\begin{table}%t1
      \caption {\label{tab:ml}{Mass-to-light ratio in $V$}, 
	using the colour transformation\protect $V=r+0.27$
	\citep{smi02}.}
              $$ 
         \begin{array}{p{0.19\linewidth}ccc}
            \hline\hline
            \noalign{\smallskip}
            Case      & M/L_V & M/L_V & M/L_V^{{a}} \\
                      & { (\sigma_{R}=45~{\rm
                          km~s^{-1}})} & { (\sigma_{\rm
                          R}=71~{\rm km~s^{-1}})} & { (\sigma_{\rm R,Alt}=10~{\rm km~s^{-1}})} \\
            \noalign{\smallskip}
            \hline
            \noalign{\smallskip}
          % r-band:  table_r_5.txt
          %cat table_r_5.txt | awk '{printf"%5.2f  %5.2f  %5.2f\n",$1*10**(0.4*0.265),$2*10**(0.4*0.265),$3*10**(0.4*0.265)}'
            $Q=1$   & 11.2 &   25.0 & 0.9 \\ %1.0 (thin)
            $Q=1.5$ &  7.4 &   16.7 & 0.6 \\ %0.7 (thin)
            $Q=2$   &  5.6 &   12.5 & 0.4 \\ %0.5 (thin)
            $\lambda=\lambda_{\rm max}$   &   2.9 &   6.2 & 0.8 \\ % 0.8 (thin)
            \noalign{\smallskip}
	    \hline
            \noalign{\smallskip}
            Stellar & \multicolumn{3}{c}{1.4^{+1.4}_{-0.8}} \\
            \noalign{\smallskip}
            \hline
         \end{array}
     $$ 
     $^{{a}}$ The
        alternative scenario, in which only part of the observed
        velocity dispersion is attributed to the disk (see Sect.~\ref{sec:discuss}).
   \end{table}