\begin{table}%t1
\caption{\label{tab:lines}Spectral lines present in the data sets, with parameters computed by CHIANTI and given by previous observations.}
\par
\small%\centerline
 {
\begin{tabular}{ll|lll|ll}
\hline \hline
&            & \multicolumn{3}{c|}{CHIANTI$^a$} & \multicolumn{2}{c}{\cite{cur01}} \\
ion & transition $j \rightarrow i$ & $\log T_{\rm max}$ (K) &
wavelength (\AA) & radiance$^b$ & wavelength (\AA) & peak radiance$^b$ \\ 
\hline
&&&&&& \\[-8pt]
\svi & $ 2{\rm p}^6\;3{\rm p}\;{}^2{\rm P}_{3/2}
\rightarrow 2{\rm p}^6\;3{\rm s}\;{}^2{\rm S}_{1/2}$ &
$5.3$ & $933.3800$ & $3.81\times10^{-3}$ & $933.40$ & $0.57$ \\
\lyeps & $ 6{\rm p}\;{}^2{\rm P}_{3/2} \rightarrow
1{\rm s}\;{}^2{\rm S}_{1/2}$ & --- & --- & --- & $937.80$ &
$1.07$ \\ 
\siviii & $ 2{\rm s}^2\;2{\rm p}^3\;{}^2{\rm P}_{3/2}
\rightarrow 2{\rm s}^2\;2{\rm p}^3\;{}^4{\rm S}_{3/2}$ &
$5.9$ &
$944.4670$ & $5.24\times10^{-3}$ & $944.34$ & $0.14$ \\ 
\svi & $ 2{\rm p}^6\;3{\rm p}\;{}^2{\rm P}_{1/2}
\rightarrow 2{\rm p}^6\;3{\rm s}\;{}^2{\rm S}_{1/2}$ &
$5.3$ & $944.5240$ & 
$1.91\times10^{-3}$ & $944.55$ & $0.29$ \\
\hline
\end{tabular}}
\medskip
$^a$ Using the ``Arnaud \& Raymond'' ionization fractions file, the ``Sun coronal'' abundance file and the ``quiet Sun'' DEM file. CHIANTI does not include data for the Hydrogen lines (\lyeps\ in particular).  \\
$^b$ Radiances  are given in ${\rm W~m^{-2}~sr^{-1}}$, and peak spectral radiances are given in ${\rm W~m^{-2}~sr^{-1}~nm^{-1}}$.
\end{table}