Astronomy and Astrophysics – Astronomy
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.5002b&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #50.02; Bulletin of the American Astronomical Society, Vol. 24, p.811
Astronomy and Astrophysics
Astronomy
Scientific paper
The two-point spatial correlation function, xi (r), of dark galaxy halos in a cold dark matter universe is determined as a function of halo mass using N-body simulations. A linear bias model is found to be a good description of the formation of halos with overdensity ~ 200, but not for halos with overdensities ~ 2000 or ~ 70. High mass halos are more biased than low mass halos in a universe in which 1/sigma_8 = 2.5 (in mass), while in a universe in which 1/sigma_8 = 1.5 (in mass), high and low mass halos are biased to the same degree. Assuming a constant mass to light ratio and that one luminous galaxy would form in each of the halos, this implies that the degree to which bright galaxies are more strongly clustered than faint galaxies is a function of sigma_8 . Therefore, in order to determine sigma_8 for the mass in the universe, it is essential to compare xi (r) for bright galaxies to xi (r) of faint galaxies. xi (r) for low mass halos shows more evolution with redshift than xi (r) for high mass halos, but less than linear theory predicts. Thus, we expect xi (r) for faint galaxies to show more evolution with redshift than xi (r) for bright galaxies.
Brainerd Tereasa G.
Villumsen Jens Verner
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