All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0004Fg1.ps} \end{figure}$ Figure 1: Sky distribution in Galactic coordinates of the selected observations. The high density of pointings in some areas of the sky correspond to planned surveys of relatively large sky areas (e.g. the XMM- Newton Large Scale Survey, Pierre et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0004Fg2.eps}\hspace*{0.8cm} \includegraphics[width=7.7cm,clip]{0004Fg3.eps} \end{figure}$ Figure 2: Left: distribution of Galactic hydrogen column density (in log units) along the line of sight taken from the 21 cm radio measurements of Dickey & Lockman (1990). Right: distribution of the exposure times (after filtering).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0004Fg4.eps}\hspace*{0.8cm} \includegraphics[width=7.9cm,clip]{0004Fg5.eps} \end{figure}$ Figure 3: Probability density distributions of the X-ray colour for sources detected in each energy band (i.e. with a detection likelihood in the band $\mathcal{L}$ $\ge$ 15). Left panel for bands <2 keV: the vertical line shows the hardness ratio which corresponds to a source with a spectral slope $\Gamma$ = 1.9 subject to the average Galactic absorption over the sample of objects ( $N_{\rm H}\sim 2$ $\times$ $10^{20}~{\rm cm}^{-2}$ ). Right panel for bands >2 keV: the vertical line shows the hardness ratio which corresponds to a source with a spectral slope $\Gamma$ = 1.6. The horizontal error bars show the change in X-ray colour for $\Delta \Gamma$ = $\pm$ 0.3.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0004Fg6.eps}\hspace*{0.8cm} \includegraphics[width=7.9cm,clip]{0004Fg7.eps} \hspace*{0.3cm} \end{figure}$ Figure 4: Distributions of the sky coverage as a function of X-ray flux for the different energy bands.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0004Fg8.eps}\hspace*{0.4cm... ...s}\hspace*{0.4cm} \includegraphics[width=8.4cm,clip]{0004Fg11.eps} \end{figure}$ Figure 5: Source count distributions in both a normalised differential ( left) and normalised integral form ( right) for sources detected in the 0.5-2 keV and 2-10 keV bands. The lines show the results of the fitting of the data using a model with two (solid) and three (dashed) power-laws (see Sect. 3.5). Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{0004Fg12.eps}\hspace*{0.5cm} \includegraphics[width=8cm,clip]{0004Fg13.eps} \end{figure}$ Figure 6: Comparison of the 0.5-2 keV ( left) and 2-10 keV ( right) normalised integral source count distributions (filled circles) with a set of representative results from previous surveys. Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0004Fg14.eps}\hspace*{0.5c... ...*{0.5cm} \includegraphics[angle=90,width=7.5cm,clip]{0004Fg21.eps} \end{figure}$ Figure 7: Source count distributions in both normalised differential ( left) and normalised integral form ( right) for sources detected in the 0.5-1 keV, 1-2 keV, 2-4.5 keV and 4.5-10 keV bands. The lines show the results of the fitting of the data using a model with two (solid) and three (dashed) power-laws (see Sect. 3.5). Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{0004Fg22.eps} \end{figure}$ Figure 8: Comparison of the measured normalised integral 4.5-10 keV source count distribution (filled circles) with a sample of representative results from previous surveys. Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{0004Fg23.ps}\vspace*{3mm} \par\includegraphics[angle=90,width=8cm,clip]{0004Fg24.eps} \end{figure}$ Figure 9: Top: dependence of the 4.5-10 keV normalised source count distribution in integral form on the exposure time of the observations. Bottom: comparison of our 4.5-10 keV normalised source count distribution in integral form ( $\mathcal{L}$ $\ge$ 15) with the distributions obtained if lower/higher detection likelihood thresholds are used instead. Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.4cm,clip]{0004Fg25.ps}\hspace*{2.5cm} \includegraphics[angle=-90,width=6.4cm,clip]{0004Fg26.ps} \end{figure}$ Figure 10: Distributions of the X-ray colour vs. flux for sources detected in our broad energy bands. The contours show the 90%, 75% and 50% level of peak intensity. Flux limits in the band are shown with a vertical solid line. The X-ray colour for a power-law spectral model with $\Gamma$ = 1.9 and different values of redshift and rest-frame absorption ( $N_{\rm H}$ in units of ${\rm 10^{22}~cm^{-2}}$ ) are represented with horizontal lines. The error bars at the top of the plots indicate the mean error in the X-ray colour at different fluxes.