\noalign{\smallskip}
\hbox{v',v''} & \hbox{$\lambda$({\rm \AA})} & \hbox{Branch}&& 
  \hbox{J}    &   \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
\noalign{\hrule\vskip 0.1cm}
\hbox{(4,0)} & 6362.743 &R1 & 46  & \\
\hbox{(4,0} & 6362.450  &Q1 & 39  & \\
\hbox{(10,5)} & 6362.765  &P2 & 21 &  \\
\hbox{(10,5)} & 6362.548  &P2 & 10 &  \\
\noalign{\vskip 0.1cm}
\hline
\noalign{\smallskip}
\end{array}$$

For the fit of the 4810 [Å]{} line, we adopted a procedure of balancing the continua points at the pseudo-continuum regions 4808.25, 4811.55, and 4812.6, with more weight for the 4811.55 [Å]{} that appears to be a better defined continuum. For the 6362.34 [Å]{} line, with a few exceptions, the local continuum is affected by the depression due to the line and, despite its being considered in the calculations, some extra depression remains. We gave priority to the continuum in the region 6361.5-6362.1 [Å]{} on the blue side of the Zn line. Examples of fitting ZnI lines in sample spectra are given in Figs. \[b6f1zn\], \[b6f8zn\], \[bwf8zn\], and \[bwc4zn\] for stars B6-f1, B6-f8, BW-f8, and BWc-4. In these figures we also show the calculations with no Zn (synthetic spectra in blue), showing that the 4810 [Å]{} line is free of blends, and the 6362 [Å]{} line shows a 