  The coupling of photons and baryons by Thomson scattering in the early
universe imprints features in both the Cosmic Microwave Background (CMB) and
matter power spectra. The former have been used to constrain a host of
cosmological parameters, the latter have the potential to strongly constrain
the expansion history of the universe and dark energy. Key to this program is
the means to localize the primordial features in observations of galaxy spectra
which necessarily involve galaxy bias, non-linear evolution and redshift space
distortions. We present calculations, based on mock catalogues produced from
particle-mesh simulations, which show the range of behaviors we might expect of
galaxies in the real universe. We find that non-linearity, galaxy bias and
redshift space distortions all introduce important modifications to the basic
picture. Both the galaxy bias and the (isotropic) redshift space distortions
lead to relatively smooth modulations in power on the scales of interest to
baryon oscillations. The halo and galaxy power spectra exhibit low order
structure beyond the acoustic oscillations over the range of scales of
relevance. Fitting a cubic polynomial to the ratio of galaxy to dark matter
power reduces any remaining structure in the range 0.03<k<0.3 h/Mpc below the 2
per cent level, which is close to the error in our calculations.