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{0004Fg27.eps}\hspac... ...ace*{0.8cm} \includegraphics[angle=90,width=8cm,clip]{0004Fg30.eps} \end{figure}$ Figure 11: Top: probability density distributions of the X-ray colour for sources detected in different energy bands. Bottom: cumulative distributions of the X-ray colour for sources detected in different energy bands. The vertical solid lines indicate the X-ray colour for an object at redshift z=0.7 with a power-law spectrum of photon index $\Gamma$ = 1.9 and different amounts of rest-frame absorption (in units of ${\rm 10^{22}~cm^{-2}}$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{0004Fg31N.eps} \end{figure}$ Figure 12: Normalised source count distribution in integral form for stars in the 0.5-2 keV band from two XMM- Newton serendipitous surveys at high galactic latitudes (|b| > 20 $^\circ$ ): the XMM- Newton Medium Sensitivity Survey ( XMS, circles) and the XMM- Newton bright survey ( XBS, squares). The dashed line shows the best fit to the 0.5-2 keV source count distribution for clusters from Rosati et al. (1998). Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0004Fg32.eps}\hsp... ...e*{0.3cm} \includegraphics[angle=90,width=8.3cm,clip]{0004Fg35.eps} \end{figure}$ Figure 13: Comparison of the normalised source count distributions in integral form in the 0.5-1 keV, 1-2 keV, 2-4.5 keV and 4.5-10 keV bands with the predictions from the synthesis models of the CXRB of Treister & Urry (2006) and Gilli et al. (2007): AGN only (solid lines), AGN+clusters+stars (dashed lines). Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0004Fg36.eps}\hspace*{0.7cm} \includegraphics[angle=90,width=8.3cm,clip]{0004Fg37.eps} \end{figure}$ Figure 14: Comparison of the normalised source count distributions in integral form in the 0.5-2 keV and 2-10 keV bands with the predictions from the synthesis models of the CXRB of Treister & Urry (2006) and Gilli et al. (2007): AGN only (solid lines), AGN+clusters+stars (dashed lines). Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{0004Fg38.ps}\hspac... ...pace*{2cm} \includegraphics[angle=-90,width=6cm,clip]{0004Fg43.ps} \end{figure}$ Figure A.1: Count rates given by the emldetect SAS task vs. pure Poissonian count rates (in units of cts s^-1). The best fit to the observed distributions is also shown with a dashed line. The contours show the 90%, 75% and 50% level of peak intensity.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0004Fg44.eps}\hsp... ...0.5cm} \includegraphics[angle=90,width=8.3cm,clip]{0004Fg45.eps} \end{figure}$ Figure A.2: Comparison of the normalised differential ( left and integral ( right) source count distributions for sources detected in the 0.5-2 keV band from our source detection (triangles) and for sources in the 2XMM catalogue (circles). The source parameters for 2XMM sources were obtained from the combination of parameters from the 2XMM energy bands 0.5-1 keV and 1-2 keV. Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0004Fg46.eps}\hsp... ...0.5cm} \includegraphics[angle=90,width=8.3cm,clip]{0004Fg47.eps} \end{figure}$ Figure A.3: Comparison of the normalised differential ( left) and integral ( right) source count distributions for sources detected in the 2-10 keV band from our source detection (triangles) and for sources from the 2XMM catalogue (circles). Source parameters for 2XMM sources were obtained from the combination of parameters from the 2XMM energy bands 2-4.5 keV and 4.5-12 keV. We also show for comparison the source count distribution in the 2-8 keV band obtained from our source detection (stars). Error bars correspond to 1 $\sigma$ confidence.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0004Fg1.ps} \end{figure}$	Figure 1: Sky distribution in Galactic coordinates of the selected observations. The high density of pointings in some areas of the sky correspond to planned surveys of relatively large sky areas (e.g. the XMM- Newton Large Scale Survey, Pierre et al. 2004).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0004Fg2.eps}\hspace*{0.8cm} \includegraphics[width=7.7cm,clip]{0004Fg3.eps} \end{figure}$	Figure 2: Left: distribution of Galactic hydrogen column density (in log units) along the line of sight taken from the 21 cm radio measurements of Dickey & Lockman (1990). Right: distribution of the exposure times (after filtering).
