Clustering, host halos, and environment of z ∼ 2 galaxies as a function of their physical properties

Using a sample of 25 683 star-forming and 2821 passive galaxies at z similar to 2, selected in the COSMOS field following the BzK color criterion, we study the hosting halo mass and environment of galaxies as a function of their physical properties. Spitzer and Herschel allow us to obtain accurate star formation rate estimates for starburst galaxies. We measure the autocorrelation and cross-correlation functions of various galaxy subsamples and infer the properties of their hosting halos using both a halo occupation model and the linear bias at large scale. We find that passive and star-forming galaxies obey a similarly rising relation between the halo and stellar mass. The mean host halo mass of star-forming galaxies increases with the star formation rate between 30 M-circle dot yr(-1) and 200 M-circle dot yr(-1), but flattens for higher values, except if we select only main-sequence galaxies. This reflects the expected transition from a regime of secular coevolution of the halos and the galaxies to a regime of episodic starburst. We find similar large-scale biases for main-sequence, passive, and starburst galaxies at equal stellar mass, suggesting that these populations live in halos of the same mass. However, we detect an excess of clustering on small scales for passive galaxies and showed, by measuring the large-scale bias of close pairs of passive galaxies, that this excess is caused by a small fraction (similar to 16%) of passive galaxies being hosted by massive halos (similar to 3 x 10(13) M-circle dot) as satellites. Finally, extrapolating the growth of halos hosting the z similar to 2 population, we show that M-star similar to 10(10) M-circle dot galaxies at z similar to 2 will evolve, on average, into massive (M-star similar to 10(11) M-circle dot), field galaxies in the local Universe and M. similar to 10(11) M-circle dot galaxies at z = 2 into local, massive, group galaxies. We also identify two z similar to 2 populations which should end up in today's clusters: massive (>M-star similar to 10(11) M-circle dot), strongly star-forming (> 200 M-circle dot yr(-1)), main-sequence galaxies, and close pairs of massive, passive galaxies.