All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{0168fg01.ps}\par... ...g02.ps}\par\includegraphics[angle=-90,width=7.4cm,clip]{0168fg03.ps}\end{figure}$ Figure 1: Top panel: redshift distribution. Central panel: counts distribution in the total band (0.2-12.0 keV). Bottom panel: flux distribution in the standard hard band (2.0-10.0 keV).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{0168fg04.ps}\end{figure}$ Figure 2: Averaged spectrum along with the power law fit.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{0168fg05.ps}\par\includegraphics[angle=-90,width=7.4cm,clip]{0168fg06.ps}\end{figure}$ Figure 3: Top panel: averaged spectrum (error bars) along with the simulated continuum (open circles). Dotted and dashed lines represent the 1 $\sigma$ and 2 $\sigma$ continuum confidence limits, respectively. Bottom panel: averaged spectrum to simulated continuum ratio and confidence limits.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.1cm,clip]{0168fg07.ps}\end{figure}$ Figure 4: Spectral fit corresponding to: baseline model + pexrav.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.1cm,clip]{0168fg08.ps}\par... ...g09.ps}\par\includegraphics[angle=-90,width=7.1cm,clip]{0168fg10.ps}\end{figure}$ Figure 5: Soft (0.5-2.0 keV) Luminosity samples. Top panel: averaged spectrum with Gaussian fit for the low luminosity sample. Central panel: medium luminosity sample. Bottom panel: high luminosity sample.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{0168fg11.ps}\end{figure}$ Figure A.1: Model: po. Simulated average spectrum corresponding to 10 simulated spectrum for each real spectrum and a simple power law model, $\Gamma$ = 1.9.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg12.ps}\end{figure}$ Figure A.2: Model: pha*po. Simulated average spectrum corresponding to 10 simulated spectrum for each real spectrum and a power law ( $\Gamma$ = 1.9) plus Galactic absorption model.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{0168fg13.ps}\par\includegraphics[angle=-90,width=7.25cm,clip]{0168fg14.ps}\end{figure}$ Figure A.3: Top panel: effective area corresponding to an individual observation for pn (solid line) and MOS cameras (dashed line). Bottom panel: pha*po models for different amounts of absorption: no absorption (solid line), 10²⁰ cm^-2 (dashed line), 10²¹ cm^-2 (dash-dotted line), 10²² cm^-2 (dotted line), 10²³ cm^-2 (dash-dot-dot-dotted line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg15.ps}\end{figure}$ Figure A.4: Model: pha*zpha*po. Simulated average spectrum corresponding to 10 simulated spectrum for each real spectrum and a power law ( $\Gamma$ = 1.9) plus Galactic absorption and intrinsic absorption model.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{0168fg16.ps}\end{figure}$ Figure A.5: Model: po+gaus: simulations without noise corresponding to E=6.4 keV, $\sigma$ = 0 and EW = 200 eV, rest-frame values.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg17.ps}\par... ...g18.ps}\par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg19.ps}\end{figure}$ Figure A.6: Top panel: model: pha*zpha*(po+gaus): simulated average spectrum corresponding to 10 simulated spectra for each real spectrum (squares) and the ``best-fit model'' continuum (circles). Central panel: simulations pha*zpha*(po+gaus) to power law ratio. Bottom panel: simulations pha*zpha*(po+gaus) to ``best-fit model'' continuum ratio.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg20.ps}\end{figure}$ Figure A.7: Average continuum with 100 simulations (circles) along with the power law fit (2-10 keV) and the 1 $\sigma$ (dotted line) and 2 $\sigma$ (dashed line) confidence limits.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{0168fg01.ps}\par... ...g02.ps}\par\includegraphics[angle=-90,width=7.4cm,clip]{0168fg03.ps}\end{figure}$	Figure 1: Top panel: redshift distribution. Central panel: counts distribution in the total band (0.2-12.0 keV). Bottom panel: flux distribution in the standard hard band (2.0-10.0 keV).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{0168fg04.ps}\end{figure}$	Figure 2: Averaged spectrum along with the power law fit.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{0168fg05.ps}\par\includegraphics[angle=-90,width=7.4cm,clip]{0168fg06.ps}\end{figure}$	Figure 3: Top panel: averaged spectrum (error bars) along with the simulated continuum (open circles). Dotted and dashed lines represent the 1 $\sigma$ and 2 $\sigma$ continuum confidence limits, respectively. Bottom panel: averaged spectrum to simulated continuum ratio and confidence limits.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.1cm,clip]{0168fg07.ps}\end{figure}$	Figure 4: Spectral fit corresponding to: baseline model + pexrav.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.1cm,clip]{0168fg08.ps}\par... ...g09.ps}\par\includegraphics[angle=-90,width=7.1cm,clip]{0168fg10.ps}\end{figure}$	Figure 5: Soft (0.5-2.0 keV) Luminosity samples. Top panel: averaged spectrum with Gaussian fit for the low luminosity sample. Central panel: medium luminosity sample. Bottom panel: high luminosity sample.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{0168fg11.ps}\end{figure}$	Figure A.1: Model: po. Simulated average spectrum corresponding to 10 simulated spectrum for each real spectrum and a simple power law model, $\Gamma$ = 1.9.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg12.ps}\end{figure}$	Figure A.2: *Model: phapo.** Simulated average spectrum corresponding to 10 simulated spectrum for each real spectrum and a power law ( $\Gamma$ = 1.9) plus Galactic absorption model.
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$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{0168fg13.ps}\par\includegraphics[angle=-90,width=7.25cm,clip]{0168fg14.ps}\end{figure}$	Figure A.3: Top panel: effective area corresponding to an individual observation for pn (solid line) and MOS cameras (dashed line). Bottom panel: pha*po models for different amounts of absorption: no absorption (solid line), 10²⁰ cm^-2 (dashed line), 10²¹ cm^-2 (dash-dotted line), 10²² cm^-2 (dotted line), 10²³ cm^-2 (dash-dot-dot-dotted line).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg15.ps}\end{figure}$	Figure A.4: *Model: phazphapo.* Simulated average spectrum corresponding to 10 simulated spectrum for each real spectrum and a power law ( $\Gamma$ = 1.9) plus Galactic absorption and intrinsic absorption model.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{0168fg16.ps}\end{figure}$	Figure A.5: Model: po+gaus: simulations without noise corresponding to E=6.4 keV, $\sigma$ = 0 and EW = 200 eV, rest-frame values.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg17.ps}\par... ...g18.ps}\par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg19.ps}\end{figure}$	Figure A.6: Top panel: *model: phazpha(po+gaus): simulated average spectrum corresponding to 10 simulated spectra for each real spectrum (squares) and the ``best-fit model'' continuum (circles). Central panel: simulations phazpha(po+gaus) to power law ratio. Bottom panel: simulations phazpha*(po+gaus) to ``best-fit model'' continuum ratio.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{0168fg20.ps}\end{figure}$	Figure A.7: Average continuum with 100 simulations (circles) along with the power law fit (2-10 keV) and the 1 $\sigma$ (dotted line) and 2 $\sigma$ (dashed line) confidence limits.
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