All Figures

$\begin{figure} \par\includegraphics[width=17cm,clip]{2162fig1.ps} \end{figure}$ Figure 1: Optical image of NGC 300 in the visible band overlaid by a contour map of the merged 0.3-6.0 keV raw X-ray image from all three EPIC cameras and from both orbits. The D₂₅ optical disk and the sources detected inside the disk are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{2162fig2.ps} \end{figure}$ Figure 2: Color-color diagram of sources detected inside the D₂₅ optical disk.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2162fig3.ps} \end{figure}$ Figure 3: Color-color diagram of the sources detected inside the D₂₅ optical disk and color-color contours for bremsstrahlung and 0.2 keV bremsstrahlung plus power law component. The equivalent hydrogen column, $N_{\rm H}$ , is given in units of $10^{22}~{\rm cm}^{-2}$ , the temperature of the bremsstrahlung spectrum, kT, is given in keV.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2162fig4.ps} \end{figure}$ Figure 4: Fluxes of the sources detected inside the D₂₅ optical disk as a function of the harder ( top) and softer ( bottom) hardness ratio defined by Eq. (2).
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In the text

$\begin{figure} \par\includegraphics[width=8.55cm,clip]{2162fig5.ps} \end{figure}$ Figure 5: ${\rm log}~ N$ - $\log S$ diagram of all sources with more than 20 net counts inside the optical D₂₅ disk (solid line), of soft sources with ${\rm HR}_{\rm soft} \leq -0.2$ (dotted line), and for sources harder than that (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,height=7.8cm,angle=-90,clip]{2162fig6.ps} \end{figure}$ Figure 6: Top: EPIC pn and MOS spectra of the central diffuse emission region and the best fit spectral model, consisting of the sum of an APEC model, and a bremsstrahlung component, bottom: residuals expressed in $\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2162fig7.ps} \end{figure}$ Figure 7: Smoothed 0.3-1.3 keV X-ray image of the central region of NGC 300 after removal of detected sources. The circle and annulus show the region for the central diffuse emission area and the associated background, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{2162fig8.ps} \includegraphics[width=11cm,clip]{2162fig9.ps} \end{figure}$ Figure 8: $7.4''\times 7.4''$ optical images of the region centered on the corrected position of the 32 brightest X-ray sources inside the D₂₅ optical disk. The circle indicates the 68% positional error of the X-ray coordinates, the thicker circles show the optical sources found within the X-ray error circle. Catalog sources having a distance of less than 5'' from the X-ray position are shown with a box.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{2162fig1.ps} \end{figure}$	Figure 1: Optical image of NGC 300 in the visible band overlaid by a contour map of the merged 0.3-6.0 keV raw X-ray image from all three EPIC cameras and from both orbits. The D₂₅ optical disk and the sources detected inside the disk are also shown.
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$\begin{figure} \par\includegraphics[width=8.35cm,clip]{2162fig2.ps} \end{figure}$	Figure 2: Color-color diagram of sources detected inside the D₂₅ optical disk.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2162fig3.ps} \end{figure}$	Figure 3: Color-color diagram of the sources detected inside the D₂₅ optical disk and color-color contours for bremsstrahlung and 0.2 keV bremsstrahlung plus power law component. The equivalent hydrogen column, $N_{\rm H}$ , is given in units of $10^{22}~{\rm cm}^{-2}$ , the temperature of the bremsstrahlung spectrum, kT, is given in keV.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2162fig4.ps} \end{figure}$	Figure 4: Fluxes of the sources detected inside the D₂₅ optical disk as a function of the harder ( top) and softer ( bottom) hardness ratio defined by Eq. (2).
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$\begin{figure} \par\includegraphics[width=8.55cm,clip]{2162fig5.ps} \end{figure}$	Figure 5: ${\rm log}~ N$ - $\log S$ diagram of all sources with more than 20 net counts inside the optical D₂₅ disk (solid line), of soft sources with ${\rm HR}_{\rm soft} \leq -0.2$ (dotted line), and for sources harder than that (dashed line).
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$\begin{figure} \par\includegraphics[width=8.8cm,height=7.8cm,angle=-90,clip]{2162fig6.ps} \end{figure}$	Figure 6: Top: EPIC pn and MOS spectra of the central diffuse emission region and the best fit spectral model, consisting of the sum of an APEC model, and a bremsstrahlung component, bottom: residuals expressed in $\sigma$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2162fig7.ps} \end{figure}$	Figure 7: Smoothed 0.3-1.3 keV X-ray image of the central region of NGC 300 after removal of detected sources. The circle and annulus show the region for the central diffuse emission area and the associated background, respectively.
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