All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_1.ps}\end{figure}$ Figure 1: Averaged mos1 and mos2 exposure map (0.5-2.0 keV) of the $4 \times 4$ pointing pattern (small white crosses). The exposure time in the central region reaches 78 ks. The black rectangle shows the area covered by the WFI R-band images. The white polygon marks the area covered by the SOFI K-band images (see Sect. 2.2).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_2.ps} \end{figure}$ Figure 2: PN exposure map (0.5-2.0 keV) of the $4 \times 4$ pointing pattern. The exposure time in the central region reaches 35.5 ks. The area inside the black contour markes the "core sample'' region where the pn-detector exposure time exceeds six ks. White rectangles show the position of the spectroscopic masks for the optical follow-up observations (see Sect. 2.4).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_3.ps} \end{figure}$ Figure 3: 0.2-10 keV X-ray flux histogram of the 328 XMM-Newton detected X-ray sources in the Marano Field. Up to an X-ray flux of $f_{\rm {X}}\sim 5 \times 10^{-15}$ erg cm^-2 s^-1 (turnover flux) we detect more and more sources. Below that X-ray flux the detection rate decreases dramactically.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5849_4.ps} \end{figure}$ Figure 4: Comparison between the 0.5-2 keV X-ray fluxes measured by ROSAT and XMM-Newton of all 50 ROSAT X-ray sources in the Marano Field. XMM-Newton fluxes are averages of the three individual EPIC camera fluxes. The black solid line represents equal ROSAT and XMM-Newton fluxes.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5849_5.ps} \end{figure}$ Figure 5: Magnitude histogram of the sources detected in the WFI R-band image. Completeness in detecting objects is lost for R>23.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_6.ps} \end{figure}$ Figure 6: Histogram of the K-band magnitudes in the NTT-SOFI images. Completeness in detecting objects is lost for K>20.5.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.9cm,clip]{5849_7.ps} \end{figure}$ Figure 7: Optical atmospheric absorption corrected, wavelength and flux calibrated spectrum for X-ray source 480. The black spectrum marks the object's spectrum. The green line (see the online colour version of the manuscript) shows the error spectrum. Possible emission and absorption features in the spectrum are labelled. The spectral feature at 5580 Å is spurious due to incomplete substraction of a night sky line.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{5849_8.ps} \end{figure}$ Figure 8: Adopted mean k correction from observed R-band to rest-frame $M_{\rm {B}}$ , for broad emission line AGN.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.2cm,clip]{5849_9.ps} \end{figure}$ Figure 9: Adopted conversion term to estimate AB magnitudes at fixed rest-frame wavelength $\lambda = 2500$ Å from observed R-band magnitudes.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5849_10.ps} \end{figure}$ Figure 10: a) Number of objects identified as X-ray counterparts vs. difference in X-ray and optical position scaled to a 1 $\sigma _{\rm {X}}$ position error with a systematic X-ray position error of 2 arcsec. The smooth line represents the theoretical distribution. The distribution of type I AGN, which are a class of well-accepted X-ray emitters, is plotted as a dotted line. The solid line characterises the complete sample including type I AGN, type II AGN, galaxies, and stars. b) The 1 $\sigma _{\rm {X}}$ position error was adjusted to the observed distribution by reducing the systematic X-ray position error from $2\hbox {$^{\prime \prime }$ }$ to $0.7\hbox {$^{\prime \prime }$ }$ . The complete sample agrees well with the type I AGN distribution, which gives evidence of a marginally false match rate.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_11.ps} \end{figure}$ Figure 11: WFI R-band magnitude vs. difference in X-ray and optical position scaled to a $1\sigma _{\rm {X}}$ position error with a systematic X-ray position error of 0.7 arcsec. Crosses mark type I AGN, asterisks type II AGN, triangle galaxies, and rectangles stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_12.ps} \end{figure}$ Figure 12: WFI R-band magnitude histogram for the core sample in the XMM-Newton Marano Field survey. The solid line represents the R-magnitude distribution of the spectroscopically classified X-ray counterparts. The dashed line shows the distribution of the optically identified but not spectroscopically classified X-ray counterparts. Six X-ray sources, which have no counterpart within a 3 $\sigma _{\rm {X}}$ error circle, are assigned to the bin at R=25.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_13.ps} \end{figure}$ Figure 13: Likelihood vs. 0.2-10 keV X-ray-flux of the 252 central X-ray sources (pn-detector exposure time $\ge$ 6 ks). Crosses mark type I AGN, asterisks type II AGN, triangle galaxies, and rectangles stars. Dots indicate X-ray sources with no spectroscopic classification. The vertical line indicates ML = 10.