All Figures

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3893fig1.ps}\hspace*{3mm} \includegraphics[width=7.7cm,clip]{3893fig2.ps} \end{figure}$ Figure 1: Distribution of the photon index before ( left) and after ( right) correction for Compton-thick candidates (after Table 4) for which a value of $\Gamma =1.62$ is assumed (see text for details).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3893fig3.ps}\hspace*{3mm} \includegraphics[width=7.6cm,clip]{3893fig4.ps} \end{figure}$ Figure 2: Distribution of the absorption column densities before ( left) and after ( right) correction for Compton-thick candidates (after Table 4). Upper and lower limits are indicated with arrows.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3893fig5.ps}\hspace*{3mm} \includegraphics[width=7.7cm,clip]{3893fig6.ps} \end{figure}$ Figure 3: Distribution of the 2-10 keV luminosities before ( left) and after ( right) correction for Compton-thick candidates (after Table 4). Upper limits have been indicated with arrows.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3893fig7.ps} \end{figure}$ Figure 4: Diagram of the absorbing column density $N{_{\rm H}}$ versus the ratio between the observed 2-10 keV flux and the reddening-corrected [O III] flux taken from Panessa (2004). Filled polygons are type 1 Seyferts and open polygons are type 2 Seyferts. The shaded region (lower-left to upper-right diagonals) indicates the expected correlation under the assumption that $L_{2-10~\rm keV}$ is absorbed by the $N{_{\rm H}}$ reported on the ordinate, starting from the average $F_{\rm HX}$ / $F_{\rm [O~III]}$ ratio observed in type 1 Seyfert galaxies and by assuming a 1% reflected component. Also, the shaded region (upper-left to lower-right diagonals) obtained by Maiolino et al. (1998) is shown.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{Figa1.eps}\end{figure}$

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{FigA2.eps}\end{figure}$

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{FigA3.eps}\end{figure}$

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{FigA4.eps}\end{figure}$

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3893fig1.ps}\hspace*{3mm} \includegraphics[width=7.7cm,clip]{3893fig2.ps} \end{figure}$	Figure 1: Distribution of the photon index before ( left) and after ( right) correction for Compton-thick candidates (after Table 4) for which a value of $\Gamma =1.62$ is assumed (see text for details).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3893fig3.ps}\hspace*{3mm} \includegraphics[width=7.6cm,clip]{3893fig4.ps} \end{figure}$	Figure 2: Distribution of the absorption column densities before ( left) and after ( right) correction for Compton-thick candidates (after Table 4). Upper and lower limits are indicated with arrows.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3893fig5.ps}\hspace*{3mm} \includegraphics[width=7.7cm,clip]{3893fig6.ps} \end{figure}$	Figure 3: Distribution of the 2-10 keV luminosities before ( left) and after ( right) correction for Compton-thick candidates (after Table 4). Upper limits have been indicated with arrows.
Open with DEXTER