Aims. We determined the K-s band luminosity function (LF), and inferred the corresponding stellar mass function, of cluster galaxies at redshift z similar or equal to 1.2, using near-infrared images of three X-ray luminous clusters at z = 1.11, 1.24, 1.27. Methods. The composite LF was derived down to M* + 4, by means of statistical background subtraction, and is well described by a Schechter function with K-s* = 20.5(-1)(+0.4) and alpha = -1.0(-0.3)(+0.2). Using available X-ray mass profiles we determined the M/L ratios of these three clusters, which tend to be lower than those measured in the local universe. Finally, from the Ks band composite LF we derived the stellar mass function of cluster galaxies. Results. With these data, no significant difference can be seen between the cluster galaxies LF and the LF of field galaxies at similar redshift. We also found no significant evolution out to z similar or equal to 1.2 in the bright (< M* + 4) part of the LF probed in this study, apart from a brightening of similar or equal to 1.3 mag of the characteristic magnitude of the high redshift LF. We confirm, and extend to higher redshift, the result from previous work that the redshift evolution of the characteristic magnitude M* is consistent with passive evolution of a stellar population formed at z > 2. Conclusions. The results obtained in this work support and extend previous findings that most of the stars in bright galaxies were formed at high redshift, and that K-s-bright (M > 10(11) M circle dot) galaxies were already in place at z similar or equal to 1.2, at least in the central regions of X-ray luminous clusters. Together with recent results on the field galaxy stellar mass function, this implies that most of the stellar mass is already assembled in massive galaxies by z similar or equal to 1, both in low and high density environments.
The near-infrared luminosity function of cluster galaxies beyond redshift one
ROSATI, Piero;
2006
Abstract
Aims. We determined the K-s band luminosity function (LF), and inferred the corresponding stellar mass function, of cluster galaxies at redshift z similar or equal to 1.2, using near-infrared images of three X-ray luminous clusters at z = 1.11, 1.24, 1.27. Methods. The composite LF was derived down to M* + 4, by means of statistical background subtraction, and is well described by a Schechter function with K-s* = 20.5(-1)(+0.4) and alpha = -1.0(-0.3)(+0.2). Using available X-ray mass profiles we determined the M/L ratios of these three clusters, which tend to be lower than those measured in the local universe. Finally, from the Ks band composite LF we derived the stellar mass function of cluster galaxies. Results. With these data, no significant difference can be seen between the cluster galaxies LF and the LF of field galaxies at similar redshift. We also found no significant evolution out to z similar or equal to 1.2 in the bright (< M* + 4) part of the LF probed in this study, apart from a brightening of similar or equal to 1.3 mag of the characteristic magnitude of the high redshift LF. We confirm, and extend to higher redshift, the result from previous work that the redshift evolution of the characteristic magnitude M* is consistent with passive evolution of a stellar population formed at z > 2. Conclusions. The results obtained in this work support and extend previous findings that most of the stars in bright galaxies were formed at high redshift, and that K-s-bright (M > 10(11) M circle dot) galaxies were already in place at z similar or equal to 1.2, at least in the central regions of X-ray luminous clusters. Together with recent results on the field galaxy stellar mass function, this implies that most of the stellar mass is already assembled in massive galaxies by z similar or equal to 1, both in low and high density environments.I documenti in SFERA sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
