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 ∼5000 passively evolving (PE) galaxies selected from ∼2.5 deg2 of deep (K lim = 23–24 AB) Canada–France–Hawaii Telescope 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 haloes. In contrast, at rest-frame ultraviolet 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 haloes. 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.