EDP Sciences
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Volume 461, Number 1, January I 2007
Page(s) 71 - 80
Section Cosmology (including clusters of galaxies)
DOI http://dx.doi.org/10.1051/0004-6361:20065676

A&A 461, 71-80 (2007)
DOI: 10.1051/0004-6361:20065676

Temperature profiles of a representative sample of nearby X-ray galaxy clusters

G. W. Pratt1, H. Böhringer1, J. H. Croston2, 3, M. Arnaud2, S. Borgani4, A. Finoguenov1, and R. F. Temple5

1  MPE Garching, Giessenbachstraße, 85748 Garching, Germany
    e-mail: gwp@mpe.mpg.de
2  CEA/Saclay, Service d'Astrophysique, L'Orme des Merisiers, Bât. 709, 91191 Gif-sur-Yvette Cedex, France
3  School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
4  Dipartimento di Astronomia dell'Università di Trieste, via Tiepolo 11, 34131 Trieste, Italy
5  School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK

(Received 23 May 2006 / Accepted 14 September 2006 )

Context.A study of the structural and scaling properties of the temperature distribution of the hot, X-ray emitting intra-cluster medium of galaxy clusters, and its dependence on dynamical state, can give insights into the physical processes governing the formation and evolution of structure.
Aims.Accurate temperature measurements are a pre-requisite for a precise knowledge of the thermodynamic properties of the intra-cluster medium.
Methods.We analyse the X-ray temperature profiles from XMM-Newton observations of 15 nearby (z<0.2) clusters, drawn from a statistically representative sample. The clusters cover a temperature range from 2.5 keV to 8.5 keV, and present a variety of X-ray morphologies. We derive accurate projected temperature profiles to ~ $ 0.5\,R_{200}$, and compare structural properties (outer slope, presence of cooling core) with a quantitative measure of the X-ray morphology as expressed by power ratios. We also compare the results to recent cosmological numerical simulations.
Results.Once the temperature profiles are scaled by an average cluster temperature (excluding the central region) and the estimated virial radius, the profiles generally decline in the region $0.1\,R_{200}
\la R \la 0.5\,R_{200}$. The central regions show the largest scatter, attributable mostly to the presence of cool core clusters. There is good agreement with numerical simulations outside the core regions. We find no obvious correlations between power ratio and outer profile slope. There may however be a weak trend with the existence of a cool core, in the sense that clusters with a central temperature decrement appear to be slightly more regular.
Conclusions.The present results lend further evidence to indicate that clusters are a regular population, at least outside the core region.

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

© ESO 2006

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