$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2729f2.ps}\hspace*{4mm} \includegraphics[width=8.3cm,clip]{2729f3.ps} \end{figure}$ Figure 2: EPIC spectra (PN in left panel, MOS1 and MOS2 in right panel) of TWA 5 with best-fit 3-T models superimposed. The lower section of each panel contains residuals. Best-fit parameters are reported in Table 3.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2729f5.ps} \end{figure}$ Figure 4: Comparison between observed and predicted line fluxes in the RGS spectra. The predicted values are obtained using the models derived with the MCMC method (see Sect. 3.2).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f6.ps} \end{figure}$ Figure 5: Emission measure distribution of TWA 5 obtained from the RGS line fluxes with the MCMC method, along with the values obtained with the 3-T best-fit model of PN and MOS spectra. The uncertainties correspond to a 68% statistical confidence level.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f7.ps} \end{figure}$ Figure 6: Abundances of TWA 5 with respect to solar photospheric values (Anders & Grevesse 1989), obtained using the RGS line fluxes with the MCMC method, along with the values obtained with the 3-T best-fit model of PN and MOS spectra. The uncertainties correspond to the 68% confidence level, except the error bar of Fe derived from RGS data, which has been obtained with a different procedure, as discussed in Sects. 3.2 and 4.2.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f8.ps} \end{figure}$ Figure 7: O VII triplet in the RGS1 spectrum of TWA 5, rebinned with a wavelength bin of 0.03 Å, with best-fit line profiles: individual lines ( dotted line) and their sum ( solid line).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f9.ps} \end{figure}$ Figure 8: Ne/Fe abundance ratio in solar photospheric units (Anders & Grevesse 1989) for the PMS stars listed in Table 1 and sorted by H $\alpha$ equivalent width.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f10.ps} \end{figure}$ Figure 9: Ne/Fe abundance ratio in solar photospheric units (Anders & Grevesse 1989) for the PMS stars listed in Table 1 vs. the X-ray to bolometric luminosity ratio.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f1.ps} \end{figure}$	Figure 1: XMM-Newton/PN light curve of TWA 5 with bin size of 500 s.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2729f2.ps}\hspace*{4mm} \includegraphics[width=8.3cm,clip]{2729f3.ps} \end{figure}$	Figure 2: EPIC spectra (PN in left panel, MOS1 and MOS2 in right panel) of TWA 5 with best-fit 3-T models superimposed. The lower section of each panel contains residuals. Best-fit parameters are reported in Table 3.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{2729f4.ps} \end{figure}$	Figure 3: Observed and predicted RGS spectra (rebinned with a wavelength bin of 0.03 Å) of TWA 5.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2729f5.ps} \end{figure}$	Figure 4: Comparison between observed and predicted line fluxes in the RGS spectra. The predicted values are obtained using the models derived with the MCMC method (see Sect. 3.2).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f6.ps} \end{figure}$	Figure 5: Emission measure distribution of TWA 5 obtained from the RGS line fluxes with the MCMC method, along with the values obtained with the 3-T best-fit model of PN and MOS spectra. The uncertainties correspond to a 68% statistical confidence level.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f8.ps} \end{figure}$	Figure 7: O VII triplet in the RGS1 spectrum of TWA 5, rebinned with a wavelength bin of 0.03 Å, with best-fit line profiles: individual lines ( dotted line) and their sum ( solid line).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f9.ps} \end{figure}$	Figure 8: Ne/Fe abundance ratio in solar photospheric units (Anders & Grevesse 1989) for the PMS stars listed in Table 1 and sorted by H $\alpha$ equivalent width.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2729f10.ps} \end{figure}$	Figure 9: Ne/Fe abundance ratio in solar photospheric units (Anders & Grevesse 1989) for the PMS stars listed in Table 1 vs. the X-ray to bolometric luminosity ratio.
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