All Figures

$\begin{figure} \par\includegraphics[width=5cm,height=3cm,angle=0]{7569fi1a.ps}\i... ...ps}\includegraphics[width=5.cm,height=3.cm,angle=0]{7569fi1n.ps}\par\end{figure}$ Figure 1: Photon index $\Gamma$ ( first row), R ( second row), $E_{\rm c}$ ( third row), and $N_{\rm H}$ ( fourth row) in units of cm^-2 distributions for the whole dataset ( left column), for type I objects ( center column), and for type II objects ( right column).
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In the text

$\begin{figure} \par\includegraphics[width=5cm,height=3cm,angle=0]{7569fi2a.ps}\i... ...9fi2e.ps}\includegraphics[width=5cm,height=3cm,angle=0]{7569fi2f.ps}\end{figure}$ Figure 2: Distribution of the Fek $\alpha$ emission line energy centroid ( first row) and of its EW ( second row). Distributions for the whole sample of observations ( left panel), for the type I objects ( center panel) and for type II objects ( right panel).
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,height=6.3cm,angle=0]{7569fi3a.p... ...b.ps}\includegraphics[width=5.8cm,height=6.7cm,angle=0]{7569fi3c.ps}\end{figure}$ Figure 3: Left panel: Log ( $EW_{{\rm FeK}\alpha }$ ) vs. Log ( $N_{\rm H}$ ). As expected, the sources are divided in two families: the ones that follow the expectations if the FeK $\alpha$ line is produced in the absorption matter and the candidate Compton-thick ones that display low absorption and large EW. The solid line indicates the prediction by Makishima (1986). Center panel: Log ( $F_{2-10~{\rm KeV}}$ / $F_{20-100~{\rm KeV}}$ ) vs. Log ( $N_{\rm H}$ ). The two quantities are correlated as expected since the 2-10 keV band is strongly affected by the absorption while the 20-100 band is almost free from absorption. The solid line is the best fit obtained with linear regression methods Right panel: Log ( $EW_{{\rm FeK}\alpha }$ ) vs. Log ( $F_{2-10~{\rm KeV}}$ / $F_{20-100~{\rm KeV}}$ ). The two quantities are strongly correlated ( $P_{\rm null} \leq 0.01$ ). The ratio between X-ray fluxes is a model independent indicator of the absorption affecting the low energy band. Thus, this correlation strongly indicates that the narrow component of FeK $\alpha$ line in emission is indeed produced by the same matter responsible for the absorption. The solid line is the linear regression obtained using Bukley-James method (Isobe et al. 1986).
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In the text

$\begin{figure} \par {\hspace*{2.9cm}\includegraphics[width=5.8cm,height=6.05cm,a... ....ps}\includegraphics[width=5.8cm,height=6.05cm,angle=0]{7569fi4e.ps}\end{figure}$ Figure 4: Panel a): Log ( $EW_{{\rm FeK}_{\alpha }}$ ) vs. $L_{2-10,~{\rm observed}}$ . Panel b): Log ( $EW_{{\rm FeK}_{\alpha }}$ ) vs. $F_{2-10,~{\rm observed}}$ . Panel c): Log ( $EW_{{\rm FeK}_{\alpha }}$ ) vs. $L_{20-100,~{\rm observed}}$ . Panel d): the same as panel c) but only for Seyfert 1 objects. Panel e): Log ( $EW_{{\rm FeK}_{\alpha }}$ ) vs. $F_{20-100,~{\rm observed}}$ . Solid lines in panel a), b), and c) are the linear regressions obtained for the whole sample of observations. The dashed line in panels c) and e) is the linear regression obtained considering only type I objects. As visible in panel b) the less scattered relation is obtained considering the 2-10 keV observed flux. The relation is linear, as expected if the correlation is due to selection effects, i.e.considering that in faint objects only large EW were detectable by the MECS instruments on-board BeppoSAX.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,height=6cm,angle=0]{7569fi5a.ps}... ...i5b.ps}\includegraphics[width=5.8cm,height=6cm,angle=0]{7569fi5c.ps}\end{figure}$ Figure 5: Left panel: photon index $\Gamma$ plotted versus the measured $N_{\rm H}$ (in units of cm²). No significant trend relating these two quantities is found; center panel: R vs. $E_{\rm c}$ (in units keV), no correlation is found between these quantities; right panel: R vs. $\Gamma$ . The two quantities are correlated with a high significance level ( $P_{\rm null} \leq 1$ %). The line is the linear regression best fit.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,height=3cm,angle=0]{7569fi1a.ps}\i... ...ps}\includegraphics[width=5.cm,height=3.cm,angle=0]{7569fi1n.ps}\par\end{figure}$	Figure 1: Photon index $\Gamma$ ( first row), R ( second row), $E_{\rm c}$ ( third row), and $N_{\rm H}$ ( fourth row) in units of cm^-2 distributions for the whole dataset ( left column), for type I objects ( center column), and for type II objects ( right column).
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$\begin{figure} \par\includegraphics[width=5cm,height=3cm,angle=0]{7569fi2a.ps}\i... ...9fi2e.ps}\includegraphics[width=5cm,height=3cm,angle=0]{7569fi2f.ps}\end{figure}$	Figure 2: Distribution of the Fek $\alpha$ emission line energy centroid ( first row) and of its EW ( second row). Distributions for the whole sample of observations ( left panel), for the type I objects ( center panel) and for type II objects ( right panel).
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