using the modified models relative to the adopted model. We adopt a mean of the uncertainty on the 4810 and 6362 [Å]{} lines. These uncertainties are given in Table \[errors2\] for star B6-f1, for which the 6362 line is strongly affected by the CN blending, and BW-f8 with negligible CN blending. The higher sensitivity to effective temperature in B6-f1 is due to the CN lines blending the 6362.339 [Å]{} line: it is the CN lines that are more sensitive to temperature. Since the stellar parameters are covariant, the sum of these errors is an upper limit. On the other hand, a continuum location uncertainty introduces a further uncertainty in \[Zn/Fe\] of $\pm$0.1.

$$\begin{array}{lccccc}
\hline\hline
\noalign{\smallskip}
\hbox{Star} & \hbox{$\Delta$T$_{\rm eff}$} & \hbox{$\Delta$$\log$ g}
& \hbox{$\Delta$[Fe/H]} & \hbox{$\Delta$v$_{t}$} & \hbox{($\sum$x$^{2}$)$^{1/2}$} \\
& \hbox{(+150 K)} & \hbox{(+0.2)} & \hbox{(+0.1)} & \hbox{(+0.1 kms$^{-1}$})&\\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
\noalign{\vskip 0.1cm}
\noalign{\hrule\vskip 0.1cm}
\hbox{B6-f1}  &  $-$0.17  &   +0.05 & $-$0.06 & $-$0.01 & 0.19 \\
\hbox{BW-f8}  &     0.00  &   $-$0.05 & +0.10 & $-$0.02 & 0.11 \\
\noalign{\vskip 0.1cm}
\hline
\noalign{\smallskip}
\end{array}$$

Results
=======

The derived Zn abundances are given in Table \[cncorrected\]. In Fig. \[plotzn\], the \[Zn/Fe\] vs. \[Fe/H\] behaviour is shown for the present sample, 