KECK DEEP FIELDS. IV. LUMINOSITY-DEPENDENT CLUSTERING AND GALAXY DOWNSIZING IN UV-SELECTED GALAXIES AT z=4, 3, AND 2

We investigate the luminosity-dependent clustering of rest-frame UV-selected galaxies at z similar to 4, 3, 2.2, and 1.7 in the Keck Deep Fields, which are complete to R = 27 and cover 169 arcmin(2). We find that at z similar to 4 and 3, UV-bright galaxies cluster more strongly than UV-faint ones, but at z similar to 2.2 and 1.7, the UV-bright galaxies are no longer the most strongly clustered. We derive mass estimates for objects in our sample by comparing our measurements to the predicted clustering of dark matter halos in the Millennium Simulation. From these estimates, we infer relationships between halo mass and star formation rate (SFR), and find that the most massive dark matter halos in our sample host galaxies with high SFRs (M-1700 < -20, or > 50 M-circle dot yr(-1)) at z similar to 3 and 4, moderate SFRs (-20 < M-1700 < -19, or similar to 20 M-circle dot yr(-1)) at z similar to 2.2, and lower SFRs (-19 < M-1700 < -18, or similar to 2M(circle dot) yr(-1)) at z similar to 1.7. We believe our measurements may provide a new line of evidence for galaxy downsizing by extending that concept from stellar to halo mass. We also find that the objects with blue UV colors in our sample are much more strongly clustered than those with red UV colors, and we propose that this may be due to the presence of the 2175 angstrom dust absorption bump in more massive halos, which contain the older stellar populations and dust needed to produce the feature. The relatively small area covered by the survey means that the absolute values of the correlation lengths and halo masses we derive are heavily dependent on the "integral constraint" correction, but the uniformly deep coverage across a large-redshift interval allows us to detect several important trends that are independent of this correction.