All Figures

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0838fig1.eps}\end{figure}$ Figure 1: Illustration of the decomposition used to isolate the AGN continuum. Top panel: ISOPHOT-S spectrum of the mixed AGN/starburst galaxy NGC 7469, showing strong PAH emission as well as an elevated continuum. Bottom panel: Cutout of the region around the 6.2 $\mu$ m PAH feature. Top continuous line = observed spectrum. Top dotted line = fit by the sum of the rebinned SWS M 82 PAH spectrum and a linear AGN continuum. Bottom dotted line = fitted AGN continuum. Bottom continuous line = difference of observed spectrum and fitted PAH component. The thick vertical line indicates the AGN 6 $\mu$ m continuum, obtained by evaluating the fitted continuum at that wavelength. An additional correction is applied to this value to account for differences between M 82 and an average starburst.
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In the text

$\begin{figure} \par\includegraphics[width=8.65cm,clip]{0838fig2.eps}\end{figure}$ Figure 2: Distance distribution for the objects in our sample, separated by type 1 (1 to 1.5) and 2 (1.8 to 2) Seyferts. Light shading identifies those Seyfert 2's where no absorption correction to the AGN hard X-ray emission was possible. We adopted distances derived assuming H₀=75, q₀=0.5 except for M 51 (8.4 Mpc), M 81 (3.63 Mpc) and Circinus (4 Mpc).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0838fig3.eps}\end{figure}$ Figure 3: Observed hard X-ray fluxes vs. 6 $\mu$ m AGN continuum for the sample galaxies. Diamonds indicate type 1 Seyferts (including objects classified as types 1, 1.2, 1.5), asterisks indicate type 2 Seyferts (including objects classified as types 1.8, 1.9, 2). Thin horizontal lines, in most cases smaller than the symbols, indicate the 1 $\sigma$ uncertainty of the 6 $\mu$ m detections.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0838fig4.eps}\end{figure}$ Figure 4: Hard X-ray fluxes corrected for absorption vs. 6 $\mu$ m AGN continuum for those objects where an absorption corrected X-ray flux was available. Symbols are as in Fig. 3. The dotted line indicates slope 1, it is not a fit.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0838fig5.eps}\end{figure}$ Figure 5: Hard X-ray luminosities corrected for absorption vs. 6 $\mu$ m AGN continuum luminosities for those objects where an absorption corrected X-ray flux was available. Symbols are as in Fig. 3. The dotted line indicates slope 1, it is not a fit.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0838fig6.eps}\end{figure}$ Figure 6: Histograms showing for the two Seyfert types the logarithm of the ratio between intrinsic hard X-ray flux and 6 $\mu$ m AGN continuum. Dark shadings indicates objects with upper limits for the 6 $\mu$ m continuum, i.e. lower limits for the ratio shown.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0838fig7.eps}\end{figure}$ Figure 7: Ratio of intrinsic hard X-ray flux and 6 $\mu$ m AGN continuum, plotted as a function of X-ray absorbing column.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0838fig8.eps}\end{figure}$ Figure 8: Distribution of luminosities of the 6.2 $\mu$ m PAH emission feature. Dark shading indicates upper limits.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0838fig9.eps}\end{figure}$ Figure 9: Distribution of luminosities of the 6 $\mu$ m AGN continuum. Dark shading indicates upper limits.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0838f10.eps} % \end{figure}$ Figure 10: Distribution of extinction corrected hard X-ray luminosities.
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In the text

$\begin{figure} \par\includegraphics[width=8.65cm,clip]{0838fig2.eps}\end{figure}$	Figure 2: Distance distribution for the objects in our sample, separated by type 1 (1 to 1.5) and 2 (1.8 to 2) Seyferts. Light shading identifies those Seyfert 2's where no absorption correction to the AGN hard X-ray emission was possible. We adopted distances derived assuming H₀=75, q₀=0.5 except for M 51 (8.4 Mpc), M 81 (3.63 Mpc) and Circinus (4 Mpc).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0838fig3.eps}\end{figure}$	Figure 3: Observed hard X-ray fluxes vs. 6 $\mu$ m AGN continuum for the sample galaxies. Diamonds indicate type 1 Seyferts (including objects classified as types 1, 1.2, 1.5), asterisks indicate type 2 Seyferts (including objects classified as types 1.8, 1.9, 2). Thin horizontal lines, in most cases smaller than the symbols, indicate the 1 $\sigma$ uncertainty of the 6 $\mu$ m detections.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0838fig4.eps}\end{figure}$	Figure 4: Hard X-ray fluxes corrected for absorption vs. 6 $\mu$ m AGN continuum for those objects where an absorption corrected X-ray flux was available. Symbols are as in Fig. 3. The dotted line indicates slope 1, it is not a fit.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0838fig5.eps}\end{figure}$	Figure 5: Hard X-ray luminosities corrected for absorption vs. 6 $\mu$ m AGN continuum luminosities for those objects where an absorption corrected X-ray flux was available. Symbols are as in Fig. 3. The dotted line indicates slope 1, it is not a fit.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0838fig6.eps}\end{figure}$	Figure 6: Histograms showing for the two Seyfert types the logarithm of the ratio between intrinsic hard X-ray flux and 6 $\mu$ m AGN continuum. Dark shadings indicates objects with upper limits for the 6 $\mu$ m continuum, i.e. lower limits for the ratio shown.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0838fig7.eps}\end{figure}$	Figure 7: Ratio of intrinsic hard X-ray flux and 6 $\mu$ m AGN continuum, plotted as a function of X-ray absorbing column.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0838fig8.eps}\end{figure}$	Figure 8: Distribution of luminosities of the 6.2 $\mu$ m PAH emission feature. Dark shading indicates upper limits.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0838fig9.eps}\end{figure}$	Figure 9: Distribution of luminosities of the 6 $\mu$ m AGN continuum. Dark shading indicates upper limits.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0838f10.eps} % \end{figure}$	Figure 10: Distribution of extinction corrected hard X-ray luminosities.
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