MODELING GALAXY CLUSTERING AT HIGH-REDSHIFT

We discuss the theoretical interpretation of observational data concer ning the clustering of galaxies at high redshifts. Building on the the oretical machinery developed by Matarrese et al., we make detailed qua ntitative predictions of galaxy clustering statistics for a variety of cosmological models, taking into account differences in spatial geome try and initial fluctuation spectra and exploring the role of bias as a complicating factor in these calculations. We demonstrate that the u sual description of evolution (in terms of the parameters epsilon and r(0)) is not useful for realistic galaxy clustering models. We compare the detailed predictions of the variation of correlation functions wi th redshift against current observational data to constrain available models of structure formation. Theories that fit the present-day abund ance of rich clusters are generally compatible with the observed redsh ift evolution of galaxy clustering if galaxies are no more than slight ly biased at z similar to 1, We also discuss the interpretation of a c oncentration of Lyman-break galaxies found by Steidel et al., coming t o the conclusion that such concentrations are not unexpected in 'stand ard' models of structure formation.