CLASH: THE CONCENTRATION-MASS RELATION OF GALAXY CLUSTERS

被引：159

作者：

Merten, J. ^{[1
,2
,3
]}

Meneghetti, M. ^{[1
,4
,5
]}

Postman, M. ^{[6
]}

Umetsu, K. ^{[7
]}

Zitrin, A. ^{[2
,32
]}

Medezinski, E. ^{[8
]}

Nonino, M. ^{[9
]}

Koekemoer, A. ^{[6
]}

Melchior, P. ^{[10
,11
]}

Gruen, D. ^{[12
,13
]}

Moustakas, L. A. ^{[1
]}

Bartelmann, M. ^{[14
]}

Host, O. ^{[15
]}

Donahue, M. ^{[16
]}

Coe, D. ^{[6
]}

Molino, A. ^{[17
]}

Jouvel, S. ^{[18
,19
]}

Monna, A. ^{[12
,13
]}

Seitz, S. ^{[12
,13
]}

Czakon, N. ^{[7
]}

Lemze, D. ^{[8
]}

Sayers, J. ^{[2
]}

Balestra, I. ^{[9
,20
]}

Rosati, P. ^{[21
]}

Benitez, N. ^{[16
]}

Biviano, A. ^{[9
]}

Bouwens, R. ^{[22
]}

Bradley, L. ^{[6
]}

Broadhurst, T. ^{[23
,24
]}

Carrasco, M. ^{[14
,25
]}

Ford, H. ^{[8
]}

Grillo, C. ^{[15
]}

Infante, L. ^{[26
]}

Kelson, D. ^{[27
]}

Lahav, O. ^{[18
]}

Massey, R. ^{[28
]}

Moustakas, J. ^{[29
]}

Rasia, E. ^{[30
]}

Rhodes, J. ^{[1
,2
]}

Vega, J. ^{[31
,32
]}

Zheng, W. ^{[6
]}

机构：

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

[2] CALTECH, Pasadena, CA 91125 USA

[3] Univ Oxford, Dept Phys, Oxford OX1 3RH, England

[4] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy

[5] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy

[6] Space Telescope Sci Inst, Baltimore, MD 21208 USA

[7] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan

[8] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[9] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy

[10] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[11] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[12] Univ Munich, D-81679 Munich, Germany

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

[14] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany

[15] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark

[16] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA

[17] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain

[18] CSIC, IEEC, Inst Ciencies Espai, E-08193 Bellaterra, Barcelona, Spain

[19] UCL, Dept Phys & Astron, London WC1E 6BT, England

[20] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy

[21] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy

[22] Leiden Univ, Leiden Observ, NL-2333 Leiden, Netherlands

[23] Univ Basque Country, UPV EHU, Dept Theoret Phys & Hist Sci, E-48080 Bilbao, Spain

[24] Basque Fdn Sci, Ikerbasque, Santiago 48011, Chile

[25] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofs, Santiago 22, Chile

[26] Pontificia Univ Catolica Chile, Ctr Astroingn, Dept Astron & Astrofis, Santiago, Chile

[27] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA

[28] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England

[29] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA

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

[31] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain

[32] Observ Paris, CNRS, LERMA, UMR 8112, F-75014 Paris, France

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 806卷 / 01期

基金：

美国国家科学基金会;

关键词：

dark matter; galaxies: clusters: general; gravitational lensing: strong; gravitational lensing: weak; HUBBLE-SPACE-TELESCOPE; WEAK-LENSING ANALYSIS; EARLY DARK ENERGY; ACT-CL J0102-4915; X-RAY; MERGING CLUSTER; ADVANCED CAMERA; PHOTOMETRIC REDSHIFTS; HALO CONCENTRATIONS; DENSITY PROFILE;

D O I：

10.1088/0004-637X/806/1/4

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a new determination of the concentration-mass (c-M) relation for galaxy clusters based on our comprehensive lensing analysis of 19 X-ray selected galaxy clusters from the Cluster Lensing and Supernova Survey with Hubble (CLASH). Our sample spans a redshift range between 0.19 and 0.89. We combine weak-lensing constraints from the Hubble Space Telescope (HST) and from ground-based wide-field data with strong lensing constraints from HST. The results are reconstructions of the surface-mass density for all CLASH clusters on multi-scale grids. Our derivation of Navarro-Frenk-White parameters yields virial masses between 0.53 x 10(15) M-circle dot/h and 1.76 x 10(15) M-circle dot/h and the halo concentrations are distributed around c(200c) similar to 3.7 with a 1 sigma significant negative slope with cluster mass. We find an excellent 4% agreement in the median ratio of our measured concentrations for each cluster and the respective expectation from numerical simulations after accounting for the CLASH selection function based on X-ray morphology. The simulations are analyzed in two dimensions to account for possible biases in the lensing reconstructions due to projection effects. The theoretical c-M relation from our X-ray selected set of simulated clusters and the c-M relation derived directly from the CLASH data agree at the 90% confidence level.

引用

页数：26

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