Volume 485, Number 3, July III 2008
|Page(s)||633 - 644|
|Section||Cosmology (including clusters of galaxies)|
|Published online||15 May 2008|
Star formation efficiency in galaxy clusters
Universidade de São Paulo, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Departamento de Astronomia, Rua do Matão 1226, Cidade Universitária, 05508-090, São Paulo, SP, Brazil e-mail: email@example.com
2 Department of Physics & Astronomy, University College London, London WC1E 6BT, UK
Accepted: 5 April 2008
Context. The luminous material in clusters of galaxies exists in two forms: the visible galaxies and the X-ray emitting intra-cluster medium. The hot intra-cluster gas is the major observed baryonic component of clusters, about six times more massive than the stellar component. The mass contained within visible galaxies is approximately 3% of the dynamical mass.
Aims. Our aim was to analyze both baryonic components, combining X-ray and optical data of a sample of five galaxy clusters (Abell 496, 1689, 2050, 2631 and 2667), within the redshift range . We determined the contribution of stars in galaxies and the intra-cluster medium to the total baryon budget.
Methods. We used public XMM-Newton data to determine the gas mass and to obtain the X-ray substructures. Using the optical counterparts from SDSS or CFHT we determined the stellar contribution.
Results. We examine the relative contribution of galaxies, intra-cluster light and intra-cluster medium to baryon budget in clusters through the stellar-to-gas mass ratio, estimated with recent data. We find that the stellar-to-gas mass ratio within r500 (the radius within which the mean cluster density exceeds the critical density by a factor of 500), is anti-correlated with the ICM temperature, which range from 24% to 6% while the temperature ranges from 4.0 to 8.3 keV. This indicates that less massive cold clusters are more prolific star forming environments than massive hot clusters.
Key words: galaxies: clusters: general / X-rays: galaxies: clusters / galaxies: luminosity function, mass function
© ESO, 2008
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