Scaling relations and mass bias in hydrodynamical f (R) gravity simulations of galaxy clusters

被引:59
作者
Arnold, Christian [1 ]
Puchwein, Ewald [1 ,2 ,3 ]
Springel, Volker [1 ,4 ]
机构
[1] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany
[2] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
[3] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England
[4] Heidelberg Univ, Zentrum Astron, Astron Recheninst, D-69120 Heidelberg, Germany
关键词
methods: numerical; cosmology: theory; RICH CLUSTERS; F(R) GRAVITY; CODE;
D O I
10.1093/mnras/stu332
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We investigate the impact of chameleon-type f (R) gravity models on the properties of galaxy clusters and groups. Our f (R) simulations follow for the first time also the hydrodynamics of the intracluster and intragroup medium. This allows us to assess how f (R) gravity alters the X-ray scaling relations of clusters and how hydrostatic and dynamical mass estimates are biased when modifications of gravity are ignored in their determination. We find that velocity dispersions and intracluster medium temperatures are both increased by up to 1/3 in f (R) gravity in low-mass haloes, while the difference disappears in massive objects. The mass scale of the transition depends on the background value f(R0) of the scalar degree of freedom. These changes in temperature and velocity dispersion alter the mass-temperature and X-ray luminosity-temperature scaling relations and bias dynamical and hydrostatic mass estimates that do not explicitly account for modified gravity towards higher values. Recently, a relative enhancement of X-ray compared to weak lensing masses was found by the Planck Collaboration. We demonstrate that an explanation for this offset may be provided by modified gravity and the associated bias effects, which interestingly are of the required size. Finally, we find that the abundance of subhaloes at fixed cluster mass is only weakly affected by f (R) gravity.
引用
收藏
页码:833 / 842
页数:10
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