期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 481, 期 1, 页码 L120-L124出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnrasl/sly172
关键词
methods: numerical; galaxy: general; intergalactic medium; large-scale structure of Universe
资金
- Horizon 2020 program under the ERC Starting Grant 'MAGCOW' [714196]
- US National Science Foundation
Due to their late formation in cosmic history, clusters of galaxies are not fully in hydrostatic equilibrium and the gravitational pull of their mass at a given radius is expected not to be entirely balanced by the thermal gas pressure. Turbulence may supply additional pressure, and recent (X-ray and SZ) hydrostatic mass reconstructions claim a pressure support of similar to 5-15 per cent of the total pressure at R-200. In this work we show that, after carefully disentangling bulk from small-scale turbulent motions in high-resolution simulations of galaxy clusters, we can constrain which fraction of the gas kinetic energy effectively provides pressure support in the cluster's gravitational potential. While the ubiquitous presence of radial inflows in the cluster can lead to significant bias in the estimate of the non-thermal pressure support, we report that only a part of this energy effectively acts as a source of pressure, providing a support of the order of similar to 10 per cent of the total pressure at R-200.
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