Cookies

We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.


Durham Research Online
You are in:

Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters.

McCarthy, I.G. and Frenk, C.S. and Font, A.S. and Lacey, C.G. and Bower, R.G. and Mitchell, N.L. and Balogh, M.L. and Theuns, Tom (2008) 'Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters.', Monthly notices of the Royal Astronomical Society., 383 (2). pp. 593-605.

Abstract

We use a large suite of carefully controlled full hydrodynamic simulations to study the ram pressure stripping of the hot gaseous haloes of galaxies as they fall into massive groups and clusters. The sensitivity of the results to the orbit, total galaxy mass, and galaxy structural properties is explored. For typical structural and orbital parameters, we find that ∼30 per cent of the initial hot galactic halo gas can remain in place after 10 Gyr. We propose a physically simple analytic model that describes the stripping seen in the simulations remarkably well. The model is analogous to the original formulation of Gunn & Gott, except that it is appropriate for the case of a spherical (hot) gas distribution (as opposed to a face-on cold disc) and takes into account that stripping is not instantaneous but occurs on a characteristic time-scale. The model reproduces the results of the simulations to within ≈10 per cent at almost all times for all the orbits, mass ratios, and galaxy structural properties we have explored. The one exception involves unlikely systems where the orbit of the galaxy is highly non-radial and its mass exceeds about 10 per cent of the group or cluster into which it is falling (in which case the model underpredicts the stripping following pericentric passage). The proposed model has several interesting applications, including modelling the ram pressure stripping of both observed and cosmologically simulated galaxies and as a way to improve present semi-analytic models of galaxy formation. One immediate consequence is that the colours and morphologies of satellite galaxies in groups and clusters will differ significantly from those predicted with the standard assumption of complete stripping of the hot coronae.

Item Type:Article
Keywords:Hydrodynamics, Methods: N-body simulations, Galaxies: clusters: general, Galaxies: evolution, Galaxies: structure, Cosmology: theory.
Full text:(VoR) Version of Record
Download PDF
(357Kb)
Status:Peer-reviewed
Publisher Web site:http://dx.doi.org/10.1111/j.1365-2966.2007.12577.x
Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2008 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Record Created:20 Feb 2015 09:35
Last Modified:03 Jun 2015 09:49

Social bookmarking: del.icio.usConnoteaBibSonomyCiteULikeFacebookTwitterExport: EndNote, Zotero | BibTex
Look up in GoogleScholar | Find in a UK Library