  We investigate the luminosity dependent clustering of rest-frame UV selected
galaxies at z~4, 3, 2.2, and 1.7 in the Keck Deep Fields (KDFs), which are
complete to R = 27 and cover 169 arcmin^2. We find that at z~4 and 3, UV-bright
galaxies cluster more strongly than UV-faint ones, but at z~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 haloes 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 haloes in our sample
host galaxies with high SFRs (M_1700 < -20, or > 50 M_sun/yr) at z~3 and 4,
moderate SFRs (-20<M_1700<-19, or ~20 M_sun/yr) at z~2.2, and lower SFRs
(-19<M_1700<-18, or ~2 M_sun/yr) at z~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 2175A 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.
