The DEEP2 Galaxy Redshift Survey: Color and Luminosity Dependence of Galaxy Clustering at \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \Decl

Abstract

We present measurements of the color and luminosity dependence of galaxy clustering at z $ 1 in the DEEP2 Galaxy Redshift Survey. Using volume-limited subsamples in bins of both color and luminosity, we find the following: (1) The clustering dependence is much stronger with color than with luminosity and is as strong with color at z $ 1 as is found locally. We find no dependence of the clustering amplitude on color for galaxies on the red sequence, but a significant dependence on color for galaxies within the blue cloud. (2) For galaxies in the range L/L Ã $ 0:7Y2, a stronger largescale luminosity dependence is seen for all galaxies than is seen for red and blue galaxies separately. The small-scale clustering amplitude depends significantly on luminosity for blue galaxies, with brighter samples having a stronger rise on scales r p < 0:5 h À1 Mpc. (3) Redder galaxies exhibit stronger small-scale redshift-space distortions (''fingers of god''), and both red and blue populations show large-scale distortions in (r p ; ) due to coherent infall. (4) While the clustering length, r 0 , increases smoothly with galaxy color (in narrow bins), its power-law exponent, , exhibits a sharp jump from the blue cloud to the red sequence. The intermediate-color ''green'' galaxy population likely includes transitional galaxies moving from the blue cloud to the red sequence; on large scales green galaxies are as clustered as red galaxies but show infall kinematics and a small-scale correlation slope akin to the blue galaxy population. (5) We compare our results to a semianalytic galaxy formation model applied to the Millennium Run simulation. Differences between the data and the model suggest that in the model star formation is shut down too efficiently in satellite galaxies.

Comparison of the VIMOS-VLT Deep Survey with the Munich semi-analytical model

“…These studies highlight a number of discrepancies between model predictions and observations. In particular, Coil et al (2008) show that red model galaxies are more strongly clustered than observed at z 1, particularly on small scales. Blue galaxies in the model show instead a lower clustering strength than observed, suggesting a significant deficit of blue satellite galaxies in the semi-analytical model of Croton et al (2006).…”

“…Here, the very prominent 1-halo term may be due to an overabundance of red satellite galaxies. Similarly, Coil et al (2008) find an absence of "Finger of God" (FoG, Jackson 1972) in the correlation function of blue model galaxies at z 1 at variance with red model galaxies, which have a very strong FoG. The FoG effect is associated with the infall of satellite galaxies inside haloes and its strength is related to the abundance of satellite galaxies (e.g.…”

“…the different clustering of red and blue galaxies (Springel et al 2005). For the highredshift Universe, only few data-model comparisons have been carried out (McCracken et al 2007;Coil et al 2008;Meneux et al 2008Meneux et al , 2009. These studies highlight a number of discrepancies between model predictions and observations.…”

Dusty star-forming galaxies at high redshift

“…Figure 39: Auto-correlation length r 0 of DSFGs compared to a variety of galaxy populations over the redshift interval 0 < z < 3. These include optically-selected SDSS QSOs at 0 < z < 3 (Myers et al, 2006;Ross et al, 2009) Lyman-break galaxies (Adelberger et al, 2005), MIPS 24 µm-selected star-forming galaxies at 0 < z < 1.4 , AGES and DEEP2 red and blue galaxies at 0.25 < z < 1 from the AGES (Hickox et al, 2009;Coil et al, 2008) SDSS-selected luminous red galaxies (LRGs) at 0 < z < 0.7 (Wake et al, 2008), and optically-selected galaxy clusters at 0.1 < z < 0.3 (Estrada et al, 2009). The figure also shows the r 0 for low-redshift galaxies with r-band luminosities in the range 1.5 to 3.5 L , derived from the luminosity dependence of clustering (Zehavi et al, 2011).…”

Quantifying the colour-dependent stochasticity of large-scale structure

“…Taking the square root of the ratios of the autocorrelations yields estimates of the relative bias b rel between red and blue galaxies (e.g., Croton et al 2007;Coil et al 2008;Guo et al 2013;Skibba et al 2014). Constructing the correlation coefficient, r ξ , we find:…”