\begin{table}%t1
\caption{\label{TabFIR}Far-infrared line flux ratios to the dereddened 5007~\AA\ line as derived from different theoretical models and observations.
(See text for details).}
%\centerline
 {\small  \begin{tabular}{llllllll}
\hline\hline
  & $\lambda$,~$\mu$m & \multicolumn{5}{c}{$I/I(5007)$} &
 $f_{\rm PIR}$ \\
& & I-H  & BS-F  & BS-DC & SD-200$^*$ & Observed$^{**}$ & SD-200$^*$\\
\hline
{}[\ion{O}{iv}] & 25.91 &
  0.0051& 5.0   & 0.53  &  8.1  & 0.20   & 0.995 \\
{}[\ion{O}{iii}]& 51.81 &
  0.031 & 1.34  & 0.72  &  0.67 & 0.25   & 0.999 \\
{}[\ion{O}{i}]  & 63.19 &
  1.30  & 170   & 12    &  --  & 0.07   & --   \\
{}[\ion{O}{iii}]& 88.36 &
  0.028 & 0.22  & 0.11  &  0.55 & 0.10   & 0.999 \\
{}[\ion{O}{i}]  & 145.5 &
  0.038 & 7.8   & 0.75  & --   & $<$0.0024&--  \\
\hline
\end{tabular}}
\medskip
$^*$ Derived in Sects.~\ref{SecIRSD} and~\ref{SecLineI}; $^{**}$ obtained in Sects.~\ref{SecISO} and~\ref{SecSpitzerO}.\\
{Notes}: the last column lists contribution to the line flux in the SD-200 model arising from the photoionized region~(PIR) before the shock. Derivation of the observed line flux ratio values is
described in Sect.~\protect\ref{SecIRObs}. The model-predicted
[\ion{O}{i}] lines are sensitive to the pre-shock ion number density
in the model, see Sect.~\ref{SecOI}.
\end{table}