Issue |
A&A
Volume 447, Number 3, March I 2006
|
|
---|---|---|
Page(s) | 827 - 842 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20053975 | |
Published online | 10 February 2006 |
Simulations of galactic winds and starbursts in galaxy clusters
1
Institut für Astrophysik, Leopold-Franzens-Universität Innsbruck, Technikerstr. 25, 6020 Innsbruck, Austria e-mail: wolfgang.e.kapferer@uibk.ac.at
2
Institut für Astrophysik, Universität Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
3
Institut für Astronomie, Türkenschanzstrasse 17, 1180 Wien, Austria
4
School of Mathematics, University of Edinburgh, Edinburgh EH9 3JZ, Scotland, UK
Received:
3
August
2005
Accepted:
24
October
2005
We present an investigation of the metal enrichment of
the intra-cluster medium (ICM) by galactic winds and merger-driven
starbursts. We use combined N-body/hydrodynamic simulations with a
semi-numerical galaxy formation model. The mass loss by galactic
winds is obtained by calculating transonic solutions of steady
state outflows, driven by thermal, cosmic ray and MHD wave
pressure. The inhomogeneities in the metal distribution caused by
these processes are an ideal tool to reveal the dynamical state of
a galaxy cluster. We present surface brightness, X-ray emission
weighted temperature and metal maps of our model clusters as they
would be observed by X-ray telescopes like XMM-Newton. We show
that X-ray weighted metal maps distinguish between pre- or
post-merger galaxy clusters by comparing the metallicity
distribution with the galaxy-density distribution: pre-mergers
have a metallicity gap between the subclusters, post-mergers a
high metallicity between subclusters. We apply our approach to two
observed galaxy clusters, Abell 3528 and Abell 3921, to show
whether they are pre- or post-merging systems. The survival time
of the inhomogeneities in the metallicity distribution found in
our simulations is up to several Gyr. We show that galactic winds
and merger-driven starbursts enrich the ICM very efficiently after
in the central (~3 Mpc radius) region of a galaxy
cluster.
Key words: galaxies: clusters: general / galaxies: abundances / galaxies: interactions / galaxies: ISM / X-ray: galaxies: clusters
© ESO, 2006
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