\begin{table}%t2
\caption{\label{line_tab}For each nova, the year, magnitude, and amplitude of the outburst, the
slope $F = \lambda ^{\alpha}$ of the continuum, 
and the {\it FWHM}, equivalent widths, and line fluxes of the main emission lines
in the observed spectra are given. 
No de-reddening has been applied.
Note that the uncertainty of the line flux describes the
uncertainty of the relative flux in the line and does not include the
photometric error. Outburst magnitudes and amplitudes are taken/calculated from
the references as given in the text.
}
%\centerline
{\begin{tabular}{l c c c c l c c c }
\hline
\hline
 \noalign{\smallskip}
Nova & Date & $m_{\rm max}$ & $\Delta m$ &$\alpha$ & Transition & {\it FWHM} [nm] & $-W$ [nm] & $F$ [$10^{-18}$~W~m$^{-2}$] \\
 \noalign{\smallskip}
\hline
 \noalign{\smallskip}
V630~Sgr & 1936 & ${\rm vis}=4.0^{\rm m}$ & 13.9$^{\rm m}$ &$-1.21 \pm 0.02^{1}$ & H$\alpha$ & $2.36\pm 0.04$ & $2.70 \pm 0.06$ & $4.09\pm 0.09$ \\
         & & & & $-2.55 \pm 0.02^{1}$ & H$\beta $ & $1.90\pm 0.04$ & $1.35 \pm 0.07$ & $3.32\pm 0.15$ \\
         & & & & & H$\gamma$ & $1.59\pm 0.04$ & $0.73 \pm 0.04$ & $2.15\pm 0.07$ \\
         & & & & & He~II~$\lambda$541 & $2.00\pm 0.09$ & $0.51\pm 0.03$ & $1.15\pm 0.06$ \\
         & & & & & He~II~$\lambda$469 & $1.93\pm 0.06$ & $2.8\pm 0.2$ & $7.0\pm 0.2$ \\
 \noalign{\smallskip}
\hline
 \noalign{\smallskip}
XX~Tau & 1927 & $p=5.9^{\rm m}$ & $>13.1^{\rm m}$ & $-2.66\pm 0.03$ & H$\alpha$ &   $3.36 \pm 0.03$ & $5.2\pm 0.1$ & $1.56\pm 0.05$ \\
        & & & & & H$\beta $ &   $2.30 \pm 0.04$ & $1.92\pm 0.06$ & $1.29\pm 0.05$ \\
        & & & & & H$\gamma$ &   $2.21 \pm 0.05$ & $1.36\pm 0.03$ & $1.17\pm 0.01$ \\
        & & & & & H$\delta$ &   $2.56 \pm 0.04$ & $1.38\pm 0.1$  & $1.3\pm 0.1$   \\
        & & & & & H$\epsilon$ & $2.29 \pm 0.04$ & $1.11\pm 0.05$ & $1.12\pm 0.04$ \\
        & & & & & H$_8$ &       $2.05 \pm 0.07$ & $0.85\pm 0.05$ & $0.88\pm 0.04$ \\
        & & & & & H$_9$ &       $1.91 \pm 0.12$ & $0.53\pm 0.05$ & $0.58\pm 0.04$ \\
        & & & & & He~I~$\lambda$668 & $1.9 \pm 1.5$ & $0.39\pm 0.1$ & $0.11\pm 0.04$ \\
        & & & & & He~I~$\lambda$588 & $2.8 \pm 0.2$ & $0.50\pm 0.1$ & $0.22\pm 0.04$ \\
        & & & & & He~I~$\lambda$447 & $2.3 \pm 0.2$ & $0.35\pm 0.1$ & $0.31\pm 0.06$ \\
 \noalign{\smallskip}
\hline
 \noalign{\smallskip}
V529~Ori & 1678 & ${\rm vis}=7^{\rm m}$ & & $+4.87\pm 0.07^{2}$ &  H$\alpha$ & $1.43\pm 0.05$ & $2.95\pm 0.06$ & $3.75\pm 0.07$  \\
 \noalign{\smallskip}
\hline
 \noalign{\smallskip}
CQ~Vel & 1940 & $p=9.0^{\rm m}$ & $>12.1^{\rm m}$ & $-1.15 \pm 0.03$ & H$\alpha$ & $2.88 \pm 0.04$ & $1.80\pm0.05$ & $0.52\pm 0.01$  \\
        & & & & & H$\beta $ & $2.1\pm 0.1$    & $0.45\pm0.05$ & $0.18\pm 0.01$  \\
 \noalign{\smallskip}
\hline
 \noalign{\smallskip}
V842~Cen & 1986 & ${\rm vis}=4.6^{\rm m}$ & $>13.4^{\rm m}$ & $-4.32\pm 0.05 ^{3}$ & H$\alpha$ & $5.08\pm 0.03$ & $7.31\pm 0.04$ & $0.0719\pm 0.0004$ \\
          & & & & $-1.59\pm 0.02 ^{3}$ & H$\beta $ & $1.79\pm 0.02$ & $1.56\pm 0.03$ & $0.0248\pm 0.0003$ \\
          & & & & & H$\gamma$ & $1.5 \pm 0.05$ & $0.86\pm 0.02$ & $0.0208\pm 0.0003$ \\
          & & & & & H$\delta$ & $1.9 \pm 0.1$  & $0.8\pm 0.2$   & $0.027\pm 0.03$\\
          & & & & & H$\epsilon$&$1.42\pm 0.02$ & $0.67\pm 0.03$ & $0.0264\pm 0.0003$ \\
          & & & & & H$_8$     & $1.41\pm 0.03$ & $0.38\pm 0.05$ & $0.016\pm 0.001$  \\
          & & & & & He~I~$\lambda$706? & $1.95\pm 0.05$& $0.12\pm 0.02$ & $0.00105\pm 0.0003$ \\
          & & & & & He~I~$\lambda$668 & $1.86\pm 0.02$& $0.33\pm 0.02$ & $0.00314$\\
          & & & & & He~I~$\lambda$588 & $1.72\pm 0.02$& $>$$0.38$ & $>$$0.0044$\\
          & & & & & He~I~$\lambda$447 & $1.35\pm 0.2$ & $0.22\pm 0.02$ & $0.0045 \pm 0.0004$\\
          & & & & & C~IV $\lambda$580 & $2.3\pm 0.2$& $0.30\pm 0.02$ & $0.0035 \pm 0.0004$\\
 \noalign{\smallskip}
\hline
\end{tabular}}
\par
\smallskip
$^1$ The continuum of V630~Sgr shows two slopes; the first for  
$\lambda < 582$~nm, the second for $\lambda \ge 582$~nm.\\
$^2$ V529~Ori shows no straight line in the double-logarithmic plot;
thus only a formal value for a linear fit to the data is given.\\
$^3$ The continuum of V842~Cen shows two slopes; the first for  
$\lambda < 500$~nm, the second for $\lambda \ge 500$~nm.
\end{table}