All Figures

$\begin{figure} \par\includegraphics[width=17.2cm,clip]{0517fig1.ps} \end{figure}$ Figure 1: The 0.4-10 keV pn lightcurves of 1H1219+301, H1426+428 and Markarian 501 (from orbits 474 and 475), all in 300 s time bins, and the RGS lightcurve of PKS 0548-322 (0.35-2.5 keV; 600 s time bins).
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In the text

$\begin{figure} \par\includegraphics[width=14.2cm,clip]{0517fig2.ps} \end{figure}$ Figure 2: Left panels: ratios of the pn spectra of 1H1219+301, H1426+428 and Markarian 501 to fitted power-laws with fixed Galactic neutral absorption (plotted in the observed frame). Right panels: the pn spectra of 1H1219+301, H1426+428 and Markarian 501 with superimposed best-fit broken power-law models (with fixed Galactic neutral absorption; plotted in the observed frame). In all plots, the spectra are grouped to a minimum of 40, 350 and 100 counts per bin respectively.
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In the text

$\begin{figure} \par\includegraphics[width=14.3cm,clip]{0517fig3.ps} \end{figure}$ Figure 3: The statistical significance of narrow absorption and emission features in the RGS spectra of 1H1219+301 ( top), and the RGS spectrum itself with best-fit broken power-law model (red) superimposed ( bottom), plotted in the source rest frame.
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In the text

$\begin{figure} \par\includegraphics[width=14.1cm,clip]{0517fig4.ps} \end{figure}$ Figure 4: The statistical significance of narrow absorption and emission features in the RGS spectra of H1426+428 ( top), and the RGS spectrum itself with best-fit broken power-law model (red) superimposed ( bottom), plotted in the source rest frame.
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In the text

$\begin{figure} \par\includegraphics[width=14.1cm,clip]{0517fig5.ps} \end{figure}$ Figure 5: The statistical significance of narrow absorption and emission features in the RGS spectra of Markarian 501 ( top), and the RGS spectrum itself with best-fit broken power-law model (red) superimposed ( bottom), plotted in the source rest frame.
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In the text

$\begin{figure} \par\includegraphics[width=14.2cm,clip]{0517fig6.ps} \end{figure}$ Figure 6: The statistical significance of narrow absorption and emission features in the RGS spectra of PKS 0548-322 ( top), and the RGS spectrum itself with best-fit broken power-law model (red) superimposed ( bottom), plotted in the source rest frame.
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In the text

$\begin{figure} \par\includegraphics[width=12.2cm,clip]{0517fig7.eps} \end{figure}$ Figure 7: 2-10 keV fluxes of 1H1219+301, H1426+428, Markarian 501 and PKS 0548-322 observed with Einstein, ROSAT, BBXRT, ASCA, BeppoSAX and XMM-Newton. Observations where intrinsic absorption was reported are circled.
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In the text

$\begin{figure} \par\includegraphics[width=17.2cm,clip]{0517fig1.ps} \end{figure}$	Figure 1: The 0.4-10 keV pn lightcurves of 1H1219+301, H1426+428 and Markarian 501 (from orbits 474 and 475), all in 300 s time bins, and the RGS lightcurve of PKS 0548-322 (0.35-2.5 keV; 600 s time bins).
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$\begin{figure} \par\includegraphics[width=14.3cm,clip]{0517fig3.ps} \end{figure}$	Figure 3: The statistical significance of narrow absorption and emission features in the RGS spectra of 1H1219+301 ( top), and the RGS spectrum itself with best-fit broken power-law model (red) superimposed ( bottom), plotted in the source rest frame.
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$\begin{figure} \par\includegraphics[width=14.1cm,clip]{0517fig4.ps} \end{figure}$	Figure 4: The statistical significance of narrow absorption and emission features in the RGS spectra of H1426+428 ( top), and the RGS spectrum itself with best-fit broken power-law model (red) superimposed ( bottom), plotted in the source rest frame.
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$\begin{figure} \par\includegraphics[width=14.1cm,clip]{0517fig5.ps} \end{figure}$	Figure 5: The statistical significance of narrow absorption and emission features in the RGS spectra of Markarian 501 ( top), and the RGS spectrum itself with best-fit broken power-law model (red) superimposed ( bottom), plotted in the source rest frame.
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$\begin{figure} \par\includegraphics[width=14.2cm,clip]{0517fig6.ps} \end{figure}$	Figure 6: The statistical significance of narrow absorption and emission features in the RGS spectra of PKS 0548-322 ( top), and the RGS spectrum itself with best-fit broken power-law model (red) superimposed ( bottom), plotted in the source rest frame.
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$\begin{figure} \par\includegraphics[width=12.2cm,clip]{0517fig7.eps} \end{figure}$	Figure 7: 2-10 keV fluxes of 1H1219+301, H1426+428, Markarian 501 and PKS 0548-322 observed with Einstein, ROSAT, BBXRT, ASCA, BeppoSAX and XMM-Newton. Observations where intrinsic absorption was reported are circled.
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