the complex distribution- and flow of $\ion{H}{i}$-gas [@Pontzen2008; @Rahmati2014]. In addition, the distribution of impact parameters correlates with absorption metallicity $([\mathrm{M}/\mathrm{H}]_\mathrm{abs})$, suggesting that DLAs probe the size of gaseous discs. This is supported by modelling DLAs as sight-lines through randomly inclined discs in high-$z$ Lyman break galaxies (LBG), which shows that the two are drawn from the same underlying distribution above $z>2$ [@Moller2004; @Fynbo2008; @Krogager2017].

Recent developments found a scaling relation that tie velocity-widths of metal lines in absorption to the absorber metallicity (the $\Delta V_{90}-[\mathrm{M/H}]_\mathrm{abs}$ relation). This relation is redshift-dependent [@Ledoux2006; @Moller2013; @Neeleman2013], column-density-dependent [@Som2015], and is interpreted as the absorber equivalent of the MZ-relation. Recognising that the relation can be used to target the most metal-rich absorbers has significantly increased the detection rate of absorbing galaxies in emission ($\sim 60-70~\%$), because these are associated with more massive and therefore more luminous galaxies [@Fynbo2010; @Fynbo2011; @Krogager2012; @Noterdaeme2012; @Peroux2012; @Bouche2013; @Fynbo2013; @Krogager2013; @Rahmani2016]. Connecting the $\Delta V_{90}$-\[M/H\] relation to the MZ-relation, [@Moller2013] predicted stellar masses in functional form $f(\tiny[\text{M/H}]_{\mathrm{abs}},~z_\mathrm{abs})$, including a free parameter $C_{[\text{M/H}]}$ to reconcile the difference between absorption- and emission-line metallicities. The relation was verified directly by comparing the stellar masses from the functional form to those derived 