\begin{table}%t1
%\centering
\par
\caption{\label{table_para37183729}Global parameters of \object{NGC~3718} and
\object{NGC~3729}.}
\begin{tabular}{l|ll|l}
\hline
\hline
 & \object{NGC~3718} & \object{NGC~3729} & references\\
\hline
RA (J2000.0)  & $11^{{\rm h}}32^{\rm {m}}35{\fs}3$ &
 $11^{\rm {h}}33^{\rm {m}}49{\fs}4$ & NED$^a$\\
Dec (J2000.0) & $+53\degr 04'01''$ & $+53\degr 07'32''$ & NED$^a$\\
Host type$^b$ & Sa & SBab & Verheijen \&
  Sancisi (\cite{Verheijen})\\
Nucleus type$^c$ & L 1.9 & H & Ho et~al. (\cite{Ho})\\
$B$-magnitude app./abs. (mag) & 11.59/$-$19.01 & 12.03/$-$18.57 & NED$^a$\\
$R_{80}^B~^d$ & 220$''$ & 60$''$ & Tully et~al. (\cite{Tully})\\
Radio flux density S~[mJy] at 10.7GHz & 8.5$^e$ & 6$^f$ & $^e$ Nagar et~al. (\cite{Nagar}), $^f$ Niklas et~al. (\cite{Niklas})\\
Radio flux density S~[mJy] at 1.49GHz$^g$ & 18.3 & 20.5 & Condon (1987)\\
Radio flux density S~[mJy] at 1.4GHz$^h$ & $<$50 & $<$50 & Hummel (1980)\\
Atomic gas mass $M_{\rm H}$  & $6\times10^9$~$M_{\odot}$ & $0.15\times10^9$~$M_{\odot}$ & Schwarz (\cite{Schwarz})
 \\
Total mass & $400\times10^9$~$M_{\odot}$  & $40\times10^9$~$M_{\odot}$ & Schwarz (\cite{Schwarz})\\
Position angle of major axis$^i$ & 15\degr & $-$16\degr & Verheijen \& Sancisi (\cite{Verheijen})\\
Inclination$^i$ & 68\degr & 48\degr & Verheijen \& Sancisi (\cite{Verheijen})\\
Heliocentric velocity$^i$ & $993 \pm 1$~km~s$^{-1}$ & $1060 \pm 1$~km~s$^{-1}$ & Verheijen \& Sancisi (\cite{Verheijen})\\
\hline
\multicolumn{4}{l}{$^a$ NED: NASA/IPAC Extragalactic Database.} \\
\multicolumn{4}{l}{$^b$ Morphological classification. S: Spiral; SB: Barred Spiral.}\\
\multicolumn{4}{l}{$^c$ Spectroscopic classification. L1.9: LINER; H: HII
 nucleus.}\\ 
\multicolumn{4}{l}{$^d$ Radius containing 80\% of the radiation in the $B$-band.
  }\\
\multicolumn{4}{l}{$^e$ Calculated with a spectral index of $\alpha=1.05$
 based on flux densities at $8.4~\rm GHz$ and $15~\rm GHz$.}\\ 
\multicolumn{4}{l}{$^g$ Integrated VLA continuum flux density.}\\ 
\multicolumn{4}{l}{$^h$ Total WSRT continuum flux density.}\\ 
\multicolumn{4}{l}{$^i$ From HI with PA pointing to the approaching major semi-axis.}
\end{tabular}
\end{table}