We present the 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 measure the two-point real-space correlation function w _ { p } ( r _ { p } ) for four volume-limited sub-samples selected by stellar mass and four volume-limited sub-samples 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 measure a correlation length r _ { 0 } = 2.87 \pm 0.22 h ^ { -1 } Mpc and slope \gamma = 1.59 \pm 0.07 , while for the most luminous ( M _ { UV } < -20.2 ) r _ { 0 } = 5.35 \pm 0.50 h ^ { -1 } Mpc and \gamma = 1.92 \pm 0.25 .
This corresponds to a strong relative bias between these two sub-samples of \Delta b / b ^ { * } = 0.43 .
Fitting a 5-parameter HOD model we find that the most luminous ( M _ { UV } < -20.2 ) and massive ( M _ { \star } > 10 ^ { 10 } h ^ { -1 } M _ { \sun } ) galaxies occupy the most massive dark matter haloes with \langle M _ { h } \rangle = 10 ^ { 12.30 } h ^ { -1 } M _ { \sun } .
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 _ { \sun } to M _ { min } = 10 ^ { 11.58 } h ^ { -1 } M _ { \sun } 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 \sim 3 , we observe that the masses at which a halo hosts , on average , one satellite and one central galaxy is M _ { 1 } \approx 4 M _ { min } over all luminosity ranges , significantly lower than observed at z \sim 0 indicating 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 .