All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1802fig1.ps} \end{figure}$ Figure 1: PG 1001+054: the confidence levels to 68.3%, 90% and 99% for two interesting parameters: column density and ionization parameter are shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{1802fig2.ps} \end{figure}$ Figure 2: PG 2112+059: the confidence levels to 68.3%, 90% and 99% for two interesting parameters: column density and ionization parameter are shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1802fig3.ps} \end{figure}$ Figure 3: PG 1535+547: the data compared with the best fitted model for a power law continuum absorbed by ionized material and partially covered by neutral material (pn: filled circles and MOS filled triangles). The best fit parameters are given in Table 4. Systematic residuals are appearing between 4 and 6 keV, i.e. the energy range of the fluorescence Fe K $_{\alpha }$ line emission.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{1802fig4.ps} \end{figure}$ Figure 4: PG 1535+547: the confidence levels to 68.3%, 90% and 99% for the two interesting parameters of a Gaussian line, line energy and and line width, are shown. Both are in the rest-frame of PG 1535+547. The line energy is not compatible with an emission of neutral iron at $6.4\;\rm keV$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1802fig5.ps} \end{figure}$ Figure 5: PG 1535+547: the data compared with the best fitted model for a power-law continuum absorbed by ionized material and partially covered by neutral material. The fluorescence Fe K $_{\alpha }$ line is described by a relativistic disk line (XSPEC model laor, Laor 1991). MOS data are given by filled triangles and pn data by filled circles, respectively. The best fit parameters are given in Table 4 (fit 15).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{1802fig6.ps} \end{figure}$ Figure 6: PG 1535+547: the confidence levels to 68.3%, 90% and 99% for the two interesting parameters: column density of ionized absorber and column density of neutral absorber are shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1802fig7.ps} \end{figure}$ Figure 7: PG 1535+547: the confidence levels to 68.3%, 90% and 99% for the two interesting parameters, column density of the ionized absorber and ionization parameter, are shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1802fig8.ps} \end{figure}$ Figure 8: PG 1535+547: confidence levels to 68.3% (green), 90% (red) and 99% (black) for the two interesting parameters: inner and outer radius, which characterize the area of the accretion disk emitting fluorescence Fe K $_{\alpha }$ line.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1802fig9.ps} \end{figure}$ Figure 9: The observed UV spectra of PG 1001+054, PG 2112+059 and PG 1535+547 show some common absorption features due to mildly ionized material in our Galaxy, but it is clear that the overall UV spectral shapes are widely different.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1802fi10.ps} \end{figure}$ Figure 10: Only when PG 2112+059 is corrected for reddening in our Galaxy and PG 1535+547 is corrected for intrinsic reddening the spectra at rest frame of the three objects become very similar.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1802fi11.ps} \end{figure}$ Figure 11: Spectral energy distribution for PG 1001+054 , PG 2112+059 and PG 1535+547. The OM observations (red error bars) have been used to re-scale UV spectra (IUE and HST) for PG 1001+054 and PG 2112+059. Unfortunately, for PG 1535+547 the are no OM data available to assure the proper scaling of the optical-UV-X-ray ranges. Optical-UV have been corrected for galactic reddening and X-ray corrected for galactic absorption. Input ionizing spectra in Cloudy models are drawn as dashed lines and output (transmitted and diffuse emission) as solid lines, both in the same color as object data.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1802fig1.ps} \end{figure}$	Figure 1: PG 1001+054: the confidence levels to 68.3%, 90% and 99% for two interesting parameters: column density and ionization parameter are shown.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{1802fig2.ps} \end{figure}$	Figure 2: PG 2112+059: the confidence levels to 68.3%, 90% and 99% for two interesting parameters: column density and ionization parameter are shown.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1802fig3.ps} \end{figure}$	Figure 3: PG 1535+547: the data compared with the best fitted model for a power law continuum absorbed by ionized material and partially covered by neutral material (pn: filled circles and MOS filled triangles). The best fit parameters are given in Table 4. Systematic residuals are appearing between 4 and 6 keV, i.e. the energy range of the fluorescence Fe K $_{\alpha }$ line emission.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{1802fig4.ps} \end{figure}$	Figure 4: PG 1535+547: the confidence levels to 68.3%, 90% and 99% for the two interesting parameters of a Gaussian line, line energy and and line width, are shown. Both are in the rest-frame of PG 1535+547. The line energy is not compatible with an emission of neutral iron at $6.4\;\rm keV$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{1802fig6.ps} \end{figure}$	Figure 6: PG 1535+547: the confidence levels to 68.3%, 90% and 99% for the two interesting parameters: column density of ionized absorber and column density of neutral absorber are shown.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1802fig7.ps} \end{figure}$	Figure 7: PG 1535+547: the confidence levels to 68.3%, 90% and 99% for the two interesting parameters, column density of the ionized absorber and ionization parameter, are shown.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1802fig8.ps} \end{figure}$	Figure 8: PG 1535+547: confidence levels to 68.3% (green), 90% (red) and 99% (black) for the two interesting parameters: inner and outer radius, which characterize the area of the accretion disk emitting fluorescence Fe K $_{\alpha }$ line.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1802fig9.ps} \end{figure}$	Figure 9: The observed UV spectra of PG 1001+054, PG 2112+059 and PG 1535+547 show some common absorption features due to mildly ionized material in our Galaxy, but it is clear that the overall UV spectral shapes are widely different.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1802fi10.ps} \end{figure}$	Figure 10: Only when PG 2112+059 is corrected for reddening in our Galaxy and PG 1535+547 is corrected for intrinsic reddening the spectra at rest frame of the three objects become very similar.
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