All Figures

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{2193fig1.ps} \end{figure}$ Figure 1: A deconvolved ISOCAM 14.3 $\mu$ m contour map of Mkn 297 overlaid on a HST image (Filter: F555W, Centre: 5407 Å, Bandwidth: 1236 Å). The contour levels, in the order a to f, are as follows (in units of mJy/arcsec²): 0.7, 1.0, 1.5, 2.0, 2.5 and 3.0. The seven regions identified by white numbers correspond to the positions of well-defined structures or extensions of emission seen in one or more of the bandpasses presented in Fig. 2. Small black underlined numbers identify some H $_{\alpha }$ emission knots as designated by Hecquet et al. (1987), and help relate this map to earlier published data. Source 4 coincides approximately with the nuclear region of galaxy A and source 2 with the nuclear region of galaxy B, oriented north-south. However the strongest source, No. 1, does not correspond to either nucleus. The open square denotes the position of one of the brightest known radio supernovae, SN 1982aa (Mkn 297A) and corresponds to H $_{\alpha }$ source 14. The position of a knot of 2MASS K-band emission is indicated by the small black triangle (see also Fig. 3). The filled light-coloured square designates the position of the centre of the PHT-S aperture, and the large dashed square on which it is centred indicates the size of the PHT-S aperture. The LWS aperture had the same centre, but was much larger than the region shown here.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{2193fig2.eps} \end{figure}$ Figure 2: Deconvolved ISOCAM contour maps overlaid on the HST image: i) 6.7 $\mu$ m, ii) 7.7 $\mu$ m, iii) 12 $\mu$ m and iv) 14.3 $\mu$ m maps are presented. Seven regions of emission are identified (the numbers running from 1 to 7). Sources 2 and 4 coincide with the nuclear regions of the constituent interacting galaxies. The contour levels in the sequence a to f are as follows (in units of mJy/arcsec²): i) 0.4, 0.7, 1.0, 1.5 and 2.0; ii) 0.7, 1.0, 1.5, 2.0 and 2.5; iii) 0.7, 1.0, 1.5 and 2.0; iv) 0.7, 1.0, 1.5, 2.0, 2.5 and 3.0.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{2193fig3.ps}} \end{figure}$ Figure 3: An overlay of the ISO 15 $\mu$ m (white contours) and 2MASS K-band (black contours) on the HST image of the Mkn 297 galaxy. The HST image and ISO contours are as in Fig. 1. The 2MASS contours are equispaced at levels 350, 355, 360, 365, 370, 375 and 380 detector units. (We have not absolutely calibrated the 2MASS data, being only interested here in spatial information.)
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{2193fig4.ps}} \end{figure}$ Figure 4: The 14.3/6.7 um ratio map overlaid on the HST image of Mkn 297. Deconvolved 6.7 and 14.3 $\mu$ m maps were used and the ratio map was convolved with the 6.7 $\mu$ m point spread function. The ratio contour levels in ascending order are: 1.0, 1.5, 2.0, 2.5, 3.0, 3.3.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2193fig5.eps} \end{figure}$ Figure 5: PHT-SL spectrum of Mkn 297, with the PHT-S aperture centred 3'' East of the nucleus of galaxy A. The PAH features are indicated. The spectrum has been Hanning smoothed. The flux levels are those recorded in the PHT-S aperture, before scaling to the larger ISOCAM field-of-view (see Sect. 2.4).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{2193fig6.ps}} \end{figure}$ Figure 6: LWS spectra of a) the [OI] line at 63.1 $\mu$ m, b) the [OIII] line at 88.8 $\mu$ m ( top right), c) the [OI] line at 146.7 $\mu$ m and d) the [CII] at 157.7 $\mu$ m.
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In the text

$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{2193fig7.ps} } \end{figure}$ Figure 7: Spectral energy distribution of Mkn 297 using ISO and IRAS flux data, including the key for the different symbols. The PHT-S spectrum has been normalised to the CAM 7.7 $\mu$ m data point as described in the text. The models fitted to the data are described in Sect. 4.4.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{2193fig8.ps}} \end{figure}$ Figure 8: An overlay of the Yin (1994) 6 cm radio contours on the HST image of Mkn 297.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{2193fig3.ps}} \end{figure}$	Figure 3: An overlay of the ISO 15 $\mu$ m (white contours) and 2MASS K-band (black contours) on the HST image of the Mkn 297 galaxy. The HST image and ISO contours are as in Fig. 1. The 2MASS contours are equispaced at levels 350, 355, 360, 365, 370, 375 and 380 detector units. (We have not absolutely calibrated the 2MASS data, being only interested here in spatial information.)
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{2193fig4.ps}} \end{figure}$	Figure 4: The 14.3/6.7 um ratio map overlaid on the HST image of Mkn 297. Deconvolved 6.7 and 14.3 $\mu$ m maps were used and the ratio map was convolved with the 6.7 $\mu$ m point spread function. The ratio contour levels in ascending order are: 1.0, 1.5, 2.0, 2.5, 3.0, 3.3.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2193fig5.eps} \end{figure}$	Figure 5: PHT-SL spectrum of Mkn 297, with the PHT-S aperture centred 3'' East of the nucleus of galaxy A. The PAH features are indicated. The spectrum has been Hanning smoothed. The flux levels are those recorded in the PHT-S aperture, before scaling to the larger ISOCAM field-of-view (see Sect. 2.4).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{2193fig6.ps}} \end{figure}$	Figure 6: LWS spectra of a) the [OI] line at 63.1 $\mu$ m, b) the [OIII] line at 88.8 $\mu$ m ( top right), c) the [OI] line at 146.7 $\mu$ m and d) the [CII] at 157.7 $\mu$ m.
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$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{2193fig7.ps} } \end{figure}$	Figure 7: Spectral energy distribution of Mkn 297 using ISO and IRAS flux data, including the key for the different symbols. The PHT-S spectrum has been normalised to the CAM 7.7 $\mu$ m data point as described in the text. The models fitted to the data are described in Sect. 4.4.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics*{2193fig8.ps}} \end{figure}$	Figure 8: An overlay of the Yin (1994) 6 cm radio contours on the HST image of Mkn 297.
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