Volume 415, Number 3, March I 2004
|Page(s)||931 - 940|
|Published online||13 February 2004|
The radio galaxy K-z relation: The M\odot mass limit
Masses of galaxies from the L luminosity, up to z
Institut d'Astrophysique de Paris, 98bis, Bd Arago, 75014 Paris, France
2 Université de Paris-Sud XI, Bât. 333, 91405 Orsay Cedex, France
3 Université Paris VI, 4, place Jussieu, 75252 Paris Cedex 05, France
4 DSM/DAPNIA, Service d'Astrophysique, CEA-Saclay, Bât. 709, 91191 Gif-sur-Yvette, France
Corresponding author: B. Rocca-Volmerange, email@example.com
Accepted: 7 November 2003
The narrow K-z relation of powerful radio galaxies in the Hubble K-band diagram is often attributed to the stellar populations of massive elliptical galaxies. Because it extends over a large range of redshifts (), it is difficult to estimate masses at high redshifts by taking into account galaxy evolution. In the present paper, we propose to estimate the stellar masses of galaxies using the galaxy evolution model PÉGASE. We use star formation scenarios that successfully fit faint galaxy counts as well as galaxy templates. These scenarios also predict spectra at higher z, used to estimate valid photometric redshifts. The baryonic mass of the initial gas cloud is then derived. The K-z relation is remarkably reproduced by our evolutionary scenario for elliptical galaxies of baryonic mass , at all z up to . is also the maximum mass limit of all types of galaxies. Using another initial mass function (IMF), even a top-heavy one, does not alter our conclusions. The high value of observed at implies that massive clouds were already formed at early epochs. We also find that the limit is similar to the critical mass of a self-gravitating cloud regulated by cooling (Rees & Ostriker [CITE]; Silk [CITE]). Moreover, the critical size is remarkably close to the typical diameter of Lyα haloes surrounding distant radio galaxies. This confirms the validity of the method of baryonic mass determination based on the K-band luminosity. A puzzling question that remains to be answered is the short time-scale of mass-accumulation required to form such massive galaxies at . We discuss the dispersion of the K-z relation in terms of uncertainties on the mass limit. The link between the presence of the active nucleus and a large stellar mass is also discussed.
Key words: galaxies: evolution / galaxies: fundamental parameters / galaxies: distances and redshifts / cosmology: observations
© ESO, 2004
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