$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f1.ps} \end{figure}$ Figure 1: The LECS, MECS and PDS spectra of PKS 2126-158 fitted with a power law model with Galactic absorption.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f2.ps} \end{figure}$ Figure 2: $N_{\rm H}$ vs. redshift $\chi ^2$ 67%, 90% and 99% confidence contours for a power law continuum.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f3.ps} \end{figure}$ Figure 3: Ratio between the BeppoSAX LECS, MECS and PDS spectra of PKS 2126-158 and the best fitting power law with exponential cutoff model.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f4.ps} \end{figure}$ Figure 4: $N_{\rm H}$ vs. redshift $\chi ^2$ 67%, 90% and 99% confidence contours for a broken power law continuum.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f5.ps} \end{figure}$ Figure 5: $N_{\rm H}$ vs. redshift $\chi ^2$ 67%, 90% and 99% confidence contours for a power law with exponential cutoff continuum.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f6.ps} \end{figure}$ Figure 6: Ionization parameter vs. iron abundance $\chi ^2$ 67%, 90% and 99% confidence contours for a power law with exponential cut-off continuum.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f7.ps} \end{figure}$ Figure 7: 2-10 keV (filled circles) and 0.1-2 keV (open triangles) fluxes observed by Einstein, EXOSAT, ROSAT, ASCA, BeppoSAX and XMM-Newton in the last 22 yrs. Error bars are 1 $\sigma$ statistical uncertainties.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f1.ps} \end{figure}$	Figure 1: The LECS, MECS and PDS spectra of PKS 2126-158 fitted with a power law model with Galactic absorption.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f2.ps} \end{figure}$	Figure 2: $N_{\rm H}$ vs. redshift $\chi ^2$ 67%, 90% and 99% confidence contours for a power law continuum.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f3.ps} \end{figure}$	Figure 3: Ratio between the BeppoSAX LECS, MECS and PDS spectra of PKS 2126-158 and the best fitting power law with exponential cutoff model.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f4.ps} \end{figure}$	Figure 4: $N_{\rm H}$ vs. redshift $\chi ^2$ 67%, 90% and 99% confidence contours for a broken power law continuum.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f5.ps} \end{figure}$	Figure 5: $N_{\rm H}$ vs. redshift $\chi ^2$ 67%, 90% and 99% confidence contours for a power law with exponential cutoff continuum.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f6.ps} \end{figure}$	Figure 6: Ionization parameter vs. iron abundance $\chi ^2$ 67%, 90% and 99% confidence contours for a power law with exponential cut-off continuum.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3466_f7.ps} \end{figure}$	Figure 7: 2-10 keV (filled circles) and 0.1-2 keV (open triangles) fluxes observed by Einstein, EXOSAT, ROSAT, ASCA, BeppoSAX and XMM-Newton in the last 22 yrs. Error bars are 1 $\sigma$ statistical uncertainties.
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