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

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 799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; 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).

引用

页数：16

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