Evolution of the gas mass fraction in galaxy clusters

被引：11

作者：

Dvorkin, Irina ^{[1
,2
]}

Rephaeli, Yoel ^{[2
,3
]}

机构：

[1] Inst Astrophys, UMR 7095, F-75014 Paris, France

[2] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel

[3] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2015年 / 450卷 / 01期

基金：

以色列科学基金会;

关键词：

galaxies: clusters: general; galaxies: clusters: intracluster medium; X-RAY CAVITIES; BARYON FRACTIONS; INTRACLUSTER MEDIUM; STAR-FORMATION; HYDRODYNAMICAL SIMULATIONS; SCALING RELATIONS; METAL ENRICHMENT; SPIRAL GALAXIES; OBSERVED GROWTH; POWER SPECTRUM;

D O I：

10.1093/mnras/stv644

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The mass fraction of hot gas in clusters is a basic quantity whose level and dependence on the cluster mass and redshift are intimately linked to all cluster X-ray and Sunyayev-Zel'dovich measures. Modelling the evolution of the gas fraction is clearly a necessary ingredient in the description of the hierarchical growth of clusters through mergers of subclumps and mass accretion on the one hand, and the dispersal of gas from the cluster galaxies by tidal interactions, galactic winds and ram-pressure stripping on the other hand. A reasonably complete description of this evolution can only be given by very detailed hydrodynamical simulations, which are, however, resource-intensive and difficult to implement in the mapping of parameter space. A much more practical approach is the use of semi-analytic modelling that can be easily implemented to explore a wide range of parameters. We present first results from a simple model that describes the build-up of the gas mass fraction in clusters by following the overall impact of the above processes during the merger and accretion history of each cluster in the ensemble. Acceptable ranges for model parameters are deduced through comparison with results of X-ray observations. Basic implications of our work for modelling cluster statistical properties, and the use of these properties in joint cosmological data analyses, are discussed.

引用

页码：896 / 904

页数：9

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