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0004Fg6.eps}\hspace{0.8cm} \includegraphics[width=7.9cm,clip]{0004Fg7.eps} \hspace{0.3cm} \end{figure}$	Figure 4: Distributions of the sky coverage as a function of X-ray flux for the different energy bands.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0004Fg8.eps}\hspace{0.4cm... ...s}\hspace{0.4cm} \includegraphics[width=8.4cm,clip]{0004Fg11.eps} \end{figure}$	Figure 5: Source count distributions in both a normalised differential ( left) and normalised integral form ( right) for sources detected in the 0.5-2 keV and 2-10 keV bands. The lines show the results of the fitting of the data using a model with two (solid) and three (dashed) power-laws (see Sect. 3.5). Error bars correspond to 1 $\sigma$ confidence.
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$\begin{figure} \par\includegraphics[width=8.25cm,clip]{0004Fg12.eps}\hspace*{0.5cm} \includegraphics[width=8cm,clip]{0004Fg13.eps} \end{figure}$	Figure 6: Comparison of the 0.5-2 keV ( left) and 2-10 keV ( right) normalised integral source count distributions (filled circles) with a set of representative results from previous surveys. Error bars correspond to 1 $\sigma$ confidence.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0004Fg14.eps}\hspace{0.5c... ...{0.5cm} \includegraphics[angle=90,width=7.5cm,clip]{0004Fg21.eps} \end{figure}$	Figure 7: Source count distributions in both normalised differential ( left) and normalised integral form ( right) for sources detected in the 0.5-1 keV, 1-2 keV, 2-4.5 keV and 4.5-10 keV bands. The lines show the results of the fitting of the data using a model with two (solid) and three (dashed) power-laws (see Sect. 3.5). Error bars correspond to 1 $\sigma$ confidence.
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$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{0004Fg22.eps} \end{figure}$	Figure 8: Comparison of the measured normalised integral 4.5-10 keV source count distribution (filled circles) with a sample of representative results from previous surveys. Error bars correspond to 1 $\sigma$ confidence.
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$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0004Fg32.eps}\hsp... ...e*{0.3cm} \includegraphics[angle=90,width=8.3cm,clip]{0004Fg35.eps} \end{figure}$	Figure 13: Comparison of the normalised source count distributions in integral form in the 0.5-1 keV, 1-2 keV, 2-4.5 keV and 4.5-10 keV bands with the predictions from the synthesis models of the CXRB of Treister & Urry (2006) and Gilli et al. (2007): AGN only (solid lines), AGN+clusters+stars (dashed lines). Error bars correspond to 1 $\sigma$ confidence.
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$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{0004Fg36.eps}\hspace*{0.7cm} \includegraphics[angle=90,width=8.3cm,clip]{0004Fg37.eps} \end{figure}$	Figure 14: Comparison of the normalised source count distributions in integral form in the 0.5-2 keV and 2-10 keV bands with the predictions from the synthesis models of the CXRB of Treister & Urry (2006) and Gilli et al. (2007): AGN only (solid lines), AGN+clusters+stars (dashed lines). Error bars correspond to 1 $\sigma$ confidence.
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$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{0004Fg38.ps}\hspac... ...pace*{2cm} \includegraphics[angle=-90,width=6cm,clip]{0004Fg43.ps} \end{figure}$	Figure A.1: Count rates given by the `emldetect` `SAS` task vs. pure Poissonian count rates (in units of cts s^-1). The best fit to the observed distributions is also shown with a dashed line. The contours show the 90%, 75% and 50% level of peak intensity.
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