How galaxies trace large scale structure at z\sim3?

We study the dependence of galaxy clustering on luminosity and stellar mass in the redshift range $2<z<3.5$ based on spectroscopic data from the VIMOS Ultra Deep Survey (VUDS).

In our work, by applying halo occupation distribution (HOD) models to the correlation function measurements for different galaxy samples, we showed how dark matter halo mass and large scale bias depend on luminosity and stellar mass of galaxies and how this dependence changes with redshift.

Additionally, we measured the stellar-to-halo mass ratio (SHMR) and found a significant model-observation discrepancy for low-mass galaxies at $z\sim3$, suggesting a higher than expected star formation efficiency of these galaxies.