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_14.ps} \end{figure}$ Figure 14: X-ray diagnostic diagram based on hardness ratios. HR2 is calculated by using the 0.5-2.0 keV and 2.0-4.5 keV band, HR3 2.0-4.5 keV and 4.5-7.5 keV. Only X-ray sources that have $\sigma _{\rm {HR2}} < 0.3$ are plotted. Labels: crosses - 63 type I AGN, asterisks - 24 type II AGN, triangles - 4 galaxies, and open circles - 24 unidentified X-ray sources with ML > 10. Large symbols represent objects with $\sigma _{\rm {HR3}} < 0.3$ , small symbols $\sigma _{\rm {HR3}} \ge 0.3$ . The solid line with box symbols (at $HR2\sim HR3\sim -0.5$ ) represents an unabsorbed power-law X-ray spectrum (corrected for galactic absorption) with different photon index $\Gamma =2.4{-}1.2$ in steps of 0.2 (squares). Different hydrogen column densities ( $N_{\rm {H}}$ /cm $^{-2}= 10^{20},10^{22},3\times 10^{22},10^{23},3\times 10^{23},10^{24}$ ; see Sect. 4.4) are plotted as a solid line with diamonds for $\Gamma =2$ and z=1.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_15.ps} \end{figure}$ Figure 15: Redshift distribution of AGN in the Marano Field. a) Complete sample of 64 optically selected quasars ( $B_{{\rm J}} \leq 22.0$ ) by Zitelli et al. (1992); b) ROSAT X-ray sources (29 type I AGN by Zamorani et al. 1999); c) 35 type I AGN newly detected by XMM-Newton (core region); d) redshift distribution of the core sample: dotted line: all 70 XMM-Newton detected type I AGN, solid line: 31 XMM-Newton detected type II AGN, and dashed line: 5 XMM-Newton detected optically normal galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_16.ps} \end{figure}$ Figure 16: Observed X-ray luminosity (0.2-10 keV) vs. redshift. Labels: crosses - 70 type I AGN, asterisks - 30 type II AGN, and triangles - 5 galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_17.ps} \end{figure}$ Figure 17: Observed X-ray luminosity (0.2-10 keV) vs. hardness ratio. HR2 is calculated by using 0.5-2.0 keV & 2.0-4.5 keV bands. Only X-ray sources that have $\sigma _{\rm {HR2}} < 0.3$ are plotted. Labels: crosses - 63 type I AGN, asterisks - 24 type II AGN (grey marked have $z \ge 2.0$ ), and triangles - 4 galaxies. The diagram separation into different regions is based on Szokoly (2004) with an adjusted threshold in the HR2-value.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5849_18.ps} \end{figure}$ Figure 18: Calculated intrinsic hydrogen column density histogram for the central Marano Field. The solid line shows the distribution of type II AGN that have reasonable fits in hydrogen column density. Objects with $N_{\rm {H}}=0$ are set to $N_{\rm{H}}=5 \times 10^{19}~{\rm cm^{-2}}$ . The dotted line represents only type II AGN that show intrinsic absorption with a significance higher than $2 \sigma$ in hydrogen column density. Optically normal galaxies are plotted as a dashed line. Dotted line - 14 type I AGN; solid line - 30 type II AGN; dashed line - 5 galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_19.ps} \end{figure}$ Figure 19: a) Histogram of the absorbed (observed) X-ray luminosity (0.2-10 keV) for the core sample. Dotted line - 70 type I AGN, solid line - 30 type II AGN, and dashed line - 5 galaxies. b) Histogram of the X-ray luminosity (0.2-10 keV) corrected for intrinsic absorption (core sample). Same notation as in a). c) Corrected X-ray luminosity (0.2-10 keV) vs. hydrogen column density (core sample). Crosses - type I AGN, asterisks - type II AGN, and triangles - galaxies. The upper right corner is suggested as being defined as the "type II QSO region'' by Mainieri et al. (2002). Objects with $N_{\rm {H}}=0$ are set to $N_{\rm{H}}=5 \times 10^{19}~{\rm cm^{-2}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_20.ps} \end{figure}$ Figure 20: Observed X-ray flux (0.2-10 keV) vs. R-band magnitude. Dashed lines indicate the $f_{\rm {X}}/f_{\rm {opt}}$ values 0.1, 1.0, and 10. Labels: crosses - 63 type I AGN, asterisks - 25 type II AGN, triangles - 5 galaxies, rectangles - 3 stars, and circles - 21 spectroscopically unidentified sources (R-band lower limits are plotted as circles at R=24). Note that for a few objects of the core sample no WFI R-magnitudes were available and therefore these are not plotted here.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_21.ps} \end{figure}$ Figure 21: Colour magnitude diagram of spectroscopically classified X-ray sources. Labels: crosses - 56 type I AGN, asterisks - 20 type II AGN, and triangles - 4 galaxies. Only objects with detections in both R and K are included. The absence of blue, faint objects (below the solid line) is due only to the K-magnitude limit.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_22.ps} \end{figure}$ Figure 22: Redshift distribution of the additional objects. Labels: solid line - 37 NELGs, and dotted line - 8 optically normal galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_23.ps}\end{figure}$ Figure 23: UV to X-ray spectral index $\alpha _{\rm OX}$ vs. redshift for type I AGN in the core sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_24.ps}\par\end{figure}$ Figure 24: UV to X-ray spectral index $\alpha _{\rm OX}$ vs. optical luminosity density at $2500 ~\AA$ for type I AGN in the core sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_25.ps}\end{figure}$ Figure 25: Observed 0.2-10 keV X-ray luminosity vs. optical luminosity density at $2500 ~\AA$ for type I AGN in the core sample (crosses). The solid line indicates the best-fit linear regression with a slope $\beta =0.84$ . The dotted line with slope $\beta =1$ marks a linear $L_{\rm X} - l_{\rm opt}$ relation.
