\begin{table}%t2
\addtocounter{table}{+1}
%\centering
\par
\caption{Parameters of the sample galaxies.}
\label{tab:sample}
\begin{tabular}{cllccccccc}
\hline\hline
\noalign{\smallskip}
\multicolumn{1}{c}{Object} &
\multicolumn{2}{c}{Morp. type} &
\multicolumn{1}{c}{$B_T$} &
\multicolumn{1}{c}{PA} &
\multicolumn{1}{c}{$i$} &
\multicolumn{1}{c}{$V_{\odot}$} &
\multicolumn{1}{c}{$D$} &
\multicolumn{1}{c}{Scale} &
\multicolumn{1}{c}{$M_{B_T}^0$} \\
\noalign{\smallskip}
\multicolumn{1}{c}{[name]} &
\multicolumn{1}{c}{[RSA]} &
\multicolumn{1}{c}{[RC3]} &
\multicolumn{1}{c}{[mag]} &
\multicolumn{1}{c}{[$\dg$]} &
\multicolumn{1}{c}{[$\dg$]} &
\multicolumn{1}{c}{[\kms]} &
\multicolumn{1}{c}{[Mpc]} &
\multicolumn{1}{c}{[pc/$''$]} &
\multicolumn{1}{c}{[mag]} \\
\noalign{\smallskip}
\multicolumn{1}{c}{(1)} &
\multicolumn{1}{c}{(2)} &
\multicolumn{1}{c}{(3)} &
\multicolumn{1}{c}{(4)} &
\multicolumn{1}{c}{(5)} &
\multicolumn{1}{c}{(6)} &
\multicolumn{1}{c}{(7)} &
\multicolumn{1}{c}{(8)} &
\multicolumn{1}{c}{(9)} &
\multicolumn{1}{c}{(10)} \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}  
\object{NGC~0949}  & Sc(s)III & Sb(rs):?  & 12.40 & 145 & 58 &  608 $\pm$ 10 & 11.2 &  54.5 & $-18.47$  \\
\object{NGC~2460}  & Sab(s)   & Sa(s)     & 12.72 &  40 & 42 & 1452 $\pm$10 & 21.3 & 103.0 & $-19.35$  \\
\object{NGC~2541}  & Sc(s)III & Scd(s)    & 12.26 & 165 & 60 &  540 $\pm$10 &  8.3 &  40.5 & $-18.03$  \\
\object{NGC~6810}  & Sb       & Sab(s):sp & 12.37 & 176 & 78 & 1961 $\pm$5 & 24.3 & 117.8 & $-20.44$  \\
\hline
\end{tabular}
NOTES -- Column (2): morphological classification from RSA.
Column (3): morphological classification from RC3.
Column (4): apparent total blue magnitude from RC3.
Column (5): major-axis position angle from RC3.
Column (6): inclination derived as $\cos^{2}{i}~=~(q^2-q_0^2)/(1-q_0^2)$.
         The observed axial ratio $q$ is taken from RC3 and the
         intrinsic flattening has been assumed following
         Guthrie (1992) with RC3 morphological classification.
Column (7): heliocentric velocity of the galaxy derived as center of
         symmetry of the rotation curve of the gas with eliocentric correction.
Column (8): distance obtained as $V_0/H_0$ with $H_0=75$ \kmsmpc\
         and $V_0$ the systemic velocity derived
         from $V_\odot$ corrected for the motion of the Sun with
         respect of the Local Group as done in the RSA.
Column (10): absolute total blue magnitude corrected for
          inclination and extinction from RC3.
\end{table}