All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0148fig1.eps} \end{figure}$ Figure 1: Red magnitude distribution of the 28 sources in the HBS28 sample. For most of the object (26) the magnitude is the APM red magnitude, while for the 2 faintest sources the R magnitude is considered.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0148fig2.eps} \end{figure}$ Figure 2: Redshift distribution of the 27 extragalactic sources in the HBS28 sample. The shaded area represents the type 2 objects asdefined in the text.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{0148fig3.eps} \end{figure}$ Figure 3: The optical spectra of 10 newly discovered Broad Emission Lines AGNs ( ${\it FWHM}>2000$ km s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0148fig4.eps} \end{figure}$ Figure 4: The spectra of the 2 NLSy1 candidates discovered in the sample: XBS J023713.5-522734 ( top) and XBS J205829.9-423634 ( bottom). The two small boxes inside the two figures show the expanded region around the Fe II $\lambda$ 4600 Å hump.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0148fig5.eps} \end{figure}$ Figure 5: Top panel: the spectrum of the NEL AGN (a Seyfert 2) XBS J040758.9-712833. Bottom panel: The spectrum of the object XBS J193248.8-723355 optically classified as a Emission Line Galaxy (ELG, i.e. a starburst or a LINER, see text for details). As explained in the text, the X-ray analysis indicates the presence of an AGN in this object.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0148fig6.eps} \end{figure}$ Figure 6: The spectra of the two Sy1.9 discovered in the sample: XBS J040658.8-712457 ( top) and XBS J031146.1-550702 ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0148fig7.eps} \end{figure}$ Figure 7: The hardness-ratio HR3 versus HR2. Filled circles represent the type 2 objects while the open circles are the type 1 objects.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0148fig8.eps} \end{figure}$ Figure 8: The X-ray photon-index distribution of the type 1objects obtained from the spectral fitting.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0148fig9.eps} \end{figure}$ Figure 9: The optical spectra of the 2 type 2 QSO discovered in the HBS28 sample: bottom panel: XBS J013240.1-133307, top panel: XBS J204043.4-004548.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0148fig10.eps} \end{figure}$ Figure 10: The distribution of the intrinsic $N_{\rm H}$ derived from the spectral fit, for type 1 objects and type 2 objects. The shaded histograms show the detections while the empty histograms represent the upper limits on $N_{\rm H}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0148fig11.eps} \end{figure}$ Figure 11: The intrinsic $N_{\rm H}$ versus the unabsorbed X-ray luminosity in the 2-10 keV energy range for a) type 1 objects (open circles) and for b) the type 2 objects (filled circles).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0148fig12.eps} \end{figure}$ Figure 12: The ratio between the (observed) flux between 2 and 10 keV and the optical flux (see text for details) versus the observed 2-10 keV flux. The loci of constant R (Cousins) magnitudes are also plotted for R=16, 18, 20 and 22. Symbols are the same as in previous figure.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=-90]{0148fig_a1.eps} \end{figure}$ Figure A.1: The optical spectrum taken with EFOSC2 in November 2002 of the XBS J041108.1-71134. The weak ( EW=10-15 Å) emission line is tentatively identified with MgII $\lambda$ 2798 Å.

In the text

$\begin{figure} \par\includegraphics[width=13.8cm,clip]{0148fig_b1_a.ps} \par\end{figure}$ Figure B.1: The best-fit X-ray spectra of the extragalactic sources in the HBS28 sample (note that the sources XBS J021822.2-050615 and XBS J031859.2-441627 are not included since these spectra have been already presented and discussed in Severgnini et al. 2003).

In the text

$\begin{figure}\par\includegraphics[width=13.8cm,clip]{0148fig_b1_b.ps}\addtocounter{figure}{-1}\par\end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\includegraphics[width=13.8cm,clip]{0148fig_b1_c.ps}\addtocounter{figure}{-1}\end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\includegraphics[angle=-90,width=7cm,clip]{0148fig_b1_d.ps}\addtocounter{figure}{-1}\end{figure}$ Figure B.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0148fig1.eps} \end{figure}$	Figure 1: Red magnitude distribution of the 28 sources in the HBS28 sample. For most of the object (26) the magnitude is the APM red magnitude, while for the 2 faintest sources the R magnitude is considered.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0148fig2.eps} \end{figure}$	Figure 2: Redshift distribution of the 27 extragalactic sources in the HBS28 sample. The shaded area represents the type 2 objects asdefined in the text.
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{0148fig3.eps} \end{figure}$	Figure 3: The optical spectra of 10 newly discovered Broad Emission Lines AGNs ( ${\it FWHM}>2000$ km s^-1).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0148fig4.eps} \end{figure}$	Figure 4: The spectra of the 2 NLSy1 candidates discovered in the sample: XBS J023713.5-522734 ( top) and XBS J205829.9-423634 ( bottom). The two small boxes inside the two figures show the expanded region around the Fe II $\lambda$ 4600 Å hump.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0148fig5.eps} \end{figure}$	Figure 5: Top panel: the spectrum of the NEL AGN (a Seyfert 2) XBS J040758.9-712833. Bottom panel: The spectrum of the object XBS J193248.8-723355 optically classified as a Emission Line Galaxy (ELG, i.e. a starburst or a LINER, see text for details). As explained in the text, the X-ray analysis indicates the presence of an AGN in this object.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0148fig6.eps} \end{figure}$	Figure 6: The spectra of the two Sy1.9 discovered in the sample: XBS J040658.8-712457 ( top) and XBS J031146.1-550702 ( bottom).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0148fig7.eps} \end{figure}$	Figure 7: The hardness-ratio HR3 versus HR2. Filled circles represent the type 2 objects while the open circles are the type 1 objects.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0148fig8.eps} \end{figure}$	Figure 8: The X-ray photon-index distribution of the type 1objects obtained from the spectral fitting.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0148fig9.eps} \end{figure}$	Figure 9: The optical spectra of the 2 type 2 QSO discovered in the HBS28 sample: bottom panel: XBS J013240.1-133307, top panel: XBS J204043.4-004548.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0148fig10.eps} \end{figure}$	Figure 10: The distribution of the intrinsic $N_{\rm H}$ derived from the spectral fit, for type 1 objects and type 2 objects. The shaded histograms show the detections while the empty histograms represent the upper limits on $N_{\rm H}$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0148fig11.eps} \end{figure}$	Figure 11: The intrinsic $N_{\rm H}$ versus the unabsorbed X-ray luminosity in the 2-10 keV energy range for a) type 1 objects (open circles) and for b) the type 2 objects (filled circles).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0148fig12.eps} \end{figure}$	Figure 12: The ratio between the (observed) flux between 2 and 10 keV and the optical flux (see text for details) versus the observed 2-10 keV flux. The loci of constant R (Cousins) magnitudes are also plotted for R=16, 18, 20 and 22. Symbols are the same as in previous figure.
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