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Galaxy clustering determined from numerical cosmological simulations | | Adrian Jenkins
; C.S. Frenk
; F.R. Pearce
; P.A. Thomas
; J.M. Colberg
; S.D.M. White
; H.M.P. Couchman
; J.A. Peacock
; G. Efstathiou
; A.H. Nelson
; | | Date: |
2 Jun 1999 | | Subject: | astro-ph | | Affiliation: | Durham), C.S. Frenk (Durham), F.R. Pearce (Durham), P.A. Thomas (Sussex), J.M. Colberg (MPA), S.D.M. White (MPA), H.M.P. Couchman (UWO), J.A. Peacock (Edinburgh), G. Efstathiou (Cambridge) and A.H. Nelson (Cardiff)(The Virgo consortium | | 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. | | Source: | arXiv, astro-ph/9906039 | | Services: | Forum | Review | PDF | Favorites | |
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