Galaxy clustering determined from numerical cosmological simulations Academic Article uri icon

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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.

authors

  • Jenkins, Adrian
  • Frenk, CS
  • Pearce, FR
  • Thomas, PA
  • Colberg, JM
  • White, SDM
  • Couchman, Hugh M
  • Peacock, JA
  • Efstathiou, G
  • Nelson, AH