All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0298fig1.eps}\end{figure}$ Figure 1: Background subtracted, combined MOS1+2, 0.4-10 keV light curves of the four sources, binned in 500 s intervals. Time is measured from the start of each observation. Filled squares in all panels indicate the respective background light curves, rescaled appropriately in each case (errors are smaller than the symbol size).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0298fig2.eps}\end{figure}$ Figure 2: Background subtracted, combined SIS 0 + 1, 0.5-10 keV band light curves of NGC 4235 and NGC 4639, binned in 5760 s intervals. Time is measured from the start of each observation.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0298fig3.eps}\end{figure}$ Figure 3: Top panel: Log of $\sigma ^{2}_{\rm NXS}$ plotted as a function of the log of X-ray luminosity for 33 AGN (open circles; data are taken from O'Neill et al. 2005). Filled squares indicate the [ $\log\left(\sigma^2_{\rm NXS}\right)$ , $\log(L_{\rm X}$ )] data of NGC 5273, NGC 5033 and NGC 4235, while the thick arrow indicates the 3 $\sigma$ upper limit on $\log\left(\sigma^2_{\rm NXS}\right)$ for NGC 4639. Bottom panel: the $\log$ of $\sigma ^{2}_{\rm NXS}$ plotted as a function of the $\log$ (BH mass) (in solar mass units) relation for the 33 AGN of O'Neill et al. and the four objects in our sample.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0298fig4.eps}\end{figure}$ Figure 4: Simultaneous model fit to the PN, MOS1 (open squares) and MOS2 (asterisks) fit to the NGC 5273 0.4-10 keV data. The model shown here suggests that the flux from the central engine and warm circumnuclear material is absorbed by an ionized absorber, as well as by cold galactic material in the source. An Fe K line at 6.4 keV can also be seen.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0298fig5.eps}\end{figure}$ Figure 5: The 0.4-10 keV EPIC spectra of NGC 4235, plotted together with the 2-10 keV best model fitting ``power-law plus Gaussian line'' model ( upper panel). The model is extrapolated to lower energies assuming Galactic absorption only. The respective model fitting residuals plot is shown in the lower panel of the figure (symbols are as in Fig. 4).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0298fig6.eps}\end{figure}$ Figure 6: Radial brightness profile of the central arcsec of NGC 4235 (from the F606W image). The solid line shows the best fit to the profile (the fit was performed to the innermost 2 $^{\prime \prime }$ only).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0298fig7.eps}\end{figure}$ Figure 7: The near-IR to X-ray SED for the four objects in our sample. Upper limits are 3 $\sigma$ . The solid, dotted and dashed lines indicate the mean radio-quiet quasar SED from Elvis et al., and the the 68 and 90 percentile contours on each side. Filled squares are our measurements from the HST data, open squares are IR data from the literature. Crosses indicate the nuclear SED of NGC 3998 (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0298fig8.eps}\end{figure}$ Figure 8: The $L_{\rm V}$ versus $L_{\rm X}$ plot for PG quasars (open circles), nearby Seyferts (open squares), the four Seyferts in our sample (filled squares), and NGC 3998 (cross). The solid line indicates the best linear fit to the quasar sample, and the dashed line is its extrapolation to lower luminosities.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0298fig1.eps}\end{figure}$	Figure 1: Background subtracted, combined MOS1+2, 0.4-10 keV light curves of the four sources, binned in 500 s intervals. Time is measured from the start of each observation. Filled squares in all panels indicate the respective background light curves, rescaled appropriately in each case (errors are smaller than the symbol size).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0298fig2.eps}\end{figure}$	Figure 2: Background subtracted, combined SIS 0 + 1, 0.5-10 keV band light curves of NGC 4235 and NGC 4639, binned in 5760 s intervals. Time is measured from the start of each observation.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0298fig4.eps}\end{figure}$	Figure 4: Simultaneous model fit to the PN, MOS1 (open squares) and MOS2 (asterisks) fit to the NGC 5273 0.4-10 keV data. The model shown here suggests that the flux from the central engine and warm circumnuclear material is absorbed by an ionized absorber, as well as by cold galactic material in the source. An Fe K line at 6.4 keV can also be seen.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0298fig5.eps}\end{figure}$	Figure 5: The 0.4-10 keV EPIC spectra of NGC 4235, plotted together with the 2-10 keV best model fitting ``power-law plus Gaussian line'' model ( upper panel). The model is extrapolated to lower energies assuming Galactic absorption only. The respective model fitting residuals plot is shown in the lower panel of the figure (symbols are as in Fig. 4).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0298fig6.eps}\end{figure}$	Figure 6: Radial brightness profile of the central arcsec of NGC 4235 (from the F606W image). The solid line shows the best fit to the profile (the fit was performed to the innermost 2 $^{\prime \prime }$ only).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0298fig8.eps}\end{figure}$	Figure 8: The $L_{\rm V}$ versus $L_{\rm X}$ plot for PG quasars (open circles), nearby Seyferts (open squares), the four Seyferts in our sample (filled squares), and NGC 3998 (cross). The solid line indicates the best linear fit to the quasar sample, and the dashed line is its extrapolation to lower luminosities.
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