All Figures

$\begin{figure} \par\resizebox{16cm}{!}{\includegraphics[]{1990f1.ps}} \end{figure}$ Figure 1: Logarithmically-scaled XMM-Newton EPIC low background image with a pixel size of 1 arcsec²of the M 31 centre observations combining PN and MOS1 and MOS2 cameras in the (0.2-4.5) keV XID band. The data are smoothed with a Gaussian of FWHM 5 $^{\prime \prime }$ which corresponds to the point spread function in the centre area of the combined observations. The image is corrected for un-vignetted exposure and masked for exposures above 5 ks for the individual cameras. Contours are at $(1, 2, 4, 8, 16, 32)\times 10^{-6}$ ct s^-1 pix^-1 including a factor of two smoothing. Sources from the catalogue are marked in the outer area. The inner area is shown in detail in Fig. 2.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[]{1990f2a.ps}\includegraphics[]{1990f2b.ps}} \end{figure}$ Figure 2: Inner area of Fig. 1. Contours are at $(1, 2, 4, 8, 16, 32, 64, 128, 256)\times 10^{-6}$ ct s^-1 pix^-1. Left: sources from the XMM-Newton catalogue are marked as $30\hbox {$^{\prime \prime }$ }\times 30\hbox {$^{\prime \prime }$ }$ squares. Right: sources from the Chandra analysis of Kong et al. (2002b) and Williams et al. (2004a) are marked.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[]{1990f3a.ps}\hskip0.2cm... ...udegraphics[]{1990f3c.ps}\hskip0.2cm\includegraphics[]{1990f3d.ps}} \end{figure}$ Figure 3: XMM-Newton EPIC M 31 images in the (0.2-4.5) keV XID band: North 3 ( upper left), North 2 ( upper right), North 1 ( lower left), and Halo 4 ( lower right).
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[]{1990f3e.ps}\hskip0.2cm\includegraphics[]{1990f3f.ps}}\addtocounter{figure}{-1} \end{figure}$ Figure 3: continued. XMM-Newton EPIC M 31 images in the (0.2-4.5) keV XID band: South 1 ( left) and South 2 ( right). The images are integrated in 2 $^{\prime \prime }$ pixels and smoothed with a Gaussian of FWHM 10 $^{\prime \prime }$ , corrected for un-vignetted exposure and masked for exposures above 5 ks for the individual cameras. Contour levels are $(4, 8, 16, 32, 64, 128)\times 10^{-6}$ ct s^-1 pix^-1 including a factor of two smoothing. Sources from the catalogue are indicated.
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In the text

$\begin{figure} \par\resizebox{10cm}{!}{\includegraphics[]{1990f4.ps}} \end{figure}$ Figure 4: Logarithmically-scaled, three-colour XMM-Newton EPIC low background image of the M 31 medium and thin filter observations combining PN and MOS1 and MOS2 cameras. Red, green and blue show respectively the (0.2-1.0) keV, (1.0-2.0) keV and (2.0-12.0) keV bands. The data in each energy band have been smoothed with a Gaussian of FWHM 20 $^{\prime \prime }$ to use an average point spread function for the different off-axis angles. The camera images have been corrected for un-vignetted exposure and masked for exposure above 5 ks. The image scale and the optical D₂₅ ellipse of M 31 are marked. Shown in detail to the upper right is a factor three zoom-in to the bulge area using images binned to 1 $^{\prime \prime }$ and smoothed with a Gaussian FWHM 5 $^{\prime \prime }$ corresponding to the point-spread-function (PSF) in the center of the field-of-view.
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In the text

$\begin{figure} \par\resizebox{8.1cm}{!}{\includegraphics[bb=50 90 355 460,angle=... ...}{!}{\includegraphics[bb=50 90 355 460,angle=-90,clip]{1990f5c.ps}} \end{figure}$ Figure 5: Hardness ratios of sources detected by XMM-Newton EPIC. Shown as dots are only sources with HR errors smaller than 0.20 on both HR(i) and HR(i+1). Foreground stars and candidate are marked as big and small stars, AGN and candidates as big and small crosses, SSS candidates as triangles, SNR and candidates as big and small hexagons, GlCs and XRBs and candidates as big and small squares. In addition, we mark positions derived from measured XMM-Newton EPIC spectra and models for SSSs (S1 to S4) as filled triangles, low mass XRBs (L1 and L2) as filled squares, SNRs (N132D as N1, 1E 0102.2-7219 as N2, N157B as N3, Crab spectra as C1 and C2) as filled hexagons, AGN (A1 and A2) as asterisk.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[]{1990f2a.ps}\includegraphics[]{1990f2b.ps}} \end{figure}$	Figure 2: Inner area of Fig. 1. Contours are at $(1, 2, 4, 8, 16, 32, 64, 128, 256)\times 10^{-6}$ ct s^-1 pix^-1. Left: sources from the XMM-Newton catalogue are marked as $30\hbox {$^{\prime \prime }$ }\times 30\hbox {$^{\prime \prime }$ }$ squares. Right: sources from the Chandra analysis of Kong et al. (2002b) and Williams et al. (2004a) are marked.
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$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[]{1990f3a.ps}\hskip0.2cm... ...udegraphics[]{1990f3c.ps}\hskip0.2cm\includegraphics[]{1990f3d.ps}} \end{figure}$	Figure 3: XMM-Newton EPIC M 31 images in the (0.2-4.5) keV XID band: North 3 ( upper left), North 2 ( upper right), North 1 ( lower left), and Halo 4 ( lower right).
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