  High resolution $N$-body simulations for variants of the CDM model are used
to derive the redshift dependence of galaxy formation and of galaxy correlation
functions. The reconstructed power spectra and clustering properties provide a
sensible test for the underlying power spectra. We compare our simulations with
new results of the analysis of recent redshift surveys. The results are used to
discuss the model of primordially broken scale invariant perturbations (BSI).
