The nature and energetics of AGN-driven perturbations in the hot gas in the Perseus Cluster

Zhuravleva, I.; Churazov, E.; Arevalo, P.; Schekochihin, A. A.; Forman, W. R.; Allen, S. W.; Simionescu, A.; Sunyaev, R.; Vikhlinin, A.; Werner, N.

doi:10.1093/mnras/stw520

Title: The nature and energetics of AGN-driven perturbations in the hot gas in the Perseus Cluster

Journal Article · Mon Mar 07 00:00:00 EST 2016 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stw520· OSTI ID:1256639

Zhuravleva, I. ^[1]; Churazov, E. ^[2]; Arevalo, P. ^[3]; Schekochihin, A. A. ^[4]; Forman, W. R. ^[5]; Allen, S. W. ^[6]; Simionescu, A. ^[7]; Sunyaev, R. ^[2]; Vikhlinin, A. ^[5]; Werner, N. ^[1]

Stanford Univ., Stanford, CA (United States)
Max Planck Institute for Astrophysics, Garching (Germany); Space Research Institute (IKI), Moscow (Russia)
Univ. de Valparaiso, Valparaiso (Chile)
Univ. of Oxford, Oxford (United Kingdom)
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
Stanford Univ., Stanford, CA (United States); SLAC National Accelerator Lab., Menlo Park, CA (United States)
Japan Aerospace Exploration Agency, Kanagawa (Japan)

In this paper, cores of relaxed galaxy clusters are often disturbed by AGN. Their Chandra observations revealed a wealth of structures induced by shocks, subsonic gas motions, bubbles of relativistic plasma, etc. In this paper, we determine the nature and energy content of gas fluctuations in the Perseus core by probing statistical properties of emissivity fluctuations imprinted in the soft- and hard-band X-ray images. About 80 per cent of the total variance of perturbations on ~8–70 kpc scales in the core have an isobaric nature, i.e. are consistent with subsonic displacements of the gas in pressure equilibrium with the ambient medium. The observed variance translates to the ratio of energy in perturbations to thermal energy of ~13 per cent. In the region dominated by weak ‘ripples’, about half of the total variance is associated with isobaric perturbations on scales of a few tens of kpc. If these isobaric perturbations are induced by buoyantly rising bubbles, then these results suggest that most of the AGN-injected energy should first go into bubbles rather than into shocks. Using simulations of a shock propagating through the Perseus atmosphere, we found that models reproducing the observed features of a central shock have more than 50 per cent of the AGN-injected energy associated with the bubble enthalpy and only about 20 per cent is carried away with the shock. Such energy partition is consistent with the AGN-feedback model, mediated by bubbles of relativistic plasma, and supports the importance of turbulence in the cooling–heating balance.

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Research Organization:: SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)

Sponsoring Organization:: USDOE Office of Science (SC), High Energy Physics (HEP)

Grant/Contract Number:: AC02-76SF00515

OSTI ID:: 1256639

Report Number(s):: SLAC-PUB-16551; arXiv:1601.02615

Journal Information:: Monthly Notices of the Royal Astronomical Society, Vol. 458, Issue 3; ISSN 0035-8711

Publisher:: Royal Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 43 works

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