Galaxy clustering determined from numerical cosmological simulations
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abstract
We have simulated the growth of structure in two 100 Mpc boxes for LCDM and
SCDM universes. These N-body/SPH simulations include a gaseous component which
is able to cool radiatively. A fraction of the gas cools into cold dense
objects which we identify as galaxies. In this article we give a preliminary
analysis of the clustering behaviour of these galaxies concentrating on the
LCDM model. We find a galaxy correlation function which is very close to a
power law and which evolves relatively little with redshift. The pairwise
dispersions of the galaxies are significantly lower than the dark matter. The
LCDM model gives a surprisingly good match to the observational determinations
of the galaxy correlation function and pairwise dispersions.