$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7016fig2.ps}\end{figure}$ Figure 2: RGS1 spectrum in the wavelength region of the O VII triplet (gray) with the best fit Lorentzian line profile (black). Wavelength bins corresponding to bad column pixels are plotted without error bars and were not considered in the fitting procedure.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7016fig3.ps}\end{figure}$ Figure 3: RGS2 spectrum around the Ne IX triplet (gray) with the predicted spectra obtained from the 3-T EPIC model and assuming different electron densities.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7016fig4.ps}\end{figure}$ Figure 4: Average plasma temperature and Ne/O ratio vs. age for the sample of four CTTSs with evidence of high density cool plasma.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7016fig1.ps}\end{figure}$	Figure 1: Background-subtracted light curve of MP Mus obtained by adding the three EPIC instrument data.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7016fig2.ps}\end{figure}$	Figure 2: RGS1 spectrum in the wavelength region of the O VII triplet (gray) with the best fit Lorentzian line profile (black). Wavelength bins corresponding to bad column pixels are plotted without error bars and were not considered in the fitting procedure.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7016fig3.ps}\end{figure}$	Figure 3: RGS2 spectrum around the Ne IX triplet (gray) with the predicted spectra obtained from the 3-T EPIC model and assuming different electron densities.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{7016fig4.ps}\end{figure}$	Figure 4: Average plasma temperature and Ne/O ratio vs. age for the sample of four CTTSs with evidence of high density cool plasma.
Open with DEXTER