Chemical evolution and depletion pattern in Damped Lyman α systems

Dust depletion plays a key role in understanding the nature of Damped Lyman α systems(DLAs). In this paper we point out a previously unnoticed anticor-relation between the observed abundance ratio [X/Zn] (where Zn is assumed to be undepleted and X stands for the refractories Fe, Cr and Ni) and metal column density ([Zn/H]+log(N HI)) in DLAs. We suggest that this trend is an unambiguous sign of dust depletion, since metal column density is a measure of the amount of dust along the line of sight. Assuming that DLAs are (proto-)galactic disks and using detailed chemical evolution models with metallicity dependent yields we study chemical evolution and dust depletion patterns for α and iron−peak elements in DLAs. When observational constraints on the metal column density of DLAs are taken into account (as suggested in Boissé et al. 1998) we find that our models reproduce fairly well the observed mild redshift evolution of the abundances of 8 elements and Ni) as well as the observed scatter at a given redshift. By considering the aforementioned dependence of abundance ratios on metal column density, we further explore the general dust depletion pattern in DLAs, comparing to our model results and to a solar reference pattern. We find that for low metal column densities (no depletion), our models compare fairly well to the data, while a solar pattern has difficulties with Mn. At high metal column densities (amount of depletion ∼0.5 dex), the solar pattern describes the data quite well, while our models have difficulties with S. We suggest that further measurements of those key elements, i.e. Zn, S and Mn, will help to gain more insight into the nature of DLAs. In any case, the presently uncertain nucleosynthe-sis of Zn in massive stars (on which a large part of these conclusions is based) should be carefully scrutinised.