Disk galaxies at Z=0 and at High Redshift: an explanation of the observed evolution of damped Ly-alpha systems

Abstract

The analysis of disk formation is based on the White & Rees (1978) picture, in which disk galaxies form by continuous cooling and accretion of gas within a merging hierarchy of dark matter halos. A simple Kennicutt law of star formation for disks, based on a single- fluid gravitational instability model is introduced. Since the gas supply in the disk is regulated by infall from the surrounding halo, the gas is always maintained at a critical threshold surface density. Chemical enrichment of the disks occurs when the surrounding hot halo gas is enriched with heavy elements ejected during surpernova explosions. This gas then cools onto the disk producing a new generation of metal-rich stars. I first show that models of this type can reproduce many of the observed properties of a typical spiral galaxy like the Milky Way, including its gas and stellar surface density profiles and the observed relationship between the ages and metallicities of solar neighbourhood stars. I then use the models to make inferences about the properties of disk galaxies at high redshift. The total neutral hydrogen density Omega(HI) increases at higher z. The predicted increase is mild, but is roughly consistent with the latest derivation of Omega(HI) as a function of z by Storrie-Lombardi & MacMahon (1995). The models are also able to account for some of the other trends other trends seen in the high-redshift data, including the increase in the number of high column-density systems at high redshift, as well as the metallicity distribution of damped Lyman-alpha systems at redshifts 2-3.