Turbulent pressure support and hydrostatic mass bias in the intracluster medium
- Angelinelli, M ORCID INAF, Osservatorio di Astrofisica e Scienza dello Spazio, Via Pietro Gobetti 93/3, I-40129 Bologna, Italy
- Vazza, F ORCID Istituto di Radioastronomia, INAF, Via Gobetti 101, I-40121 Bologna, Italy
- Giocoli, C ORCID INFN, Sezione di Bologna, Viale Berti Pichat 6/2, I-40127 Bologna, Italy
- Ettori, S ORCID INFN, Sezione di Bologna, Viale Berti Pichat 6/2, I-40127 Bologna, Italy
- Jones, T W University of Minnesota Twin Cities Minneapolis, MN 55414, USA
- Brunetti, G Istituto di Radioastronomia, INAF, Via Gobetti 101, I-40121 Bologna, Italy
- Brüggen, M Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany
- Eckert, D The Astronomy Department, University of Geneva, Ch. d’Ecogia 16, CH-1290 Versoix, Switzerland
- 2020-4-13
Published in:
- Monthly Notices of the Royal Astronomical Society. - Oxford University Press (OUP). - 2020, vol. 495, no. 1, p. 864-885
English
ABSTRACT
The degree of turbulent pressure support by residual gas motions in galaxy clusters is not well known. Mass modelling of combined X-ray and Sunyaev–Zel’dovich observations provides an estimate of turbulent pressure support in the outer regions of several galaxy clusters. Here, we test two different filtering techniques to disentangle bulk from turbulent motions in non-radiative high-resolution cosmological simulations of galaxy clusters using the cosmological hydrocode enzo. We find that the radial behaviour of the ratio of non-thermal pressure to total gas pressure as a function of cluster-centric distance can be described by a simple polynomial function. The typical non-thermal pressure support in the centre of clusters is ∼5 per cent, increasing to ∼15 per cent in the outskirts, in line with the pressure excess found in recent X-ray observations. While the complex dynamics of the intracluster medium makes it impossible to reconstruct a simple correlation between turbulent motions and hydrostatic bias, we find that a relation between them can be established using the median properties of a sample of objects. Moreover, we estimate the contribution of radial accelerations to the non-thermal pressure support and conclude that it decreases moving outwards from 40 per cent (in the core) to 15 per cent (in the cluster’s outskirts). Adding this contribution to one provided by turbulence, we show that it might account for the entire observed hydrostatic bias in the innermost regions of the clusters, and for less than 80 per cent of it at r > 0.8 r200,m.
- Language
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- English
- Open access status
- green
- Identifiers
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- DOI 10.1093/mnras/staa975
- ISSN 0035-8711
- Persistent URL
- https://sonar.ch/global/documents/279568
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