Adami, C. and Giles, P. and Koulouridis, E. and Pacaud, F. and Caretta, C. A. and Pierre, M. and Eckert, D. and Ramos-Ceja, M. E. and Gastaldello, F. and Fotopoulou, S. and Guglielmo, V. and Lidman, C. and Sadibekova, T. and Iovino, A. and Maughan, B. and Chiappetti, L. and Alis, S. and Altieri, B. and Baldry, I. and Bottini, D. and Birkinshaw, M. and Bremer, M. and Brown, M. and Cucciati, O. and Driver, S. and Elmer, E. and Ettori, S. and Evrard, A. E. and Faccioli, L. and Granett, B. and Grootes, M. and Guzzo, L. and Hopkins, A. and Horellou, C. and Lefèvre, J. P. and Liske, J. and Malek, K. and Marulli, F. and Maurogordato, S. and Owers, M. and Paltani, S. and Poggianti, B. and Polletta, M. and Plionis, M. and Pollo, A. and Pompei, E. and Ponman, T. and Rapetti, D. and Ricci, M. and Robotham, A. and Tuffs, R. and Tasca, L. and Valtchanov, I. and Vergani, D. and Wagner, G. and Willis, J. (2018) 'The XXL Survey : XX. the 365 cluster catalogue.', Astronomy & astrophysics., 620 . A5.
Context. In the currently debated context of using clusters of galaxies as cosmological probes, the need for well-defined cluster samples is critical. Aims. The XXL Survey has been specifically designed to provide a well characterised sample of some 500 X-ray detected clusters suitable for cosmological studies. The main goal of present article is to make public and describe the properties of the cluster catalogue in its present state, as well as of associated catalogues of more specific objects such as super-clusters and fossil groups. Methods. Following from the publication of the hundred brightest XXL clusters, we now release a sample containing 365 clusters in total, down to a flux of a few 10−15 erg s−1 cm−2 in the [0.5–2] keV band and in a 1′ aperture. This release contains the complete subset of clusters for which the selection function is well determined plus all X-ray clusters which are, to date, spectroscopically confirmed. In this paper, we give the details of the follow-up observations and explain the procedure adopted to validate the cluster spectroscopic redshifts. Considering the whole XXL cluster sample, we have provided two types of selection, both complete in a particular sense: one based on flux-morphology criteria, and an alternative based on the [0.5–2] keV flux within 1 arcmin of the cluster centre. We have also provided X-ray temperature measurements for 80% of the clusters having a flux larger than 9 × 10−15 erg s−1 cm−2. Results. Our cluster sample extends from z ~ 0 to z ~ 1.2, with one cluster at z ~ 2. Clusters were identified through a mean number of six spectroscopically confirmed cluster members. The largest number of confirmed spectroscopic members in a cluster is 41. Our updated luminosity function and luminosity–temperature relation are compatible with our previous determinations based on the 100 brightest clusters, but show smaller uncertainties. We also present an enlarged list of super-clusters and a sample of 18 possible fossil groups. Conclusions. This intermediate publication is the last before the final release of the complete XXL cluster catalogue when the ongoing C2 cluster spectroscopic follow-up is complete. It provides a unique inventory of medium-mass clusters over a 50 deg2 area out to z ~ 1.
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|Publisher Web site:||https://doi.org/10.1051/0004-6361/201731606|
|Publisher statement:||Reproduced with permission from Astronomy & Astrophysics, © ESO.|
|Record Created:||06 Dec 2018 10:58|
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