Bower, R. G. and Benson, A. J. and Lacey, Cedric G. and Baugh, C. M. and Cole, Shaun and Frenk, C. S. (2001) 'The impact of galaxy formation on the X-ray evolution of clusters.', Monthly Notices of the Royal Astronomical Society., 325 (2). pp. 497-508.
We present a new model for the X-ray properties of the intracluster medium that explicitly includes heating of the gas by the energy released during the evolution of cluster galaxies. We calculate the evolution of clusters by combining the semi-analytic model of galaxy formation of Cole et al. with a simple model for the radial profile of the intracluster gas. We focus on the cluster X-ray luminosity function and on the relation between X-ray temperature and luminosity (the T–L relation). Observations of these properties are known to disagree with predictions based on scaling relations that neglect gas cooling and heating processes. We show that cooling alone is not enough to account for the flatness of the observed T–L relation or for the lack of strong redshift evolution in the observed X-ray luminosity function. Gas heating, on the other hand, can solve these two problems: in the Λ cold dark matter cosmology, our model reproduces fairly well the T–L relation and the X-ray luminosity function. Furthermore, it predicts only weak evolution in these two properties out to z=0.5, in agreement with recent observational data. A successful model requires an energy input of 1–2×1049 erg per solar mass of stars formed. This is comparable to the total energy released by the supernovae associated with the formation of the cluster galaxies. Thus, unless the transfer of supernovae energy to the intracluster gas is very (perhaps unrealistically) efficient, additional sources of energy, such as mechanical energy from active galactic nuclei winds are required. However, the amplification of an initial energy input by the response of the intracluster medium to protocluster mergers might ease the energy requirements. Our model makes definite predictions for the X-ray properties of groups and clusters at high redshift. Some of these, such as the T–L relation at z1, may soon be tested with data from the Chandra and Newton satellites.
|Keywords:||Galaxies, Clusters, Formation.|
|Full text:||(NA) Not Applicable |
Download PDF (470Kb)
|Full text:||(VoR) Version of Record|
Download PDF (359Kb)
|Publisher Web site:||http://dx.doi.org/10.1046/j.1365-8711.2001.04382.x|
|Publisher statement:||This article has been published in the Monthly Notices of the Royal Astronomical Society © 2001 RAS. Published by Oxford University Press on behalf of The Royal Astronomical Society. All rights reserved.|
|Date accepted:||No date available|
|Date deposited:||20 November 2013|
|Date of first online publication:||August 2001|
|Date first made open access:||No date available|
Save or Share this output
|Look up in GoogleScholar|