We examine the distribution of stellar masses of galaxies in MS 1054.4 - 0321 and Cl 0152.7 - 1357, two X-ray-selected clusters of galaxies at z = 0.83. Our stellar mass estimates, from spectral energy distribution fitting, reproduce the dynamical masses as measured from velocity dispersions and half-light radii with a scatter of 0.2 dex in the mass for early-type galaxies. When we restrict our sample of members to high stellar masses, those over 10(11.1) M-circle dot (M* in the Schechter mass function for cluster galaxies), we find that the fraction of early-type galaxies is 79% +/- 6% at z = 0.83 and 87% +/- 6% at z = 0.023 for the Coma Cluster, consistent with no evolution. Previous work with luminosity-selected samples has found that the early-type fraction in rich clusters declines from similar or equal to 80% at z = 0 to similar or equal to 60% at z = 0.8. The observed evolution in the early-type fraction from luminosity-selected samples must predominantly occur among sub-M* galaxies. As M* for field and group galaxies, especially late types, is below M* for cluster galaxies, infall could explain most of the recent growth in the early-type fraction. Future surveys could determine the morphological distributions of lower mass systems, which would confirm or refute this explanation.
The possible z=0.83 precursors of z=0, M* early-type cluster galaxies
ROSATI, Piero;
2006
Abstract
We examine the distribution of stellar masses of galaxies in MS 1054.4 - 0321 and Cl 0152.7 - 1357, two X-ray-selected clusters of galaxies at z = 0.83. Our stellar mass estimates, from spectral energy distribution fitting, reproduce the dynamical masses as measured from velocity dispersions and half-light radii with a scatter of 0.2 dex in the mass for early-type galaxies. When we restrict our sample of members to high stellar masses, those over 10(11.1) M-circle dot (M* in the Schechter mass function for cluster galaxies), we find that the fraction of early-type galaxies is 79% +/- 6% at z = 0.83 and 87% +/- 6% at z = 0.023 for the Coma Cluster, consistent with no evolution. Previous work with luminosity-selected samples has found that the early-type fraction in rich clusters declines from similar or equal to 80% at z = 0 to similar or equal to 60% at z = 0.8. The observed evolution in the early-type fraction from luminosity-selected samples must predominantly occur among sub-M* galaxies. As M* for field and group galaxies, especially late types, is below M* for cluster galaxies, infall could explain most of the recent growth in the early-type fraction. Future surveys could determine the morphological distributions of lower mass systems, which would confirm or refute this explanation.I documenti in SFERA sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
