Galaxy clustering determined from numerical cosmological simulations

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dc.creatorJenkins, Adrian
dc.creatorFrenk, C. S.
dc.creatorPearce, F. R.
dc.creatorThomas, P. A.
dc.creatorColberg, J. M.
dc.creatorWhite, S. D. M.
dc.creatorCouchman, H. M. P.
dc.creatorPeacock, J. A.
dc.creatorEfstathiou, G.
dc.creatorNelson, A. H.
dc.date1999-06-02
dc.date.accessioned2026-07-07T02:31:48Z
dc.date.available2026-07-07T02:31:48Z
dc.descriptionWe 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.
dc.description4 pages, Proceedings X Rencontres de Blois: The Birth of Galaxies
dc.identifierhttps://arxiv.org/abs/astro-ph/9906039
dc.identifierhttp://arxiv.org/abs/astro-ph/9906039
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/14286
dc.subjectAstrophysics
dc.titleGalaxy clustering determined from numerical cosmological simulations
dc.typetext

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