\begin{table}%t3 %\centering \par \caption{\label{tab3}Summary of the properties of the spectroscopic datasets employed in this study.} \begin{tabular}{lccccccl} \hline \hline\noalign{\smallskip} Date & MJD & Telescope & Instrument & Setting & $\lambda$ & Resln. & Reference\\ & & & & & ($\AA$) & & \\ \hline 23--25/06/01 & 52~083-5 & ESO 1.52m &Boller \& Chivens & Grat. \#1 & 6000--11~000 & 500 & C05 \\ & & & & & & \\ 07/06/02 +& 52~432 & NTT & EMMI & Grat. \#7 & 6310-7835 & 2600 & C05 \\ 06--08/06/03 & 52796--8 & & & Grat.\#6 & 8225-8900 & 5000 & Negueruela \& Clark (\cite{nc}) \\ & & & & & & & \\ 12--13/06/04 & 53168-69 & VLT & FORS longslit & G1028z & 7730--9480 & $\sim$7000 & Negueruela et~al. (\cite{n09})\\ & & & & G1200R & 5750--7310 & $\sim$7000 & \\ & & &FORS MXU & G1200R & 7730--9480\tablefootmark{a} & 2560 & \\ & & &FORS MXU & G1028z & 5750--7310\tablefootmark{a} & 2140 & \\ & & & & & & & \\ 25/03/05 + &53~454 & VLT &FLAMES+ & LR6 & 6438--7184 & 8600 & Ritchie et~al. (\cite{benLBV})\\ 29/05/05 +& 53519 & & MEDUSA & LR8 & 8206--9400 & 6500 & \\ 13/07/05& 53~564& & & & & & \\ & & & & & & \\ 29--30/06/05& 53~550-1 & NTT & SOFI & IJ Grism & 9500--13~500 & 1000 & Crowther et~al. (\cite{crowther}) \\ & & & & HK Grism & 15~000--22~700 & 1000 & \\ & & & & & & \\ 17/02/06 & 53~783 &NTT & EMMI & Grat. \#6 & 5740--8730 & 1500 & Marco \& Negueruela (\cite{marco}) \\ & & & & & & & \\ 11-12/03/06& 53805-6 & VLT & ISAAC &SWS(MR) & 22~490--23~730 & 9000 & Mengel \& \\ & & & & & & & Tacconi-Garman (\cite{mengel}) \\ & & & & & & & \\ 20+29/06/08 + & 54367+76& VLT &FLAMES+ & HR21 & 8484--9001 & 16200 & Ritchie et~al. (\cite{benbin})\\ 18+24/07/08 + & 54665+71 & & MEDUSA & & & & \\ 14+17/08/08 + & 54692+95 & & & & & & \\ 04+15/09/08 + & 54713+24 & & & & & \\ 19+25/09/08 + & 54728+34 & & & & & \\ 14+18/05/09 + & 54965+69 & & & & & \\ 20/08/09 & 55063 & & & & & \\ \hline \end{tabular} \tablefoot{\tablefootmark{a}{Note that the nominal wavelength range is given for the 2004 FORS MXU observations; in practice this can be displaced by a few hundred~$\AA$ depending on the position of an individual star on the CCD.}} \end{table}