A census of cool-core galaxy clusters in IllustrisTNG

被引：74

作者：

Barnes, David J. ^{[1
,2
]}

Vogelsberger, Mark ^{[1
]}

Kannan, Rahul ^{[1
,3
]}

Marinacci, Federico ^{[1
]}

Weinberger, Rainer ^{[4
]}

Springel, Volker ^{[4
,5
,6
]}

Torrey, Paul ^{[1
]}

Pillepich, Annalisa ^{[7
]}

Nelson, Dylan ^{[6
]}

Pakmor, Ruediger ^{[4
]}

Naiman, Jill ^{[3
]}

Hernquist, Lars ^{[3
]}

McDonald, Michael ^{[1
]}

机构：

[1] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[2] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astnmorny, Manchester M13 9PL, Lancs, England

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

[4] Heidelbetg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany

[5] Heidelberg Univ, Zentrum Astron, ARI, Monchhofstr 12-14, D-69120 Heidelberg, Germany

[6] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany

[7] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2018年 / 481卷 / 02期

基金：

欧洲研究理事会;

关键词：

methods: numerical; galaxies: clusters: general; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters; MATTER HALO CONCENTRATIONS; RHAPSODY-G SIMULATIONS; COSMOLOGICAL SIMULATIONS; INTRACLUSTER MEDIUM; THERMAL-INSTABILITY; MAGNETIC-FIELDS; HOT GAS; EVOLUTION; DARK; FEEDBACK;

D O I：

10.1093/mnras/sty2078

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The thermodynamic structure of hot gas in galaxy clusters is sensitive to astrophysical processes and typically difficult to model with galaxy formation simulations. We explore the fraction of cool-core (CC) clusters in a large sample of 370 clusters from IllustrisTNG, examining six common CC definitions. IllustrisTNG produces continuous CC criteria distributions, the extremes of which are classified as CC and non-cool core (NCC), and the criteria are increasingly correlated for more massive clusters. At z = 0, the CC fractions for two criteria are in reasonable agreement with the observed fractions but the other four CC fractions are lower than observed. This result is partly driven by systematic differences between the simulated and observed gas fraction profiles. The simulated CC fractions with redshift show tentative agreement with the observed fractions, but linear fits demonstrate that the simulated evolution is steeper than observed. The conversion of CCs to NCCs appears to begin later and act more rapidly in the simulations. Examining the fraction of CCs and NCCs defined as relaxed we find no evidence that CCs are more relaxed, suggesting that mergers are not solely responsible for disrupting CCs. A comparison of the median thermodynamic profiles defined by different CC criteria shows that the extent to which they evolve in the cluster core is dependent on the CC criteria. We conclude that the thermodynamic structure of galaxy clusters in IllustrisTNG shares many similarities with observations, but achieving better agreement most likely requires modifications of the underlying galaxy formation model.

引用

页码：1809 / 1831

页数：23

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