LARGE-SCALE STRUCTURE OF THE UNIVERSE

The current situation with the cosmological model and fundamental cons tants is briefly reviewed. Here, we concentrate on evolutionary effect s of large-scale structure formation, in particular, the relationship with the quasar distribution and dynamics is discussed. We argue that groups of bright quasars with few or more than dozen of members within regions less than or equal to l(LS) similar to (100-150)h(-1) Mpc fou nd at z < 2 may belong to concentrations of young rich clusters of gal axies, and thus be distant Great Attractors like the local GA or the S hapley concentration. These early large-scale galactic structures (i) provide a natural way to 'bias' the distribution of Abell clusters, an d (ii) suggest that the spectrum of primordial density perturbations i s nearly flat on scales encompassing both the cluster and GAs, l = pi k(-1) is an element of (10, 100)h(-1) Mpc: Delta(k)(2) similar to k(3) P(k) similar to k(gamma), gamma = 1(-0.4)(+0.6), where P(k) is the pow er spectrum of density perturbations.