\begin{table}%t5
\caption{\label{TabAIR}Infrared line fluxes $I$ and their ratios $I/I$(5007~\AA)  to the dereddened optical [\ion{O}{iii}] 5007~\AA\ line from the \emph{Spitzer} data.}
%\centerline
 {\small \begin{tabular}{llllllllllll}
\hline\hline\noalign{\smallskip}
Line
    & \multicolumn{5}{c}{Line flux $I$, $10^{-13}$~erg/cm$^2$/s/pixel}
    & \multicolumn{5}{c }{Flux ratio $I/I$(5007~\AA)} \\
    & FMK 1 &FMK 2 &FMK 3 &FMK 4 &FMK 5
    & Average
    & FMK 1 &FMK 2 &FMK 3 &FMK 4 &FMK 5\\
\hline
{}[\ion{Ar}{ii}]  6.985~$\mu$m
    & 3.8  & 14   & 17   & 5.6  & 11
    & 0.5(1)
    &0.41  &0.75  &1.15  &0.46  &0.79 \\
{}[\ion{Ar}{iii}] 8.991~$\mu$m
    & 0.46 & 2.0  & 1.7  & 0.80 & 1.5
    & 0.08(3)
    &0.05  &0.13  &0.12  &0.07  &0.12 \\
{}[\ion{S}{iv}]   10.51~$\mu$m
    & 0.24 & 1.6  & 1.4  & 0.67 & 0.91
    & 0.07(2)
    &0.025 &0.11  &0.10  &0.06  &0.07 \\
{}[\ion{Ne}{ii}]  12.81~$\mu$m
    & 0.31 & 0.92 & 0.89 & 1.0  & 0.30
    & 0.10(8)
    &0.04  &0.07  &0.07  &0.08  &0.025\\
{}[\ion{Ne}{v}]   14.32~$\mu$m
    & 0.071& 0.20 & 0.18 & 0.10 & 0.14
    & 0.012(7)
    &0.009 &0.012 &0.012 &0.009 &0.014\\
{}[\ion{Ne}{iii}] 15.56~$\mu$m
    & 0.29 & 2.2  & 1.2  & 3.0  & 0.47
    & 0.05(3)
    &0.009 &0.03  &0.03  &0.05  &0.006\\
{}[\ion{Fe}{ii}]  17.94~$\mu$m
    & 0.16 & 0.90 & 1.3  & 1.8  & 0.87
    & 0.03(2)
    &0.005 &0.015 &0.03  &0.04  &0.013\\
{}[\ion{S}{iii}]  18.71~$\mu$m
    & 0.82 & 5.0  & 5.2  & 2.5  & 4.2
    & 0.08(2)
    &0.025 &0.08  &0.15  &0.05  &0.06 \\
{}[\ion{O}{iv}]   25.91~$\mu$m
    & 2.3  & 13   & 11   & 12   & 7.2
    & 0.20(5)
    &0.08  &0.24  &0.26  &0.26  &0.13 \\
{}[\ion{S}{iii}]  33.48~$\mu$m
    & 0.28 & 1.9  & 2.3  & 0.76 & 0.6
    & 0.04(1)
    &0.011 &0.05  &0.06  &0.015 &0.015\\
{}[\ion{Si}{ii}]  34.81~$\mu$m
    & 1.0  & 3.7  & 3.9  & 1.7  & 1.7
    & 0.07(3)
    &0.04  &0.10  &0.11  &0.03  &0.04 \\
\hline
\end{tabular}}
\medskip
The column ``average'' contains the ratio values averaged over the northern part of Cas~A and their observed scatter, and other columns contain data for the \citet{HF96} FMKs.\\
 {Notes}: the table contains data for the strongest lines only.
The regions are numbered as in \citet{HF96} with their positions
shown in Fig.~\protect\ref{FigIRvsHST}.
The ``average'' column assumes single optical line reddening
correction of 200~times. Note that the pixel sizes are different for
the IRS~LL (5\farcs08 or $6.06 \times 10^{-10}$~sr,
$\lambda > 15$~$\mu$m) and SL (1\farcs85 or $8.04 \times 10^{-11}$~sr,
$\lambda < 15$~$\mu$m) modules. 
\end{table}