2006/12/12 by A. Pollo, L. Guzzo, Pollo, A. +9
Physics and Astronomy · #Astronomy and Astrophysical Research #Galaxies: Formation, Evolution, Phenomena #Gamma-ray bursts and supernovae #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0612313
2 pages, 2 figures, to appear in the proceedings of the "Cosmic Frontiers" conference, Durham, August 2006
arxiv created 2006/12/12 · arxiv updated 2009/12/01
We have investigated the dependence of galaxy clustering on their intrinsic luminosities at z ~ 1, using the data from the First Epoch VIMOS-VLT Deep Survey (VVDS). We have measured the projected two-point correlation function of galaxies, wp(rp), for a set of volume-limited samples at an effective redshift <z>=0.9 and median absolute magnitude -19.6< MB < -21.3. We find that the clustering strength is rising around MB^*, apparently with a sharper turn than observed at low redshifts. The slope of the correlation function is observed to steepen significantly from γ=1.6+0.1-0.1 to γ=2.4+0.4-0.2. This is due to a significant change in the shape of wp(rp), increasingly deviating from a power-law for the most luminous samples, with a strong upturn at small (< 1-2 h-1 Mpc) scales. This trend, not observed locally, also results in a strong scale dependence of the relative bias, b/b* and possibly imply a significant change in the way luminous galaxies trace dark-matter halos at z ~ 1 with respect to z ~ 0.