$\begin{figure} \par\includegraphics[width=8.5cm,clip]{Gi131_f1.eps}\end{figure}$ Figure 1: HST/WFC2 image of the ESO509-IG066 field in the F606W filter. The circles represent the EPIC/XMM-Newton sources error boxes.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{Gi131_f2.eps} \end{figure}$ Figure 2: EPIC combined image of the innermost 1 $\hbox {$^\prime $ }$ around the ESO509-IG066 galaxy pair centroid in the 0.2-2 keV ( left panel) and 2-15 keV ( right panel) energy bands. A constant level of 2 counts per pixel has been subtracted.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{Gi131_f3.eps} \includegraphics[angle=-90,width=8cm,clip]{Gi131_f4.eps} \end{figure}$ Figure 3: Spectra ( upper panels) and residuals in units of standard deviations ( lower panels) when the best-fit model is applied to the pn and MOS spectra of source #1 ( top) and #2 ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{Gi131_f1.eps}\end{figure}$	Figure 1: HST/WFC2 image of the ESO509-IG066 field in the F606W filter. The circles represent the EPIC/XMM-Newton sources error boxes.
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$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{Gi131_f2.eps} \end{figure}$	Figure 2: EPIC combined image of the innermost 1 $\hbox {$^\prime $ }$ around the ESO509-IG066 galaxy pair centroid in the 0.2-2 keV ( left panel) and 2-15 keV ( right panel) energy bands. A constant level of 2 counts per pixel has been subtracted.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{Gi131_f3.eps} \includegraphics[angle=-90,width=8cm,clip]{Gi131_f4.eps} \end{figure}$	Figure 3: Spectra ( upper panels) and residuals in units of standard deviations ( lower panels) when the best-fit model is applied to the pn and MOS spectra of source #1 ( top) and #2 ( bottom).
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