On the HI content, dust-to-gas ratio and nature of MgII absorbers

TL;DR

This study investigates the dust-to-gas ratio in MgII absorbers across redshifts 0.5 to 1.4, revealing its independence from equivalent width and suggesting galactic outflows from L* galaxies as their primary origin.

Contribution

It provides the first detailed analysis of the dust-to-gas ratio's dependence on equivalent width and redshift in MgII absorbers, linking these properties to galaxy evolution and outflows.

Findings

Dust-to-gas ratio is independent of equivalent width.

Redshift evolution of dust-to-gas ratio matches that of L* galaxies.

Strong MgII systems follow the Bohlin relation at lower column densities.

Abstract

We estimate the mean dust-to-gas ratio of MgII absorbers as a function of rest equivalent width W_0 and redshift over the range 0.5<z<1.4. Using the expanded SDSS/HST sample of low-redshift Lyman-alpha absorbers we first show the existence of a 8-sigma correlation between the mean hydrogen column density <N_HI> and W_0, an indicator of gas velocity dispersion. By combining these results with recent dust-reddening measurements we show that the mean dust-to-gas ratio of MgII absorbers does not appreciably depend on rest equivalent width. Assuming that, on average, dust-to-gas ratio is proportional to metallicity, we find its redshift evolution to be consistent with that of L^star galaxies from z=0.5 to 1.4 and we show that our constraints disfavor dwarf galaxies as the origin of such absorbers. We discuss other scenarii and favor galactic outflows from ~L^star galaxies as the origin of the majority of strong MgII absorbers. Finally, we show that, once evolutionary effects are taken into account, the Bohlin et al. relation between A_V and N_H is also satisfied by strong MgII systems down to lower column densities than those probed in our Galaxy.