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We present measurements of projected autocorrelation functions   w  p ( r  p )  for the stellar mass of galaxies and for their light in the  U ,  B  and  V  bands, using data from the third data release of the DEEP2 Galaxy Redshift Survey and the final data release of the Sloan Digital Sky Survey (SDSS). We investigate the clustering bias of stellar mass and light by comparing these to projected autocorrelations of dark matter estimated from the Millennium Simulations (MS) at  z = 1 and 0.07, the median redshifts of our galaxy samples. All of the autocorrelation and bias functions show systematic trends with spatial scale and waveband which are impressively similar at the two redshifts. This shows that the well‐established environmental dependence of stellar populations in the local Universe is already in place at  z = 1. The recent MS‐based galaxy formation simulation of Guo et al. reproduces the scale‐dependent clustering of luminosity to an accuracy better than 30 per cent in all bands and at both redshifts, but substantially overpredicts mass autocorrelations at separations below about 2 Mpc. Further comparison of the  shapes  of our stellar mass bias functions with those predicted by the model suggests that both the SDSS and DEEP2 data prefer a fluctuation amplitude of σ 8 ∼ 0.8 rather than the σ 8 = 0.9 assumed by the MS.

Autocorrelations of stellar light and mass at z ∼ 0 and ∼1: from SDSS to DEEP2