Evolution of the 3.6 micron Cluster Luminosity Function
| dc.creator | Muzzin, Adam | |
| dc.creator | Wilson, Gillian | |
| dc.creator | Lacy, Mark | |
| dc.date | 2005-03-29 | |
| dc.date.accessioned | 2026-07-07T02:17:20Z | |
| dc.date.available | 2026-07-07T02:17:20Z | |
| dc.description | We have measured the 3.6 micron cluster luminosity function (LF) using a sample of 123 galaxy clusters selected from the 4 degree^2 Spitzer First Look Survey (FLS). The clusters were selected on the basis of their R - 3.6 micron colors using the cluster red-sequence technique of Gladders & Yee (2000). The binned LFs are well-fit by a Schechter function at all redshifts. However, we note two interesting trends. Firstly, the evolution of Mstar with redshift is consistent with models that form galaxies in a single-burst of star-formation at z > 2.0, and evolve passively thereafter. Secondly, the faint-end slope of the LF appears to become shallower at higher redshift. We conclude that the most massive galaxies were formed in the cluster at high redshift (z > 2), while lower-mass galaxies have subsequently been accreted from the field at lower redshift (z ~ 0.5). These results are consistent with the ``downsizing'' picture seen in previous cluster studies using smaller samples. | |
| dc.description | To appear in the conference proceedings "Spitzer Space Telescope: New Views of the Universe, held Nov. 2004 in Pasadena, 2 pages including 1 figure | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0503640 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0503640 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/9136 | |
| dc.subject | Astrophysics | |
| dc.title | Evolution of the 3.6 micron Cluster Luminosity Function | |
| dc.type | text |