2015ApJ...806..189K

We study the dependence of angular two-point correlation functions on stellar mass (M_*) and specific star formation rate (sSFR) of M_* > 10¹⁰ M_☉ galaxies at z ∼ 1. The data from the UK Infrared Telescope Infrared Deep Sky Survey Deep eXtragalactic Survey and Canada-France-Hawaii Telescope Legacy Survey cover 8.2 deg² sample scales larger than 100 h^–1 Mpc at z ∼ 1, allowing us to investigate the correlation between clustering, M_*, and star formation through halo modeling. Based on halo occupation distributions (HODs) of M_* threshold samples, we derive HODs for M_*binned galaxies, and then calculate the M_*/M_halo ratio. The ratio for central galaxies shows a peak at M_halo, and satellites predominantly contribute to the total stellar mass in cluster environments with M_*/M_halo values of 0.01-0.02. Using star-forming galaxies split by sSFR, we find that main sequence galaxies (log sSFR/yr ∼ 9) are mainly central galaxies in ∼ 10^12.5h^–1M_☉ halos with the lowest clustering amplitude, while lower sSFR galaxies consist of a mixture of both central and satellite galaxies where those with the lowest M_* are predominantly satellites influenced by their environment. Considering the lowest M_halo samples in each M_*bin, massive central galaxies reside in more massive halos with lower sSFRs than low mass ones, indicating star-forming central galaxies evolve from a low M_*-high sSFR to a high M_*-low sSFR regime. We also find that the most rapidly star-forming galaxies ((log sSFR/yr > -8.5) are in more massive halos than main sequence ones, possibly implying galaxy mergers in dense environments are driving the active star formation. These results support the conclusion that the majority of star-forming galaxies follow secular evolution through the sustained but decreasing formation of stars.