2008/10/23 by D. Harsono, Daniel Harsono, Roberto De Propris
Physics and Astronomy · #Astronomy and Astrophysical Research #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1088/0004-6256/137/2/3091
Accepted by AJ. Only a selection of figures shown in paper: extra figures to be made available on the AJ web site. Email R. De Propris for them in the meantime. Fig. 1 could not be compressed to arXiv size limits. See note in caption for how to obtain it
arxiv created 2008/10/23 · openalex publication_date 2009/01/14 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We present deep composite luminosity functions (LFs) in B , g , V , r , i , and z for six clusters at 0.14 < z < 0.40 observed with the Hubble Space Telescope Advanced Camera for Surveys. The LFs reach to an absolute magnitude of ∼−14 + 5log h mag and are well fitted by a single Schechter function with M * BgVriz = −19.8, − 20.9 − 21.9, − 22.0, − 21.7, − 22.3 mag, respectively, and α ∼ −1.3 (in all bands). The observations suggest that the galaxy LF is dominated by objects on the red sequence to at least 6 mag below the L * point. Comparison with local data shows that the red sequence is well established at least at z ∼ 0.3 down to ∼ 1/600th of the luminosity of the Milky Way and that galaxies down to the regime of dwarf spheroidals have been completely assembled in clusters at this redshift. We do not detect a steepening of the LF at M > − 16, as is locally observed. If the faint-end upturn is real, the steepening of the LF must be due to a newly infalling population of faint dwarf galaxies.