adopted. Other such relations are given by Cen & Ostriker (1999) and Madau & Pozzetti (2000), for example. This figure shows that a comparison of Zn in DLAs and in bulge stars benefit from an overlap only at metallicities $-$1.5 $<$ \[Fe/H\] $<$ $-$0.1, with most sample bulge stars being more metal-rich than this.

### Selected DLAs with Fe abundance measurements

$$\begin{array}{lccr@{}r@{}r@{}r@{}r@{}}
\hline\hline
\noalign{\smallskip}
\hbox{QSO} & \hbox{z$_{\rm abs}$} & \hbox{[Zn/H]}
& \hbox{[Fe/H]} & \phantom{-}\hbox{[Fe/H]$_{\rm c}$} & 
\phantom{-}\hbox{[Zn/Fe]} 
& \phantom{-}\hbox{[Zn/Fe]$_{\rm c}$}    &   \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
\noalign{\hrule\vskip 0.1cm}
\noalign{\smallskip}
\noalign{Akerman et al. 2005}
\noalign{\smallskip}    
\noalign{\hrule\vskip 0.1cm}
\noalign{\smallskip}
\hbox{B0438-436} & 2.34736 & $-$0.68 & $-$1.30& $-$0.87& 0.62 &  0.24&\\        
\hbox{B0458-020} & 2.03950 & $-$1.15 & $-$1.61& $-$1.34& 0.46 &  0.21&\\        
\hbox{B0528-250} & 2.14100 & $-$1.45 & $-$1.57& $-$1.34& 0.12 & $-$0.09&\\      
\hbox{B0528-250} & 2.81100 & $-$0.47 & $-$1.11& $-$0.57& 0.64 &  0.18&\\        
\hbox{B1055-301} & 1.90350 & $-$1.26 & $-$1.57& $-$1.32& 0.31 &  0.08&\\        
\hbox{B1230-101} & 1.93136 & $-$0.17 & $-$0.63&  0.10& 0.46 & $-$0.15&\\        
\hbox{B2314-409} & 1.85730 & $-$1.01 & $-$1.29& $-$1.01& 0.28 &  0.02&\\        
\noalign{\smallskip}
\noalign{\hrule\vskip 0.1cm}
\noalign{\smallskip}
\noalign{Vladilo et al. 2011}
\noalign{\smallskip}
\noalign{\hrule\vskip 0.1cm}
\noalign{\smallskip}
\hbox{0216+080}  & 2.2930 & $-$0.63 &$-$1.12&$-$0.67 &0.49 &0.10 &\\
\hbox{2206-199A} & 1.9200 & $-$0.33 &$-$0.87&$-$0.25 