\begin{table}%t4
%
\par
\caption{\label{table.comp}Comparison with other temperature scales.}  
%\centerline
{
\small\begin{tabular}{lcrrr}
\hline
\hline
Sample	& [Fe/H] range & $\Delta T_{\rm eff}$ & $\sigma_{T_{\rm eff}}$ & $N^{a}$ 
\\       
\hline
\multicolumn{5}{c}{Dwarf Stars} \\
\citet{aam96a} & [--3.5,~+0.3] & +64 & 104 & 332 \\
\citet{aam96a} & [--3.5,~--2.5] & +61 & 91  & 18  \\
\citet{aam96a} & [--0.5,~+0.3] & +32 & 130 & 122 \\
\citet{ram05a} & [--4.0,~+0.3] & +33 & 98 & 84 \\
\citet{ram05a} & [--4.0,~--2.5] & --87 & 194  & 12  \\
\citet{ram05a} & [--0.5,~+0.3] & +45 & 91 & 69 \\
\citet{cas06}  & [--1.9,~+0.4] & --12 & 56 & 101 \\
\citet{cas06}$^b$  & [--1.9,~+0.4] & --41 & 50 & 101 \\
\citet{san04}  & [--0.7,~+0.5] & +11 & 120 & 133 \\
\citet{san04}$^b$  & [--0.7,~+0.5] & --13 & 129 & 133 \\
\citet{bon07}  & [--3.6,~--2.4] & +165 & 79 & 16 \\
\citet{bar02}  & [--2.5,~+0.1] & +77 & 133 & 23 \\
\citet{bar02}  & [--0.5,~--0.1] & +51 & 129 & 16 \\
\citet{chr04}  & [--3.1,~--1.6] & +177 & 80 & 8 \\
\citet{bai08}$^c$  & [--0.4,~0.5] & --32 & 163 & 22 \\
\hline
\multicolumn{5}{c}{Giant stars} \\
\citet{aam99a} & [--3.0,~+0.5] & +54 & 131 & 202 \\
\citet{aam99a} & [--3.0,~-2.5] & +76 & 120 & 10 \\
\citet{aam99a} & [--0.5,~+0.5] & +43 & 144 & 116 \\
\citet{ram05a} & [--4.0,~+0.3] & +63 & 57 & 25 \\
\citet{ram05a} & [--4.0,~--2.5] & +61 & 62 & 18  \\
\citet{ram05a} & +0.2$^d$ & +116 & -- & 1  \\
\citet{cay04}  & [--4.0,~--2.0] & +115 & 76 & 34 \\
\citet{chr04}  & [--3.4,~--2.6] & +128 & 71 & 22 \\
\citet{bai08}$^c$  & 0$^e$ & --67 & 139 & 6 \\
\hline     
\end{tabular}}
\medskip
$^{a}$ The number of stars.\\
$^{b}$ If we consider all reddening corrections equal to zero.\\
$^{c}$ $\Delta T_{\rm eff}=T_{\rm
eff}^{\rm IRFM}-T_{\rm eff}^{\rm dir}$, where $T_{\rm eff}^{\rm dir}$
is a direct determination of \teff using the angular diameter
$\theta$. \\
$^{d}$ One metal-rich giant star.\\
$^{e}$ Did not find any metallicity determination so decided to
adopt [Fe/H]~$=0$. 
\end{table}