All Figures

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics{H4554F1.PS}} \end{figure}$ Figure 1: Hubble Space Telescope image of MCG-6-30-15 (Malkan et al. 1998). A dust lane is apparent crossing the southern part of the galactic disk.
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics{H4554F2.PS}} \end{figure}$ Figure 2: The results of photoionization models of a DWA shown over the X-ray band. Constant density ( $n_{{\rm H}} = 10$ cm^-3) gas with $N_{{\rm H}}=4\times 10^{21}$ cm^-2 was illuminated by a toy AGN SED (shown with the dashed line), and the transmitted spectrum is shown with the solid line. Typical interstellar dust was included at Galactic abundances. The positions of the most prominent photoelectric absorption edges are indicated in the lower panel. The gas was placed at different distances r from the AGN. The greatest column of O VII ( $N_{{\rm O VII}}=6\times 10^{17}$ cm^-2) was found when r=150-175 pc.
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In the text

$\begin{figure} \resizebox{\hsize}{!}{\includegraphics{H4554F3.PS}}\end{figure}$ Figure 3: The effect of grains on the transmitted spectrum (see also Komossa & Bade 1998). Both panels show the results of Cloudy models where the gas cloud was 150 pc from the AGN. The dashed curve shows the incident spectrum and the solid curve shows the transmitted spectrum. The positions of the C I, O I, Fe I, and O VII edges are indicated. Solar abundances were used for the dust-free model, except that the oxygen abundance was set to the F and G star value from Sofia & Meyer (2001).
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics{H4554F1.PS}} \end{figure}$	Figure 1: Hubble Space Telescope image of MCG-6-30-15 (Malkan et al. 1998). A dust lane is apparent crossing the southern part of the galactic disk.
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