AAS Meeting #193 - Austin, Texas, January 1999
Session 39. Cosmology/Large Scale Structure
Display, Thursday, January 7, 1999, 9:20am-6:30pm, Exhibits Hall 1

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[39.13] Evolution of Galaxy Clustering and of Metallicity in the Universe

R Cen (Princeton University)

Using the state-of-the-art, large-scale, high resolution cosmological, hydrodynamic galaxy formation simulations of a cosmological constant dominated cold dark matter model, we compute the evolution of galaxy clustering. Physical bias of galaxies and correlation function of galaxies are both computed. We find that bias is a strongly increasing function of redshift, consistent with observations at both low (z=0) and high redshift (z=3). The correlation function of galaxies as a function of comoving separation, on the other hand, is nearly non-evolving, in agreement with a host of observations in the redshift range z=0-3.

We also self-consistently compute the dynamics of metals that are produced in the galaxies and allowed to feedback to the intergalactic medium through galactic winds or supernovae. We are therefore able to follow the metallicity evolution in different cosmic regions ranging from clusters and groups of galaxies, filaments of galaxies, Lyman alpha clouds to low density ``voids". It is found that the evolution of metallicity is strongly density dependent and there is no universal evolution. For comparisons with observations, when available, we find good agreement.

The author(s) of this abstract have provided an email address for comments about the abstract: cen@astro.princeton.edu

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