Angular clustering of z~2 star-forming and passive galaxies in 2.5
  square degrees of deep CFHT imaging
  We study the angular clustering of z~2 galaxies using ~40,000 star-forming
(SF) and ~5,000 passively-evolving (PE) galaxies selected from ~2.5 deg$^2$ of
deep ($K_{lim}$=23-24 AB) CFHT imaging. For both populations the clustering is
stronger for galaxies brighter in rest-frame optical and the trend is
particularly strong for PE galaxies, indicating that passive galaxies with
larger stellar masses reside in more massive halos. In contrast, at rest-frame
UV we find that while the clustering of SF galaxies increases with increasing
luminosity, it decreases for PE galaxies; a possible explanation lies in
quenching of star formation in the most massive halos. Furthermore, we find two
components in the correlation functions for both SF and PE galaxies,
attributable to one- and two-halo terms. The presence of one-halo terms for
both PE and SF galaxies suggests that environmental effects were producing
passive galaxies in virtualized environments already by z~2. Finally, we find
notable clustering differences between the four widely-separated fields in our
study; the popular COSMOS field is the most discrepant (as is also the case for
number counts and luminosity functions), highlighting the need for very large
areas and multiple sightlines in galaxy evolution statistical studies.
