Metal enrichment of the intra-cluster medium by thermally and cosmic-ray driven galactic winds

Free access article

Issue		A&A Volume 504, Number 3, September IV 2009


Page(s)		719 - 726
Section		Cosmology (including clusters of galaxies)
DOI		http://dx.doi.org/10.1051/0004-6361/200912099
Published online		24 July 2009

A&A 504, 719-726 (2009)
DOI: 10.1051/0004-6361/200912099

An analytical prescription for galactic outflows

W. Kapferer¹, T. Kronberger¹, D. Breitschwerdt², S. Schindler¹, E. van Kampen¹, S. Kimeswenger¹, W. Domainko³, M. Mair¹, and M. Ruffert⁴

¹ Institute for Astro- and Particle Physics, University of Innsbruck, Technikerstr. 25, 6020 Innsbruck, Austria
e-mail: wolfgang.e.kapferer@uibk.ac.at
² Zentrum für Astronomie und Astrophysik, Technische Universität Berlin, Hardenbergstrasse 36, 10623 Berlin, Germany
³ Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
⁴ School of Mathematics and Maxwell Institute, University of Edinburgh, Edinburgh EH9 3JZ, Scotland, UK

Received 18 March 2009 / Accepted 14 July 2009

Abstract
Aims. We investigate the efficiency and time-dependence of thermally and cosmic ray driven galactic winds for the metal enrichment of the intra-cluster medium (ICM) using a new analytical approximation for the mass outflow. The spatial distribution of the metals are studied using radial metallicity profiles and 2D metallicity maps of the model clusters as they would be observed by X-ray telescopes like XMM-Newton.
Methods. Analytical approximations for the mass loss by galactic winds driven by thermal and cosmic ray pressure are derived from the Bernoulli equation and implemented in combined N-body/hydrodynamic cosmological simulations with a semi-analytical galaxy formation model. Observable quantities like the mean metallicity, metallicity profiles, and 2D metal maps of the model clusters are derived from the simulations.
Results. We find that galactic winds alone cannot account for the observed metallicity of the ICM. At redshift z=0 the model clusters have metallicities originating from galactic winds which are almost a factor of 10 lower than the observed values. For massive, relaxed clusters we find, as in previous studies, a central drop in the metallicity due to a suppression of the galactic winds by the pressure of the ambient ICM. Combining ram-pressure stripping and galactic winds we find radial metallicity profiles of the model clusters which agree qualitatively with observed profiles. Only in the inner parts of massive clusters the observed profiles are steeper than in the simulations. Also the combination of galactic winds and ram-pressure stripping yields too low values for the ICM metallicities. The slope of the redshift evolution of the mean metallicity in the simulations agrees reasonably well with recent observations.

Key words: galaxies: clusters: general -- intergalactic medium -- ISM: jets and outflows -- methods: numerical

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