Impact of stochastic gas motions on galaxy cluster abundance profiles

被引:110
作者
Rebusco, P
Churazov, E
Böhringer, H
Forman, W
机构
[1] Max Planck Inst Astrophys, D-85741 Garching, Germany
[2] Space Res Inst IKI, Moscow 117810, Russia
[3] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany
[4] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
关键词
cooling flows; galaxies : clusters : general; galaxies : clusters : individual : Perseus;
D O I
10.1111/j.1365-2966.2005.08965.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The impact of stochastic gas motions on the metal distribution in cluster cores is evaluated. Peaked abundance profiles are a characteristic feature of clusters with cool cores, and abundance peaks are probably associated with the brightest cluster galaxies (BCGs), which dwell in cluster cores. However, the width of the abundance peaks is significantly broader than the BCG light distribution, suggesting that some gas motions are transporting metals originating from within the BCG. Assuming that this process can be treated as diffusive, and using the brightest X-ray cluster A426 (Perseus) as an example, we estimate that a diffusion coefficient of the order of 2 x 10(29) cm(2) s(-1) is needed to explain the width of the observed abundance profiles. Much lower (higher) diffusion coefficients would result in too peaked (too shallow) profiles. Such diffusion could be produced by stochastic gas motions, and our analysis provides constraints on the product of their characteristic velocity and their spatial coherence scale. We speculate that the activity of the supermassive black hole of the BCG is driving the stochastic gas motions in cluster cores. When combined with the assumption that the dissipation of the same motions is a key gas heating mechanism, one can estimate both the velocity and the spatial scale of such diffusive processes.
引用
收藏
页码:1041 / 1048
页数:8
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