\begin{table}%t8
 %\centering
\par
\caption{\label{tab8}Spectra equivalent widths (\AA).}
 \begin{tabular}{cccc}
 \hline\hline \noalign{\smallskip}
Telescope& WHT & Keck I & Keck I\\
instrument& ISIS& LRIS&LRIS \\
 \hline
Date&2004-12-05&2004-12-12&2008-08-28\\  
 \hline 
H$\delta$ 4102&1.2$\pm$0.4&--&--\\
H$\gamma$ 4341&1.7$\pm$0.3&--&--\\
He II 4686&2.9$\pm$0.2& 0.6&--\\
H$\beta$ 4861&2.4$\pm$0.3 & 5.4&--\\
H$\alpha$ 6563&6.5$\pm$0.4 & 9.6 & 29.2$\pm$1.7\\
He I 6678 & --&1.0&--\\
Reference&1&2&3\\ 
\hline
$R$ Mag&17.40&18.61&21.10\\
$L_{\rm X}$(erg s$^{-1})$&8.6 $\times$ 10$^{35}$&1.7 $\times$ 10$^{35}$&$<$2.6 $\times$ 10$^{32}$\\
\hline
 \end{tabular}
\tablefoot{1 = \cite{tor08a}, 2 = \cite{rey} 3 = this paper. $R$-band magnitudes and \mbox{X-ray} luminosities are taken within one day of the optical spectra \citep[][this paper]{tor08a}. \mbox{X-ray} luminosities are from RXTE/PCA are based on a distance of 2.8~kpc as adopted in Sect.~10.3 of \cite{tor08a}.}\vspace*{2.5mm}
\end{table}