\begin{table}%t1
\caption{\label{tab:kinematics}Ionised gas kinematics.}
%\centerline
 {\small \begin{tabular}{lccccc}
\hline\hline
Spectral line & \multicolumn{2}{c}{Narrow component} & \multicolumn{2}{c}{Broad component} &   $\Delta v$ \\
 & $v_{\rm center}$ & $v_{\rm width}$ & $v_{\rm center}$ & $v_{\rm width}$ & \\
\hline
\NII\     & $16505 \pm 15$ & $544 \pm 26$ & $16674 \pm 83$  & $1353 \pm 126$ & $169 \pm 84$  \\  
H$\alpha$ & $16500 \pm 18$ & $398 \pm 36$ & $16845 \pm 303$ & $1634 \pm 779$ & $345 \pm 304$ \\  
\SII\     & $16469 \pm 18$ & $513 \pm 43$ & $16725 \pm 88$  & $1384 \pm 253$ & $256 \pm 90$  \\  
\hline
\end{tabular}}
\medskip 
Notes -- All units are \kms\  and values have been corrected for instrumental resolution. $\Delta v$ is the difference between the central velocity of the narrow and the broad component. Results for \SII\ need to be taken with caution (because, due to the underlying stellar continuum, the intensity ratio of the broad component was constrained to be the same as that of the narrow component) and are merely included to show the reliability of our model for fitting \HaNII.
\end{table}