EDP Sciences
Free access
Volume 487, Number 2, August IV 2008
Page(s) 461 - 466
Section Cosmology (including clusters of galaxies)
DOI http://dx.doi.org/10.1051/0004-6361:200810113
Published online 09 June 2008

A&A 487, 461-466 (2008)
DOI: 10.1051/0004-6361:200810113

Radial metallicity profiles for a large sample of galaxy clusters observed with XMM-Newton

A. Leccardi1, 2 and S. Molendi2

1  Università degli Studi di Milano, Dip. di Fisica, via Celoria 16, 20133 Milano, Italy
2  INAF - IASF Milano, via Bassini 15, 20133 Milano, Italy
    e-mail: leccardi@iasf-milano.inaf.ot

Received 2 May 2008 / Accepted 4 June 2008

Aims. We measured radial metallicity profiles for a sample of $\approx$50 hot, intermediate redshift galaxy clusters, selected from the XMM-Newton archive.
Methods. As in our previous paper, we used background modeling rather than background subtraction, and the Cash statistic rather than the $\chi^2$. This method requires a careful characterization of all background components. We also performed Montecarlo simulations to assess systematic effects.
Results. The mean metallicity profile shows a peak in the center, and gently declines out to 0.2 R180. Beyond 0.2 R180 the metallicity is $\approx$0.2 solar and, at variance with recently published expectations based on simulations, consistent with being flat. We find no evidence of profile evolution from z = 0.1 to z = 0.3. When comparing our mean profile to those obtained by recent works with BeppoSAX and Chandra, we find remarkable agreement over the entire radial range.

Key words: X-rays: galaxies: clusters -- galaxies: clusters: general -- cosmology: observations

© ESO 2008