On the cosmic evolution of Fe/Mg in QSO absorption line systems

Abstract

We investigate the variation of the ratio of the equivalent widths of the Fe II λ2600 line to the MgII λλ2796, 2803 doublet as a function of redshift in a large sample of absorption lines drawn from the Johns Hopkins University - Sloan Digital Sky Survey Absorption Line Catalog. We find that despite large scatter, the observed ratio shows a trend where the equivalent width ratio R = WFe II/WMgII decreases monotonically with increasing redshift z over the range 0.55 ≤ z ≤ 1.90. Selecting the subset of absorbers where the signal-to-noise ratio of the MgII equivalent width WMgII is ≥ 3 and modelling the equivalent width ratio distribution as a Gaussian, we find that themean of theGaussian distribution varies as R α (-0.045 ± 0.005)z. We discuss various possible reasons for the trend. A monotonic trend in the Fe/Mg abundance ratio is predicted by a simple model where the abundances of Mg and Fe in the absorbing clouds are assumed to be the result of supernova (SN) ejecta and where the cosmic evolution in the SNIa and core-collapse SN rates is related to the cosmic star formation rate. If the trend in R reflects the evolution in the abundances, then it is consistent with the predictions of the simple model.