All Figures

$\begin{figure} \par\mbox{\includegraphics[width=6.5cm,clip]{4091fg01.eps}\hspace... ...}\hspace{0.5cm} \includegraphics[width=6.5cm,clip]{4091fg06.eps} }\end{figure}$ Figure 1: Chandra soft X-ray contours superimposed on HST [O III] images. The contours correspond to five logarithmic intervals in the range of 1.5-50% (NGC 1386), 5-80% (Mrk 3), 5-90% (NGC 3393), 4-50% (NGC 4388), 0.5-50% (NGC 4507) and 2-50% (NGC 5347) of the peak flux. The HST images are scaled with the same criterion for each source, with the exception of NGC 4388 and NGC 4507, whose [O III] emission goes down to the 2% and the 0.1% of the peak, respectively. The images are aligned as explained in Sect. 2.2.2 and centered on the Chandra count peak.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=6.5cm,clip]{4091fg07.eps}\hspace{0.5cm} \includegraphics[width=6.5cm,clip]{4091fg08.eps} }\end{figure}$ Figure 2: Same of Fig. 1, but for NGC 5643 (8-80%) and NGC 7212 (1-50%). In the case of NGC 5643, the [O III] emission goes down to the 0.5% of the peak.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=7.5cm,clip]{4091fg09.eps}\hspace... ...4cm}\includegraphics[width=7.5cm,clip]{4091fg13.eps}\hspace*{4cm}}\end{figure}$ Figure 3: Chandra data and best fit models for the sources in our sample analysed for the first time in this paper. The inner box shows the "local'' fit for the iron line, along with a dotted line to show the energy of the neutral iron K $\alpha$ line at the redshift of the source.
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In the text

$\begin{figure} \par\includegraphics[width=16.1cm,clip]{4091fg14.eps} \end{figure}$ Figure 4: Mrk 3: XMM-Newton 190 ks combined RGS spectrum, plotted in the rest frame of the source (12-25 Å). The strongest emission features are labelled.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4091fg15.eps} \end{figure}$ Figure 5: Each symbol represents one solution in our grid of CLOUDY models that satisfies the condition of total [O III] to soft X-ray flux ratio in the range observed in our sample, plotted in a three-parameter space U, $n_{\rm e}$ and $\beta$ , i.e. the ionization parameter and the density at the beginning of the cone of gas (1 pc), and the index of the density powerlaw, represented by different symbols (triangles: $\beta =1.6$ , diamonds: $\beta =1.8$ , stars: $\beta =2.0$ , squares: $\beta =2.4$ ). The horizontal lines determine the limit corresponding to a total column density of 10²⁰ cm^-2 for each index: solutions below this limit are not plotted. Solutions with $\beta =2.2$ are not plotted for clarity reasons. The net effect of the filling factor f is to shift the density values: the two y axes refer to f=0.1 and f=0.01 (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4091fg16.eps} \end{figure}$ Figure 6: The [O III] to soft X-ray ratio plotted as a function of the radius of the gas, for different values of $\beta$ , when $\log{n_{\rm e}}=3$ and f=0.1. The corresponding values of $\log{U}$ for these solutions are ( from top to bottom): -0.85, -1.15, -1.4, -1.5, -1.6.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4091fg17.eps} \end{figure}$ Figure 7: NGC 3393: HST to Chandra soft X-ray counts ratio as a function of distance from the nucleus. The two curves refers to the photoionized models plotted in Fig. 6 (see text for details).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=6.5cm,clip]{4091fg07.eps}\hspace{0.5cm} \includegraphics[width=6.5cm,clip]{4091fg08.eps} }\end{figure}$	Figure 2: Same of Fig. 1, but for NGC 5643 (8-80%) and NGC 7212 (1-50%). In the case of NGC 5643, the [O III] emission goes down to the 0.5% of the peak.
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$\begin{figure} \par\mbox{\includegraphics[width=7.5cm,clip]{4091fg09.eps}\hspace... ...4cm}\includegraphics[width=7.5cm,clip]{4091fg13.eps}\hspace*{4cm}}\end{figure}$	Figure 3: Chandra data and best fit models for the sources in our sample analysed for the first time in this paper. The inner box shows the "local'' fit for the iron line, along with a dotted line to show the energy of the neutral iron K $\alpha$ line at the redshift of the source.
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$\begin{figure} \par\includegraphics[width=16.1cm,clip]{4091fg14.eps} \end{figure}$	Figure 4: Mrk 3: XMM-Newton 190 ks combined RGS spectrum, plotted in the rest frame of the source (12-25 Å). The strongest emission features are labelled.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4091fg16.eps} \end{figure}$	Figure 6: The [O III] to soft X-ray ratio plotted as a function of the radius of the gas, for different values of $\beta$ , when $\log{n_{\rm e}}=3$ and f=0.1. The corresponding values of $\log{U}$ for these solutions are ( from top to bottom): -0.85, -1.15, -1.4, -1.5, -1.6.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4091fg17.eps} \end{figure}$	Figure 7: NGC 3393: HST to Chandra soft X-ray counts ratio as a function of distance from the nucleus. The two curves refers to the photoionized models plotted in Fig. 6 (see text for details).
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