The VIMOS VLT Deep Survey: Evolution of the non-linear galaxy bias up to z=1.5

TL;DR

This study measures galaxy density fluctuations and bias evolution up to redshift 1.5, revealing increasing bias with redshift, non-linear bias effects, and the influence of density thresholds on galaxy formation.

Contribution

First measurement of galaxy fluctuation PDF and bias evolution up to z=1.5, highlighting non-linear bias effects and their dependence on redshift and scale.

Findings

Galaxy bias increases with redshift, especially beyond z=0.8.

Biasing function is non-linear across all investigated redshifts.

Formation of bright galaxies is suppressed below a density threshold that grows with redshift.

Abstract

We present the first measurements of the Probability Distribution Function (PDF) of galaxy fluctuations in the VIMOS-VLT Deep Survey (VVDS) cone, covering 0.4x0.4 deg between 0.4<z<1.5. The second moment of the PDF, i.e. the rms fluctuations of the galaxy density field, is with good approximation constant over the full redshift baseline investigated: we find that, in redshift space, sigma_8 for galaxies brighter than M=-20+5log h has a mean value of 0.94\pm0.07 in the redshift interval 0.7<z<1.5. The third moment, i.e. the skewness, increases with cosmic time: we find that the probability of having underdense regions is greater at z~0.7 than it was at z~1.5. By comparing the PDF of galaxy density contrasts with the theoretically predicted PDF of mass fluctuations we infer the redshift-, density-, and scale-dependence of the biasing function b(z, \delta, R) between galaxy and matter overdensities up to redshift z=1.5. Our results can be summarized as follows: i) the galaxy bias is an increasing function of redshift: evolution is marginal up to z~0.8 and more pronounced for z>0.8; ii) the formation of bright galaxies is inhibited below a characteristic mass-overdensity threshold whose amplitude increases with redshift and luminosity; iii) the biasing function is non linear in all the redshift bins investigated with non-linear effects of the order of a few to 10% on scales >5Mpc.