The turbulent pressure support in galaxy clusters revisited

F. Vazza, M. Angelinelli, T. W. Jones, D. Eckert, M. Brüggen, G. Brunetti, C. Gheller

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Abstract

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 ∼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 ∼10 per cent of the total pressure at R 200.

Original languageEnglish (US)
Pages (from-to)L120-L124
JournalMonthly Notices of the Royal Astronomical Society: Letters
Volume481
Issue number1
DOIs
StatePublished - Nov 21 2018

Keywords

  • Galaxy: general
  • Intergalactic medium
  • Large-scale structure of Universe
  • Methods: numerical

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    Vazza, F., Angelinelli, M., Jones, T. W., Eckert, D., Brüggen, M., Brunetti, G., & Gheller, C. (2018). The turbulent pressure support in galaxy clusters revisited. Monthly Notices of the Royal Astronomical Society: Letters, 481(1), L120-L124. https://doi.org/10.1093/mnrasl/sly172