\begin{table}%ta1
\caption{\label{tabriga}Optical emission line fluxes of the core galaxies.}
\par
%\centerline
{
\begin{tabular}{c | c c c c c c c}
\hline\hline
Name     & V    & H$\beta$  & [O~III] & [O~I] & H$\alpha$ & [N II] & [S~II] \\
\hline
UGC~5902 & 950  &3.2 $\pm$ 0.5  & 4.8 $\pm$ 0.4 & $<$1.2      & 6.2 $\pm$ 0.7   & 3.8 $\pm$ 0.4 & $-$ \\
UGC~7203 & 2379 &0.9 $\pm$ 0.1  & 1.0 $\pm$ 0.1 & 0.5 $\pm$ 0.1 & 2.8 $\pm$ 0.1   & 4.4 $\pm$ 0.2 & $-$ \\
UGC~7629 & 1047 &0.9 $\pm$ 0.2  & 1.1 $\pm$ 0.2 & $<$0.6     & 1.6 $\pm$ 0.2   & 3.3 $\pm$ 0.2 & $-$\\
UGC~7760 & 450  &2.0 $\pm$ 0.5  & 4.4 $\pm$ 0.7 & $<$1.2      & 10 $\pm$ 1      & 20.0 $\pm$ 0.4& $-$ \\ 
UGC~7898 & 1198 &0.8 $\pm$ 0.2  & $<$0.7     & $<$0.8     & 0.6 $\pm$ 0.2   & $<$1.2      & $-$ \\    
UGC~8745 & 2054 &3.0 $\pm$ 0.3  & 2.8 $\pm$ 0.3 & $<$1.1      & 6.4 $\pm$ 0.3   &12.0 $\pm$ 0.3 & $-$ \\
UGC~9655 & 2037 &1.1 $\pm$ 0.3  & $<$1.2      & $<$0.91     &1.6 $\pm$ 0.3    & 3.3 $\pm$ 0.3 & $-$ \\ 
\hline	       									
UGC~0968  & 2422 & 0.94$^{b}$&  $<$0.45 & $<$0.42  &  3.0 & 4.7   &  2.1  \\     
UGC~6297 & 1025 & 3.2       &   7.3    &   3.4    &  18  & 38    &  15 \\
UGC~7386 & 788  & 51        &  67      & 54       &   132&  161  &  195  \\
UGC~7797 & 2283 & 2.4       &    5.6   &  4.6     &   11 & 16    &  19   \\
UGC~7878 & 1012 & 1.9       &   3.6    &  1.2     &  5.4 &  9.9  &  7.8  \\       
UGC~9706 & 1832 & 1.7       &   2.1    & 0.6$^{c}$&  6.6 & 10    &  6.3 \\     
UGC~9723 & 950  & 0.54      &  1.1     &  $<$0.47 &  3.6 &  4.9  &  2.7 \\
\hline
\end{tabular}}
\par
\medskip 
Column desctription: (1) name; (2) radial
  velocity (cz) corrected for Local Group infall onto Virgo cluster [km
  s$^{-1}$]; emission line flux in units of 10$^{-15}$ erg s$^{-1}$ cm$^{-2}$:
  (3) H$\beta\lambda$4861, (4) [O~III]$\lambda$5007, (5) [O~I]$\lambda$6300,
  (6) H$\alpha\lambda$6563, (7) [N~II]$\lambda$6584, (8) sum of
  [S~II]$\lambda$6716 and [S~II]$\lambda$6731. The upper limit fluxes are
  measured at 3$\sigma$.  The data below the horizontal line are from
  \citet{ho97}. For these sources, values with uncertainties of $\pm$30\%--50\%
  are marked by `b', while highly uncertain values with probable errors of
  $\pm$100\% are marked by `c'.
\end{table}