Issue |
A&A
Volume 466, Number 3, May II 2007
|
|
---|---|---|
Page(s) | 813 - 821 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20066804 | |
Published online | 24 April 2007 |
Metal enrichment of the intra-cluster medium over a Hubble time for merging and relaxed galaxy clusters
1
Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstr. 25, 6020 Innsbruck, Austria e-mail: Wolfgang.E.Kapferer@uibk.ac.at
2
Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
3
School of Mathematics, University of Edinburgh, Edinburgh EH9 3JZ, Scotland, UK
Received:
24
November
2006
Accepted:
26
January
2007
We investigate the efficiency of galactic mass loss,
triggered by ram-pressure stripping and galactic winds of cluster
galaxies, on the chemical enrichment of the intra-cluster medium
(ICM). We combine N-body and hydrodynamic simulations with a
semi-numerical galaxy formation model. By including simultaneously
different enrichment processes, namely ram-pressure stripping and
galactic winds, in galaxy-cluster simulations, we are able to
reproduce the observed metal distribution in the ICM. We find that
the mass loss by galactic winds in the redshift regime is
~10% to 20% of the total galactic wind mass loss, whereas the
mass loss by ram-pressure stripping in the same epoch is up to 5%
of the total ram-pressure stripping mass loss over the whole
simulation time. In the cluster formation epochs
ram-pressure
stripping becomes more dominant than galactic winds. We discuss the
non-correlation between the evolution of the mean metallicity of
galaxy clusters and the galactic mass losses. For comparison with
observations we present two dimensional maps of the ICM quantities
and radial metallicity profiles. The shape of the observed profiles
is well reproduced by the simulations in the case of merging
systems. In the case of cool-core clusters the slope of the observed
profiles are reproduced by the simulation at radii below ~300
kpc, whereas at larger radii the observed profiles are shallower. We
confirm the inhomogeneous metal distribution in the ICM found in
observations. To study the robustness of our results, we investigate
two different descriptions for the enrichment process interaction.
Key words: hydrodynamics / methods: numerical / Galaxy: abundances / galaxies: interactions / galaxies: intergalactic medium / galaxies: evolution
© ESO, 2007
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