The Mass Density of MgII Absorbers from the Australian Dark Energy Survey

We present an all-southern sky survey for MgII doublet absorbers in 951 z = 0. 3 A. We studied 656 MgII absorption systems over the redshift range 0. 33 < z < 2. 19 with equivalent widths 0. 3 < Wᵣ (2796) < 3. 45 A. The equivalent width distribution is well fit by an exponential function with W* = 0. 76 +/- 0. 04 A and the redshift path density exhibits very little evolution. Overall, our findings are consistent with the large, predominantly northern-sky, surveys of MgII absorbers. We developed and implemented a Monte Carlo model informed by a high-resolution MgII survey for determining the MgII mass density, OmegaMgII. We found OmegaMgII ~ 5 x 10^-7 with no evidence of evolution over a ~7 Gyr time span following Cosmic Noon. Incorporating measurements covering 2. 0 < z < 6. 4 from the literature, we extended our insights into MgII mass density evolution from the end of reionization well past the Cosmic Noon epoch. The presented Monte Carlo model has potential for advancing our knowledge of the evolution of mass densities of metal-ions common to quasar absorption line studies, as it exploits the efficiency of large low-resolution surveys while requiring only small samples from expensive high-resolution surveys.