& \hbox{} & \multispan4  Sun && \multispan2 
  \hbox{\rm Arcturus}  
&  &  \hbox{\rm $\mu$ Leo} &  \\
  \cline{3-6}  \cline{8-9} \cline{11-11}  \\
&  & (1) & (2)  & (3) & (4) & & (5)  & (6)& & (7) &  \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
\noalign{\hrule\vskip 0.1cm}
\hbox{Fe} & 26  &~7.67 &  ~7.50  & ~7.50  & ~7.46 & &6.98 
&6.95 & & 7.80 &  \\
%\hbox{Fe} & 26  &~7.67 &  ~7.50  & ~7.50  & ~7.46 & &6.98(-0.52) 
%&6.95 (-0.54) & 7.80 &  \\
%\hbox{Cu} & 29  &~4.21 &  ~4.21  & ~4.19 & ~4.27 &  & &-- & ... & \\
\hbox{Zn} & 30  &~4.60 &  ~4.60  & ~4.56 & ~4.65 & & 4.26 & 4.06 & & 4.80 &  \\
\noalign{\vskip 0.1cm}
\hline
\noalign{\smallskip}
\end{array}$$

Abundance analysis
==================

Elemental abundances were obtained through line-by-line spectrum synthesis calculations, carried out using the code described in Barbuy et al. (2003) and Coelho et al. (2005). The molecular lines present in the region, namely the CN B$^2$$\Sigma$-X$^2$$\Sigma$ blue system, CN A$^2$$\Pi$-X$^2$$\Sigma$ red system, C$_2$ Swan A$^3$$\Pi$-X$^3$$\Pi$, MgH A$^3$$\Pi$-X$^3$$\Sigma^{+}$, and TiO A$^3$$\Phi$-X$^3$$\Delta$ $\gamma$ and B$^3$$\Pi$-X$^3$$\Delta$ $\gamma$’ systems were taken into account. The atmospheric models were obtained by interpolation in the grid of MARCS LTE models (Gustafsson et al. 