  In this review, I outline the use of galaxy correlations to constrain
cosmological parameters. As with the Cosmic Microwave Background (CMB), the
density of dark and baryonic matter imprints important scales on the
fluctuations of matter and thus the clustering of galaxies, e.g., the particle
horizon at matter--radiation equality and the sound horizon at recombination.
Precision measurements of these scales from the Baryon Acoustic Oscillations
(BAO) and the large scale shape of the power spectrum of galaxy clustering
provide constraints on Omega_m h^2. Recent measurements from the Sloan Digital
Sky Survey (SDSS) and 2dF Galaxy Redshift Survey (2dFGRS) strongly suggest that
Omega_m < 0.3. This forms the basic evidence for a flat Universe dominated by a
Cosmological Constant (Lambda) today (when combined with results from the CMB
and supernova surveys). Further evidence for this cosmological model is
provided by the late-time Integrated Sachs-Wolfe (ISW) effect, which has now
been detected using a variety of tracers of the large scale structure in the
Universe out to redshifts of z>1. The ISW effect also provides an opportunity
to discriminate between Lambda, dynamical dark energy models and the
modification of gravity on large scales.
