Galaxy clustering determined from numerical cosmological simulations
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.
Cite
@article{arxiv.astro-ph/9906039,
title = {Galaxy clustering determined from numerical cosmological simulations},
author = {Adrian Jenkins and C. S. Frenk and F. R. Pearce and P. A. Thomas and J. M. Colberg and S. D. M. White and H. M. P. Couchman and J. A. Peacock and G. Efstathiou and A. H. Nelson},
journal= {arXiv preprint arXiv:astro-ph/9906039},
year = {2007}
}
Comments
4 pages, Proceedings X Rencontres de Blois: The Birth of Galaxies