This article has an erratum: [erratum]
Volume 593, September 2016
|Number of page(s)||17|
|Section||Cosmology (including clusters of galaxies)|
|Published online||29 August 2016|
Size growth of red-sequence early-type galaxies in clusters in the last 10 Gyr⋆
1 INAF–Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy
2 Instituto de Astrofisica de Andalucia (CSIC), Glorieta de la Astronoma S/N, 18008 Granada, Spain
3 CEA, Centre de Saclay, IRFU/SPP, 91191 Gif-sur-Yvette, France
Received: 7 March 2016
Accepted: 28 May 2016
We carried out a photometric and structural analysis in the rest-frame V band of a mass-selected (log M/M⊙> 10.7) sample of red-sequence galaxies in 14 galaxy clusters, 6 of which are at z> 1.45, namely JKCS041, IDCS J1426.5+3508, SpARCS104922.6+564032.5, SpARCSJ021524-034331, XDCPJ0044.0-2033, and SPT-CLJ2040-4451. To this end, we reduced/analyzed about 300 orbits of multicolor images taken with the Advanced Camera for Survey and the Wide Field Camera 3 on the Hubble Space Telescope. We uniformly morphologically classified galaxies from z = 0.023 to z = 1.803, and we homogeneously derived sizes (effective radii) for the entire sample. Furthermore, our size derivation allows, and therefore is not biased by, the presence of the usual variety of morphological structures seen in early-type galaxies, such as bulges, bars, disks, isophote twists, and ellipiticy gradients. By using such a mass-selected sample, composed of 244 red-sequence early-type galaxies, we find that the log of the galaxy size at a fixed stellar mass, log M/M⊙ = 11, has increased with time at a rate of 0.023 ± 0.002 dex per Gyr over the last 10 Gyr, in marked contrast with the threefold increase found in the literature for galaxies in the general field over the same period. This suggests, at face value, that secular processes should be excluded as the primary drivers of size evolution because we observed an environmental dependent size growth. Using spectroscopic ages of Coma early-type galaxies we also find that recently quenched early-type galaxies are a numerically minor population not different enough in size to alter the mean size at a given mass, which implies that the progenitor bias is minor, i.e., that the size evolution measured by selecting galaxies at the redshift of observation is indistinguishable from the one that compares ancestors and descendents.
Key words: galaxies: clusters: general / galaxies: elliptical and lenticular, cD / galaxies: evolution
Full Table 3 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/593/A2
© ESO, 2016
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