\begin{table}%t4 
% %\centering
\par
\caption{Stellar parameters and Fe abundances
for stars in NGC~6253. Numbers in parenthesis in Col.~6 are
[Fe/H] estimated by spectral synthesis.}\label{tab_Fe}
 %\centerline
{\begin{tabular}{lllllllll}
\hline
\hline
Star & \teff$_{\rm{phot}}$ & $\log g_{\rm{phot}}$ & \teff$_{\rm{spec}}$ & $\xi$ & [Fe/H] &$\sigma_{1}$ & $\sigma_{\rm{tot}}$ & Membership \\
 & (K) & & (K) & (km s$^{-1}$) & & &\\
\hline
069885 & 6032 & 3.84 & 6200 & 1.27 & +0.45(+0.35) &0.09 & 0.11& M\\
023501 & 5842 & 3.75 & 6050 & 0.90 & +0.29 &0.09 & 0.11& M?\\
023498 & 5509 & 3.44 & 5630 & 1.30 & +0.32 &0.09 & 0.11& M\\
024707 & 4972 & 3.05 & 4940 & 1.16 & +0.39 &0.09 & 0.11& M\\
105495* & 4520 & 2.46 & 4450 & 1.23 & +0.49(+0.35) &0.10 & 0.13& M\\
Average Fe& & & & &+0.39(+0.34)&& 0.08(0.04) (rms)& \\
\hline
Likely non-members \\
069360 & 4741 & 2.81 & 4680 & 1.20 & +0.48 &0.10 & 0.12& NM\\
022182 & 4865 & 3.13 & 4770 & 1.20 & +0.12 &0.07 & 0.09& NM\\
\hline
\end{tabular}}\medskip
\par
* Note:  the initial parameters of the clump star have been computed from EIS magnitudes
calibrated to Bragaglia et~al.~(1997, see Table 2). 
We also performed a test using the Str\"omgren photometry
by Twarog et~al.~(2003) reported to the $UBV$ system. 
In this case we found \teff$_{\rm{phot}}$~=~4666~K and
$\log g=2.58$, and, from the spectroscopic analysis, \teff$_{\rm{spec}}=4500$~K, $\xi=1.23$~km~s$^{-1}$, 
[Fe/H$]=+0.51$ ($\log g=2.58$), which agree within the errors with the values reported in Table \ref{tab_Fe}.
\end{table}