Volume 431, Number 2, February IV 2005
|Page(s)||405 - 413|
|Section||Cosmology (including clusters of galaxies)|
|Published online||04 February 2005|
Simulating the soft X-ray excess in clusters of galaxies
Dipartimento di Astronomia dell'Universitá di Trieste, via Tiepolo 11, 34131 Trieste, Italy e-mail: firstname.lastname@example.org
2 Department of Astronomy, Beijing Normal University, Beijing 100875, PR China
3 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR China
4 INFN - National Institute for Nuclear Physics, Trieste, Italy
5 INAF, Osservatorio Astronomico di Trieste, via Tiepolo 11, 34131 Trieste, Italy
6 Dipartimento di Fisica Generale “Amedeo Avogadro”, Universitá degli Studi di Torino, Torino, Italy
7 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild Strasse 1, Garching bei München, Germany
8 Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy
9 INAF, Osservatorio Astronomico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Italy
10 Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 2, 35122 Padova, Italy
Accepted: 6 October 2004
The detection of an excess of soft X-ray or Extreme Ultraviolet (EUV) radiation, above the thermal contribution from the hot intracluster medium (ICM), has been a controversial subject ever since the initial discovery of this phenomenon. We use a large-scale hydrodynamical simulation of a concordance ΛCDM model, to investigate the possible thermal origin of such an excess in a set of 20 simulated clusters having temperatures in the range 1-7 keV. Simulated clusters are analysed by mimicking the observational procedure applied to ROSAT-PSPC data, which for the first time showed evidence for the soft X-ray excess: we compare the low-energy (e.g. [ 0.2-1] keV) part of the spectrum of each cluster with that predicted for a plasma having temperature and metallicity as computed after weighting by the emissivity in a harder band (e.g., [ 1-2] keV). For distances to the cluster center we detect a significant excess in most of the simulated clusters, whose relative amount changes from cluster to cluster and, for the same cluster, by changing the projection direction. In about 30 per cent of the cases the soft X-ray flux is measured to be at least 50 per cent larger than predicted by the one-temperature plasma model. We find that this excess is generated in most cases within the virialized regions of the cluster. It mainly comes from low-entropy and high-density gas associated with merging sub-halos, rather than from diffuse warm gas. Only in a few cases does the excess arise from fore/background groups observed in projection, while no evidence is found for a significant contribution from gas lying within large-scale filaments. We compute the distribution of the relative soft excess, as a function of the distance to the cluster center , and compare it with the observational result by Bonamente et al. ([CITE]) for the Coma cluster. As in the observations, we find that the relative excess increases with the distance from the cluster center, with no significant excess detected for . However, an excess as large as that reported for the Coma cluster at scales is found to be rather unusual in our set of simulated clusters.
Key words: cosmology: diffuse radiation / galaxies: clusters: general / X-rays: galaxies: clusters / methods: numerical
© ESO, 2005
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