\begin{table}%t2
%\centering
\par
\caption{\label{T:blends}Contribution of possible blends to \ion{Fe}{15} at 284~{\AA}.}
\par
\begin{tabular}{lcccccc}
\hline\hline\noalign{\smallskip}
& Rest &  Relative  &\multicolumn{4}{c}{Modeled contribution  [\%]~\tablefootmark{a}}\\
\cline{4-7}
\multicolumn{2}{c}{wavelength}  & shift\tablefootmark{b}  & & active &  quiet  & coronal \\
line & $[$\AA$]$ & $[$km~s$^{-1}$$]$ & flare & region & Sun  & hole \\
\hline
\ion{Fe}{17} & 284.010\tablefootmark{c} & $-$158 & 2.8 &  0.1 & $<$0.1  &     0.0 \\
\ion{Al}{9} & 284.015\tablefootmark{d} & $-$152 &   0.2 & 0.6 & 2.1  &    83.7 \\
\ion{Fe}{15} & 284.160\tablefootmark{e} & 0 &  97.0 & 99.3 & 97.8  & 16.3 \\
\hline
\end{tabular}
\tablefoot{\tablefoottext{a}{Contribution modeled using the Chianti atomic data base.}
\tablefoottext{b}{Doppler shift according to difference in rest wavelength. }
\tablefoottext{c}{From NIST atomic spectra data base \citep{Ralchenko:2008}.}
\tablefoottext{d}{From NIST (as $^c$); based on laboratory measurements by \cite{Valero+Goorvitch:1972}, who estimate uncertainty to be  $\pm$0.04~{\AA} ($\pm$40~km~s$^{-1}$).} \tablefoottext{e}{Based on solar observations as provided by \cite{Brown+al:2008}, uncertainty is given as $\pm$0.004~{\AA} ($\pm$4~km~s$^{-1}$). Within errors consistent with NIST data base (observed and theoretical calculated values).}}
\end{table}