocity dispersion (sigma(v)) and 16 X-ray Y-X measurements of sample clusters, we simultaneously calibrate the mass-observable relation and constrain cosmological parameters. Our method accounts for cluster selection, cosmological sensitivity, and uncertainties in the mass calibrators. The calibrations using sigma(v) and Y-X are consistent at the 0.6 sigma level, with the sigma(v) calibration preferring similar to 16% higher masses. We use the full SPTCL data set (SZ clusters+sigma(v)+Y-X) to measure sigma(8)(Omega(m)/0.27)(0.3) = 0.809 +/- 0.036 within a flat ACDM model. The SPT cluster abundance is lower than preferred by either the WMAP9 or Planck+WMAP9 polarization (WP) data, but assuming that the sum of the neutrino masses is Sigma m(upsilon) = 0.06 eV, we find the data sets to be consistent at the 1.0 sigma level for WMAP9 and 1.5 sigma for Planck+WP. Allowing for larger Sigma m(upsilon) further reconciles the results. When we combine the SPTCL and Planck+WP data sets with information from baryon acoustic oscillations and Type Ia supernovae, the preferred cluster masses are 1.9 sigma higher than the Y-X calibration and 0.8 sigma higher than the sigma(v) calibration. Given the scale of these shifts (similar to 44% and similar to 23% in mass, respectively), we execute a goodness-of-fit test; it reveals no tension, indicating that the best-fit model provides an adequate description of the data. Using the multi-probe data set, we measure Omega(m) = 0.299 +/- 0.009 and sigma(8) = 0.829 +/- 0.011. Within upsilon CDM model we find Sigma m(upsilon) = 0.148 +/- 0.081 eV. We present a consistency test of the cosmic growth rate using SPT clusters. Allowing both the growth index gamma and the dark energy equation-of-state parameter w to vary, we find gamma = 0.73 +/- 0.28 and w = -1.007 +/- 0.065, demonstrating that the expansion and the growth histories are consistent with ACDM universe (gamma = 0.55; w = -1).
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