All Figures

$\begin{figure} \par\includegraphics[height=7.5cm,width=8.3cm,angle=0,clip]{Hg041_f1.ps}\end{figure}$ Figure 1: A zoom in MECS 4-10 keV of data/model ratios when the spectrum is fitted with BLM (panel a) or with the simplified model described in the text (panel b). Data have been binned adopting 3 bins per resolution element (FWHM). This choice maximize the S/N ratio per bin still providing the minimum over-sampling to retain the spectral information. The continuous line is the profile of the absorption edge convoluted through the MECS response. Panel c) shows the ratio of Dec. 2001 to the sum of the other spectra.
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In the text

$\begin{figure} \par\includegraphics[height=4cm,width=4cm,angle=-90,clip]{Hg041_f... ...}\includegraphics[height=4cm,width=4cm,angle=-90,clip]{Hg041_f2b.ps}\end{figure}$ Figure 2: Contour plot of the edge optical depth vs. energy ( left) and absorption line intensity vs. energy ( right). Confidence levels are at 68%, 90%, 99%
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm,width=7.5cm,clip]{Hg041_f3.ps}\end{figure}$ Figure 3: XSTAR simulation. The energy of the Fe absorption edge in the external ionized gas is plotted versus the covered fraction of the internal cold gas with $N{\rm _H=1.5\times 10^{23}}$ cm^-2. The case of Dec. 2001 is plotted with a diamond. The incident continuum is a cut-off power-law with ${\rm\Gamma }=1.7$ and $E_{\rm c}=130$ keV. The plot can explain the appearance of the absorption feature only in a peculiar state of NGC 4151 when the central source was almost uncovered.
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In the text

$\begin{figure} \par\includegraphics[height=4cm,width=4cm,angle=-90,clip]{Hg041_f... ...}\includegraphics[height=4cm,width=4cm,angle=-90,clip]{Hg041_f2b.ps}\end{figure}$	Figure 2: Contour plot of the edge optical depth vs. energy ( left) and absorption line intensity vs. energy ( right). Confidence levels are at 68%, 90%, 99%
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