Galaxy-Galaxy Lensing Predictions from the Semi-Analytic Galaxy Formation Models

luminosity and the halo mass. The cross-correlation cannot, however, be used to infer the halo profile directly because different halo masses dominate on different scales and because not all galaxies are at the centres of the corresponding haloes. We compute the redshift evolution of the cross-correlation amplitude and compare it with those of galaxies and dark matter. We also compute the galaxy‐dark matter correlation coefficient and show that it is close to unity on scales above 1 h 21 Mpc for all considered galaxy types. This would allow one to extract the bias and the dark matter power spectrum on large scales from the galaxy and galaxy‐dark matter correlations.