All Figures

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4173F1.ps} \end{figure}$ Figure 1: H-R diagram of single giants (Gondoin 1999) compared with evolutionary tracks (Schaller et al. 1992). The dot-dashed lines from bottom to top describe the evolutionary tracks of 1 $M_\odot$ , 1.25 $M_\odot$ , 1.5 $M_\odot$ , 2 $M_\odot$ , 2.5 $M_\odot$ and 3 $M_\odot$ stars, respectively. The solid line is the evolutionary track of a 1.7 $M_\odot$ star. Open circles mark the H-R diagram positions of single field giants. Black circles mark giants known as X-ray sources. The H-R diagram location of HD 223460 is indicated by an error bar.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7cm,clip]{H4173F2.ps}\hspace*{6mm} \includegraphics[angle=270,width=7cm,clip]{H4173F3.ps} \end{figure}$ Figure 2: Light curves of HD 223460 during revolutions 107 (left) and 200 (right) obtained with the EPIC p-n camera. In each graph, the upper curve is the count rate within the 0.3 to 2 keV band and the lower curve is the count rate within the 2 to 10 keV band. The events are binned in 300 s time intervals and the background contribution has been subtracted.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{H4173F4.ps}\hspace*{2mm} \includegraphics[angle=270,width=8cm,clip]{H4173F5.ps} \end{figure}$ Figure 3: Best fit models to revolution 107 (left) and revolution 200 (right) EPIC spectra. The data (crosses) and spectral fit (solid line) to the EPIC pn (upper curve) and EPIC MOS (lower curve) spectra are shown in the upper panel. The $\chi ^{2}$ contributions are given in the lower panel of each graph.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4173F6.ps} \end{figure}$ Figure 4: Comparison of the EPIC pn spectrum of HD 223460 obtained during revolution 107 with a best fit power law + Gaussian model in the 3-9 keV range.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4173F7.ps} \end{figure}$ Figure 5: Comparison of the RGS spectra of HD 223460 obtained during revolution 107 with a best fit VMEKAL model with 3 temperature components (see Table 6, model C) in the 10-25 Å range. The data (crosses) and spectral fit to the RGS spectra are shown in the upper panel. The $\chi ^{2}$ contributions are given in the lower panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4173F8.ps}\par\vspace*{3mm} \includegraphics[width=8.8cm,clip]{H4173F9.ps} \end{figure}$ Figure 6: Averaged first order spectra of RGS 1 and 2 obtained during revolutions 107 (top) and 200 (bottom).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4173F10.ps} \end{figure}$ Figure 7: Equatorial rotational velocity of HD 223460 (filled circle) compared with $v \sin i$ values of single field giants (Gondoin 1999). The solid line and the dashed line describe the equatorial velocity evolution of 1.7 $M_\odot$ and 2.5 $M_\odot$ stars respectively assuming angular momentum conservation and $v \sin i = 150$ km s^-1 at $T_{\rm eff} = 7000$ K.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4173F11.ps} \end{figure}$ Figure 8: XMM-Newton luminosities of HD 223460 (filled circles) in the 0.3 to 2 keV band compared with ROSAT PSPC measurements of single field giants (Hünsch et al. 1998; Pizzolato et al. 2000). Upper limits of X-ray luminosities measured with the Einstein (Maggio et al. 1990) and ROSAT (Pizzolato et al. 2000) observatories are indicated by small triangles, large triangles and filled triangles for low-mass (1.2 $M_\odot < M < 2.0~M_\odot$ ), intermediate- mass (2.0 $M_\odot < M < 2.5$ $M_\odot$ ) and clump giants respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4173F12.ps} \end{figure}$ Figure 9: Ratio of the X-ray to bolometric luminosities of HD 223460 (filled circles) in the 0.3 to 2 keV band compared with single field giants (Hünsch et al. 1998; Gondoin 1999; Pizzolato et al. 2000).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7cm,clip]{H4173F2.ps}\hspace*{6mm} \includegraphics[angle=270,width=7cm,clip]{H4173F3.ps} \end{figure}$	Figure 2: Light curves of HD 223460 during revolutions 107 (left) and 200 (right) obtained with the EPIC p-n camera. In each graph, the upper curve is the count rate within the 0.3 to 2 keV band and the lower curve is the count rate within the 2 to 10 keV band. The events are binned in 300 s time intervals and the background contribution has been subtracted.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{H4173F4.ps}\hspace*{2mm} \includegraphics[angle=270,width=8cm,clip]{H4173F5.ps} \end{figure}$	Figure 3: Best fit models to revolution 107 (left) and revolution 200 (right) EPIC spectra. The data (crosses) and spectral fit (solid line) to the EPIC pn (upper curve) and EPIC MOS (lower curve) spectra are shown in the upper panel. The $\chi ^{2}$ contributions are given in the lower panel of each graph.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4173F6.ps} \end{figure}$	Figure 4: Comparison of the EPIC pn spectrum of HD 223460 obtained during revolution 107 with a best fit power law + Gaussian model in the 3-9 keV range.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4173F7.ps} \end{figure}$	Figure 5: Comparison of the RGS spectra of HD 223460 obtained during revolution 107 with a best fit VMEKAL model with 3 temperature components (see Table 6, model C) in the 10-25 Å range. The data (crosses) and spectral fit to the RGS spectra are shown in the upper panel. The $\chi ^{2}$ contributions are given in the lower panel.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4173F8.ps}\par\vspace*{3mm} \includegraphics[width=8.8cm,clip]{H4173F9.ps} \end{figure}$	Figure 6: Averaged first order spectra of RGS 1 and 2 obtained during revolutions 107 (top) and 200 (bottom).
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4173F10.ps} \end{figure}$	Figure 7: Equatorial rotational velocity of HD 223460 (filled circle) compared with $v \sin i$ values of single field giants (Gondoin 1999). The solid line and the dashed line describe the equatorial velocity evolution of 1.7 $M_\odot$ and 2.5 $M_\odot$ stars respectively assuming angular momentum conservation and $v \sin i = 150$ km s^-1 at $T_{\rm eff} = 7000$ K.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4173F12.ps} \end{figure}$	Figure 9: Ratio of the X-ray to bolometric luminosities of HD 223460 (filled circles) in the 0.3 to 2 keV band compared with single field giants (Hünsch et al. 1998; Gondoin 1999; Pizzolato et al. 2000).
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