Meléndez et al. (2003). For the metal-rich star $\mu$ Leo, the stellar parameters and C, N, O abundances from Lecureur et al. (2007) were adopted: T$_{\rm eff}$ = 4540 K, log g = 2.3, \[Fe/H\] = +0.3, v$_{\rm t}$ = 1.3 km s$^{-1}$. The C, N, O abundances for $\mu$ Leo were revised from $\epsilon$(C) = 8.85, $\epsilon$(N) = 8.55, $\epsilon$(O) = 9.12, to \[C/Fe\]=$-$0.3, \[N/Fe\]=+0.6, \[O/Fe\]=$-$0.1 or $\epsilon$(C) = 8.55, $\epsilon$(N) = 8.83, $\epsilon$(O) = 8.97. Also for better fitting the line on the red side of the 4810.5 [Å]{} line, which is not well fitted with literature log gf values, we refitted them with the astrophysical log gf values reported in Table \[lines2\], assuming \[Cr/Fe\]=\[Ti/Fe\]=0.0 for $\mu$ Leo. Finally, for $\mu$ Leo, the resulting Zn abundance of \[Zn/Fe\]=$-$0.1 is derived from both ZnI lines.

$$\begin{array}{lcccccccccccc}
\hline\hline
\noalign{\smallskip}
%\hbox{El.} & \hbox{Z} & \multispan4  \hbox{log $\epsilon(X)_{\odot}$}&& \multis%pan2 
%  \hbox{log $\epsilon(X)_{\rm Arcturus}$}  
%&  &  \hbox{log $\epsilon$(X)$_{\rm \mu Leo}$} &  \\
%\hbox{El.} & \hbox{Z} & \multispan4  \hbox{log $\epsilon(X)_{\odot}$}&& \multis%pan2   \hbox{log $\epsilon(X)$}  &  &  \hbox{log $\epsilon$(X)} &  \\
\hbox{El.} & \hbox{Z} & \multispan6  \hbox{log $\epsilon(X)$} & & & & \\
  \cline{3-11}  \\
%& \multispan2   \hbox{log $\epsilon(X)$}  &  &  \hbox{log $\epsilon$(X)} &  \\
\hbox{} 