\begin{table}%T3
\caption{\label{fwhm}
Heliocentric velocities and line widths ($FWHM$) (separated by $|$) in
km~s$^{-1}$ as well as mean $d$-parameter as
derived from $d$-Lorentz fits for the central row.}
\par
%\begin{center}
 {
\begin{tabular}{lccc}
\hline
\hline
line & \rm{ESO~103-G035} & \rm{TXS~2226-184} & \rm{\object{IC~1481}}\\
\hline
H$\beta$                      & 4011$|$479 & 7498$|$446 & 6138$|$445\\
{}[\ion{O}{iii}]~$\lambda$5007 & 4045$|$539 & 7553$|$397 & 6123$|$405\\
{}[\ion{O}{i}]~$\lambda$6300   & 4063$|$584 & 7564$|$676 & 6087$|$405\\
H$\alpha$                     & 4046$|$504 & 7486$|$327 & 6098$|$392\\
{}[\ion{N}{ii}]~$\lambda$6583  & 4046$|$443 & 7486$|$526 & 6097$|$416\\
{}[\ion{S}{ii}]~$\lambda$6731  & 4059$|$411 & 7515$|$389 & 6107$|$363$^a$\\
\hline
mean    & $4045\pm8 | 493\pm26$ & $7517\pm14 | 460\pm51$ &
$6108\pm7 | 404\pm11$\\
mean $d$ & $1.6\pm0.2$ & $1.1\pm0.1$ & $1.4\pm0.3$\\
\hline
\end{tabular}
}
$^a$ [\ion{S}{ii}]~$\lambda$6731 was truncated by telluric absorption
  bands and thus, [\ion{S}{ii}]~$\lambda$6716
  was used instead.
  %\end{center}
\end{table}