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Title:
The evolution of the brightest cluster galaxies since z ~ 1 from the ESO Distant Cluster Survey (EDisCS)
Authors:
Whiley, I. M.; Aragón-Salamanca, A.; De Lucia, G.; von der Linden, A.; Bamford, S. P.; Best, P.; Bremer, M. N.; Jablonka, P.; Johnson, O.; Milvang-Jensen, B.; Noll, S.; Poggianti, B. M.; Rudnick, G.; Saglia, R.; White, S.; Zaritsky, D.
Affiliation:
AA(School of Physics and Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD), AB(School of Physics and Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD), AC(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany), AD(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany), AE(Institute of Cosmology and Gravitation, Mercantile House, Hampshire Terrace, University of Portsmouth, Portsmouth PO1 2EG), AF(SUPA, Institute for Astronomy, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ), AG(H H Wills Physics Laboratory, Tyndall Avenue, Bristol BS8 1TL), AH(Université de Genéve, Laboratoire d'Astrophysique de l'Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire, CH-1290 Sauverny, Switzerland), AI(SUPA, Institute for Astronomy, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ), AJ(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark; The Royal Library/Copenhagen University Library, Research Department, Box 2149, DK-1016 Copenhagen K, Denmark), AK(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr., D-85741 Garching, Germany), AL(Osservatorio Astronomico, vicolo dell' Osservatorio 5, 35122 Padova, Italy), AM(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany), AN(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr., D-85741 Garching, Germany), AO(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany), AP(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson AZ 85721, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 387, Issue 3, pp. 1253-1263. (MNRAS Homepage)
Publication Date:
07/2008
Origin:
MNRAS
MNRAS Keywords:
galaxies: clusters: general , galaxies: elliptical and lenticular, cD , galaxies: evolution , galaxies: formation , infrared: galaxies
Abstract Copyright:
(c) Journal compilation © 2008 RAS
DOI:
10.1111/j.1365-2966.2008.13324.x
Bibliographic Code:
2008MNRAS.387.1253W

Abstract

We present K-band data for the brightest cluster galaxies (BCGs) from the ESO Distant Cluster Survey (EDisCS). These data are combined with the photometry published by Aragón-Salamanca, Baugh & Kauffmann and a low-redshift comparison sample built from the BCG catalogue of von der Linden et al. BCG luminosities are measured inside a metric circular aperture with 37kpc diameter. In agreement with previous studies, we find that the K-band Hubble diagram for BCGs exhibits very low scatter (~0.35) over a redshift range of 0 < z < 1. The colour and rest-frame K-band luminosity evolution of the BCGs are in good agreement with population synthesis models of stellar populations which formed at z > 2 and evolved passively thereafter. In contrast with some previous studies, we do not detect any significant change in the stellar mass of the BCG since z ~ 1. These results do not seem to depend on the velocity dispersion of the parent cluster. We also find that there is a correlation between the 1D velocity dispersion of the clusters (σcl) and the K-band luminosity of the BCGs (after correcting for passive-evolution). The clusters with large velocity dispersions, and therefore masses, tend to have brighter BCGs, i.e. BCGs with larger stellar masses. This dependency, although significant, is relatively weak: the stellar mass of the BCGs changes only by ~70 per cent over a two order of magnitude range in cluster mass. Furthermore, this dependency does not change significantly with redshift. We have compared our observational results with the hierarchical galaxy formation and evolution model predictions of De Lucia & Blaizot. We find that the models predict colours which are in reasonable agreement with the observations because the growth in stellar mass is dominated by the accretion of old stars. However, the stellar mass in the model BCGs grows by a factor of 3-4 since z = 1, a growth rate which seems to be ruled out by the observations. The models predict a dependency between the BCG's stellar mass and the velocity dispersion (mass) of the parent cluster in the same sense as the data, but the dependency is significantly stronger than observed. However, one major difficulty in this comparison is that we have measured magnitudes inside a fixed metric aperture while the models compute total luminosities.
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