The Fraction of Cool-core Clusters in X-Ray versus SZ Samples Using Chandra Observations

被引：79

作者：

Andrade-Santos, Felipe ^{[1
]}

Jones, Christine ^{[1
]}

Forman, William R. ^{[1
]}

Lovisari, Lorenzo ^{[1
]}

Vikhlinin, Alexey ^{[1
]}

van Weeren, Reinout J. ^{[1
]}

Murray, Stephen S. ^{[1
]}

Arnaud, Monique ^{[2
]}

Pratt, Gabriel W. ^{[2
]}

Democles, Jessica ^{[2
]}

Kraft, Ralph ^{[1
]}

Mazzotta, Pasquale ^{[1
,3
]}

Boehringer, Hans ^{[4
]}

Chon, Gayoung ^{[4
]}

Giacintucci, Simona ^{[5
]}

Clarke, Tracy E. ^{[6
]}

Borgani, Stefano ^{[7
,8
]}

David, Larry ^{[1
]}

Douspis, Marian ^{[9
]}

Pointecouteau, Etienne ^{[10
,11
]}

Dahle, Hakon ^{[12
]}

Brown, Shea ^{[13
]}

Aghanim, Nabila ^{[14
]}

Rasia, Elena ^{[8
]}

机构：

[1] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[2] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS INSU,CEA Saclay, F-91191 Gif Sur Yvette, France

[3] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy

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

[5] Naval Res Lab, 4555 Overlook Ave SW,Code 7213, Washington, DC 20375 USA

[6] US Naval Res Lab, Code 7213,4555 Overlook Ave SW, Washington, DC 20375 USA

[7] Univ Trieste, Dipartimento Fis, Sez Astron, Via Tiepolo 11, I-34131 Trieste, Italy

[8] INAF, Osservatorio Astron Trieste, Via Tiepolo 11, I-34131 Trieste, Italy

[9] Univ Paris Sud 11, CNRS, Inst Astrophys Spatiale, UMR8617, Batiment 121, Orsay, France

[10] CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France

[11] Univ Toulouse, UPS OMP, IRAP, Toulouse, France

[12] Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway

[13] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52245 USA

[14] Univ Paris Saclay, Univ Paris Sud, CNRS, Inst Astrophys Spatiale, Bat 121, F-91405 Orsay, France

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 843卷 / 01期

基金：

美国国家科学基金会; 欧洲研究理事会;

关键词：

galaxies: clusters: general; large-structure of universe; RELAXED GALAXY CLUSTERS; XMM-NEWTON OBSERVATIONS; COSMOLOGICAL CONSTRAINTS; MASS FUNCTION; TEMPERATURE RELATION; HIGH-RESOLUTION; EVOLUTION; GAS; FLOWS; SIMULATIONS;

D O I：

10.3847/1538-4357/aa7461

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We derive and compare the fractions of cool-core clusters in the Planck Early Sunyaev-Zel'dovich sample of 164 clusters with z <= 0.35 and in a flux-limited X-ray sample of 100 clusters with z <= 0.30, using Chandra observations. We use four metrics to identify cool-core clusters: (1) the concentration parameter, which is the ratio of the integrated emissivity profile within 0.15 r(500) to that within r(500); (2) the ratio of the integrated emissivity profile within 40 kpc to that within 400 kpc; (3) the cuspiness of the gas density profile, which is the negative of the logarithmic derivative of the gas density with respect to the radius, measured at 0.04 r(500); and (4) the central gas density, measured at 0.01 r(500). We find that the sample of X-ray-selected clusters, as characterized by each of these metrics, contains a significantly larger fraction of cool-core clusters compared to the sample of SZ-selected clusters (44% +/- 7% versus 28% +/- 4% using the concentration parameter in the 0.15-1.0 r(500) range, 61% +/- 8% versus 36% +/- 5% using the concentration parameter in the 40-400 kpc range, 64% +/- 8% versus 38% +/- 5% using the cuspiness, and 53% +/- 7% versus 39 +/- 5% using the central gas density). Qualitatively, cool-core clusters are more X-ray luminous at fixed mass. Hence, our X-ray, flux-limited sample, compared to the approximately mass-limited SZ sample, is overrepresented with cool-core clusters. We describe a simple quantitative model that uses the excess luminosity of cool-core clusters compared to non-cool-core clusters at fixed mass to successfully predict the observed fraction of cool-core clusters in X-ray-selected samples.

引用

页数：11

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