2005/12/31 by Alison L. Coil, Jeffrey A. Newman, Michael C. Cooper +5 · 4 citations
Physics and Astronomy · #Artificial intelligence #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Cluster analysis #Computer science #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gamma-ray bursts and supernovae #Luminosity function #Physics #Redshift #Redshift survey #astro-ph
paper · pdf · doi:10.1086/503601
published as Astrophys.J.654:115-124,2006 · 13 pages, 3 figures, accepted to ApJ
openalex publication_date 2006/06/19 · arxiv created 2006/09/12 · arxiv updated 2014/10/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We measure the clustering of DEEP2 galaxies at z = 1 as a function of luminosity on scales 0.1-20 h -1 Mpc. Drawing from a parent catalog of 25,000 galaxies at 0.7 < z < 1.3 in the full DEEP2 survey, we create volume-limited samples having upper luminosity limits between M B = -19 and -20.5, roughly 0.2-1 L * at z = 1. We find that brighter galaxies are more strongly clustered than fainter galaxies and that the slope of the correlation function does not depend on luminosity for L < L *. The brightest galaxies, with L > L *, have a steeper slope. The clustering scale length, r 0 , varies from 3.69 ± 0.14 for the faintest sample to 4.43 ± 0.14 for the brightest sample. The relative bias of galaxies as a function of L / L * is steeper than the relation found locally for SDSS galaxies by Zehavi et al. in 2005 over the luminosity range that we sample. The absolute bias of galaxies at z ~ 1 is scale dependent on scales r p < 1 h -1 Mpc, and rises most significantly on small scales for the brightest samples. For a concordance cosmology, the large-scale bias varies from 1.26 ± 0.04 to 1.54 ± 0.05 as a function of luminosity and implies that DEEP2 galaxies reside in dark matter halos with a minimum mass of ~ × 10 12 h -1 M ☉ .