The VIMOS Ultra Deep Survey Luminosity and stellar mass dependence of galaxy clustering at z ∼ 3

We present a study of the dependence of galaxy clustering on luminosity and stellar mass in the redshift range 2 < z < 3.5 using 3236 galaxies with robust spectroscopic redshifts from the VIMOS Ultra Deep Survey (VUDS), covering a total area of 0.92 deg(2). We measured the two-point real-space correlation function w(p)(r(p)) for four volume-limited subsamples selected by stellar mass and four volume-limited subsamples selected by M-uv absolute magnitude. We find that the scale-dependent clustering amplitude r(0) significantly increases with increasing luminosity and stellar mass. For the least luminous galaxies (M-uv < -19.0), we measured a correlation length r(0) = 2.87 +/- 0.22 h(-1) Mpc and slope gamma = 1.59 +/- 0.07, while for the most luminous (M-uv < -20.2) r(0) = 5.35 +/- 0.50 h(-1) Mpc and gamma = 1.92 +/- 0.25. These measurements correspond to a strong relative bias between these two subsamples of Delta b/b* = 0.43. Fitting a five-parameter halo occupation distribution (HOD) model, we find that the most luminous (M-uv < -20.2) and massive (M-* > 10h(-1) M-circle dot) galaxies occupy the most massive dark matter haloes with < M-h > = 10(12.30) h(-1) M-circle dot. Similar to the trends observed at lower redshift, the minimum halo mass M-min depends on the luminosity and stellar mass of galaxies and grows from M-min = 10 9.73 h(-1) M-circle dot to M-min = 10(11.58) h(-1) M circle dot from the faintest to the brightest among our galaxy sample, respectively. We find the difference between these halo masses to be much more pronounced than is observed for local galaxies of similar properties. Moreover, at z similar to 3, we observe that the masses at which a halo hosts, on average, one satellite and one central galaxy is M-1 approximate to 4M(min) over all luminosity ranges, which is significantly lower than observed at z similar to 0; this indicates that the halo satellite occupation increases with redshift. The luminosity and stellar mass dependence is also reflected in the measurements of the large-scale galaxy bias, which we model as b(g.HOD)(>L) = 1.92 + 25.36(L/L*)(7.01). We conclude our study with measurements of the stellar-to-halo mass ratio (SHMR). We observe a significant model-observation discrepancy for low-mass galaxies, suggesting a higher than expected star formation efficiency of these galaxies.