The representative XMM-Newton cluster structure survey (REXCESS) of an X-ray luminosity selected galaxy cluster sample

¹ Max-Planck-Institut für extraterrestrische Physik, 85748 Garching, Germany e-mail: hxb@mpe.mpg.de
² Service d'Astrophysique, CEA Saclay, L'Ormes des Merisiers, 91191 Gif-sur-Yvette Cedex, France
³ School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
⁴ School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
⁵ Dipartimento di Astronomia dell'Universitá di Trieste, via Tiepolo 11, 34133 Trieste, Italy
⁶ Institute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK
⁷ Liverpool John Moores University, Liverpool, UK
⁸ Department of Physics and Astronomy, Michigan State University, BPS Building, East Lansing, MI 48824, USA
⁹ Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA, USA
¹⁰ INAF - Osservatorio Astronomico di Brera-Merate, via Bianchi 46, 23807 Merate, Italy
¹¹ Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
¹² Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
¹³ Department of Physics, University of Illinois, 1110 West Green Street, Urbana, IL 61801, USA
¹⁴ Department of Physics, Tokyo University of Science, 1-3 Kagurazaka, Shinjyuku-ku, Tokyo 162-8601, Japan
¹⁵ Department of Astronomy, University of Michigan, 918 Dennison, 500 Church Street, Ann Arbor, MI 48109, USA
¹⁶ Department of Physics, Tokyo Metropolitan University, Hachioji, Tokyo 192-0397, Japan
¹⁷ Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark
¹⁸ Departamento de Astronomiá y Astrofisica, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22, Chile
¹⁹ Argelander Institute for Astronomy (AIfA), Bonn University, Auf dem Hügel 71, 53121 Bonn, Germany
²⁰ Astronomy Centre, University of Sussex, Falmer, Brighton BN1 9QJ, UK
²¹ European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
²² Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15217, USA
²³ Departamento de Matemática Aplicada da Faculdade de Ciências da Universidade do Porto, Rua do Campo Alegre 687, 4169-007 Porto, Portugal
²⁴ Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal

Received: 13 November 2006
Accepted: 5 March 2007

Abstract

Context.The largest uncertainty for cosmological studies using clusters of galaxies is introduced by our limited knowledge of the statistics of galaxy cluster structure, and of the scaling relations between observables and cluster mass.

Aims.To improve on this situation we have started an XMM-Newton Large Programme for the in-depth study of a representative sample of 33 galaxy clusters, selected in the redshift range z = 0.055 to 0.183 from the REFLEX Cluster Survey, having X-ray luminosities above 0.410⁴⁴  erg s^-1 in the 0.1-2.4 keV band. This paper introduces the sample, compiles properties of the clusters, and provides detailed information on the sample selection function.

Methods.We describe the selection of a nearby galaxy cluster sample that makes optimal use of the XMM-Newton field-of-view, and provides nearly homogeneous X-ray luminosity coverage for the full range from poor clusters to the most massive objects in the Universe.

Results.For the clusters in the sample, X-ray fluxes are derived and compared to the previously obtained fluxes from the ROSAT All-Sky Survey. We find that the fluxes and the flux errors have been reliably determined in the ROSAT All-Sky Survey analysis used for the REFLEX Survey. We use the sample selection function documented in detail in this paper to determine the X-ray luminosity function, and compare it with the luminosity function of the entire REFLEX sample. We also discuss morphological peculiarities of some of the sample members.

Conclusions.The sample and some of the background data given in this introductory paper will be important for the application of these data in the detailed studies of cluster structure, to appear in forthcoming publications.