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In the text

$\begin{figure}\par\includegraphics[width=9cm,clip]{11.eps}\end{figure}$

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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_1.ps}\end{figure}$	Figure 1: Averaged mos1 and mos2 exposure map (0.5-2.0 keV) of the $4 \times 4$ pointing pattern (small white crosses). The exposure time in the central region reaches 78 ks. The black rectangle shows the area covered by the WFI R-band images. The white polygon marks the area covered by the SOFI K-band images (see Sect. 2.2).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_2.ps} \end{figure}$	Figure 2: PN exposure map (0.5-2.0 keV) of the $4 \times 4$ pointing pattern. The exposure time in the central region reaches 35.5 ks. The area inside the black contour markes the "core sample'' region where the pn-detector exposure time exceeds six ks. White rectangles show the position of the spectroscopic masks for the optical follow-up observations (see Sect. 2.4).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_3.ps} \end{figure}$	Figure 3: 0.2-10 keV X-ray flux histogram of the 328 XMM-Newton detected X-ray sources in the Marano Field. Up to an X-ray flux of $f_{\rm {X}}\sim 5 \times 10^{-15}$ erg cm^-2 s^-1 (turnover flux) we detect more and more sources. Below that X-ray flux the detection rate decreases dramactically.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5849_4.ps} \end{figure}$	Figure 4: Comparison between the 0.5-2 keV X-ray fluxes measured by ROSAT and XMM-Newton of all 50 ROSAT X-ray sources in the Marano Field. XMM-Newton fluxes are averages of the three individual EPIC camera fluxes. The black solid line represents equal ROSAT and XMM-Newton fluxes.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5849_5.ps} \end{figure}$	Figure 5: Magnitude histogram of the sources detected in the WFI R-band image. Completeness in detecting objects is lost for R>23.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_6.ps} \end{figure}$	Figure 6: Histogram of the K-band magnitudes in the NTT-SOFI images. Completeness in detecting objects is lost for K>20.5.
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$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{5849_8.ps} \end{figure}$	Figure 8: Adopted mean k correction from observed R-band to rest-frame $M_{\rm {B}}$ , for broad emission line AGN.
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$\begin{figure} \par\includegraphics[angle=270,width=8.2cm,clip]{5849_9.ps} \end{figure}$	Figure 9: Adopted conversion term to estimate AB magnitudes at fixed rest-frame wavelength $\lambda = 2500$ Å from observed R-band magnitudes.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_11.ps} \end{figure}$	Figure 11: WFI R-band magnitude vs. difference in X-ray and optical position scaled to a $1\sigma _{\rm {X}}$ position error with a systematic X-ray position error of 0.7 arcsec. Crosses mark type I AGN, asterisks type II AGN, triangle galaxies, and rectangles stars.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_13.ps} \end{figure}$	Figure 13: Likelihood vs. 0.2-10 keV X-ray-flux of the 252 central X-ray sources (pn-detector exposure time $\ge$ 6 ks). Crosses mark type I AGN, asterisks type II AGN, triangle galaxies, and rectangles stars. Dots indicate X-ray sources with no spectroscopic classification. The vertical line indicates ML = 10.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_16.ps} \end{figure}$	Figure 16: Observed X-ray luminosity (0.2-10 keV) vs. redshift. Labels: crosses - 70 type I AGN, asterisks - 30 type II AGN, and triangles - 5 galaxies.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_21.ps} \end{figure}$	Figure 21: Colour magnitude diagram of spectroscopically classified X-ray sources. Labels: crosses - 56 type I AGN, asterisks - 20 type II AGN, and triangles - 4 galaxies. Only objects with detections in both R and K are included. The absence of blue, faint objects (below the solid line) is due only to the K-magnitude limit.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_22.ps} \end{figure}$	Figure 22: Redshift distribution of the additional objects. Labels: solid line - 37 NELGs, and dotted line - 8 optically normal galaxies.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5849_23.ps}\end{figure}$	Figure 23: UV to X-ray spectral index $\alpha _{\rm OX}$ vs. redshift for type I AGN in the core sample.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_24.ps}\par\end{figure}$	Figure 24: UV to X-ray spectral index $\alpha _{\rm OX}$ vs. optical luminosity density at $2500 ~\AA$ for type I AGN in the core sample.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{5849_25.ps}\end{figure}$	Figure 25: Observed 0.2-10 keV X-ray luminosity vs. optical luminosity density at $2500 ~\AA$ for type I AGN in the core sample (crosses). The solid line indicates the best-fit linear regression with a slope $\beta =0.84$ . The dotted line with slope $\beta =1$ marks a linear $L_{\rm X} - l_{\rm opt}$ relation.
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