The outcome of the evolutionary history of galaxies is recorded in the interstellar abundances of chemical elements. Observations of the interstellar medium (ISM) in galaxies of various types, differing in terms of mass, size, metallicity, and their respective evolutionary stages, may provide a key to understanding the processes taking place in galaxies. The [α/Fe] ratio, and its evolution with the metallicity [M/H] is a strong diagnostic of the chemical evolution of galaxies.

We have constrained, for the first time, the distribution of the α-element enhancement with metallicity in the neutral ISM in distant galaxies at redshifts of 0.60 < z < 3.40. By dividing our sample of QSO-DLAs into two parts by velocity widths we have found that less massive (with lower velocity widths) galaxies show an α-element knee at lower metallicities than more massive (with higher velocity widths) galaxies.

We aim to investigate chemical properties of gas component in chemo-hydro- dynamical models of dwarf galaxies simulated by Revaz & Jablonka (2018) and compare them with the data derived from the observations. Furthermore, we aim to test velocity widths of absorption lines as a measure of a galaxy stellar mass as well as to test the influence of the supernovae feedback.