All Figures

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5544f1a.ps}\vspace*{5mm} \includegraphics[width=7.6cm,clip]{5544f1b.ps}\end{figure}$ Figure 1: Infrared color-magnitude diagrams with the observed (i.e. not dereddened) positions of the IR counterparts to the XEST X-ray sources. Known TMC members are shown as filled diamonds and asterisks (asterisks are protostars), candidate members as open squares and sources that are not selected as new candidates as open diamonds. Isochrones of 1, 5 and 10 Myr (solid and dashed lines), calculated at 140 pc, are superimposed. The reddening vectors from the extinction laws by Rieke & Lebofsky (1985) are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5544f2.ps}\end{figure}$ Figure 2: Infrared color-color diagram with the observed (i.e. not dereddened) positions of known TMC members and candidate members (symbols are as in Fig. 1). The solid and dashed lines are the 10 Myr models by Baraffe et al. (1998) and Siess et al. (2000) respectively. The reddening vector is shown. The dotted lines bracket the region where stars with no excess reddening are expected to lie.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5544f3a.ps}\hspace*{7mm} \includegraphics[width=7.6cm,clip]{5544f3b.ps}\end{figure}$ Figure 3: Quantile space for X-ray sources with more than 10 net counts in the PN: known members (filled diamonds) and candidates (open squares) are shown in the left panel, X-ray sources without an IR counterpart are shown as crosses in the right panel. A theoretical grid relevant to an absorbed, isothermal and optically thin plasma is superimposed, with abundances fixed to 0.3 times the solar values of Anders & Grevesse (1989), calculated for temperatures going from $\log T =6.5$ up to $\log T =7.75$ at a logarithmic step of 0.25 and seven values for the hydrogen column density ( $N_{\rm H}=$ 0.01, 0.1, 0.5, 1, 2, 5 and 10 in units of 10²² cm^-2).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5544f4a.ps}\hspace*{7mm} \includegraphics[width=7.6cm,clip]{5544f4b.ps}\end{figure}$ Figure 4: Same as the previous figure, but for sources with more than 80 net counts in the PN. The error bars are generally smaller than those shown in the lower right part of the plots, typical of sources with about 80 counts.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5544f5.ps}\end{figure}$ Figure 5: IR color-magnitude diagram for the TMC members shown in the left panel of Fig. 3: filled and open diamonds refer to stars lying, in the quantile space, at $\log_{10} [Q_{50}/(1-Q_{50})]$ greater and lower than -0.8, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=13.15cm,clip]{5544f6.ps}\end{figure}$ Figure 6: Background-subtracted light curves (points with error bars) of six sources showing flares, obtained adding the PN, MOS1 and MOS2 counts. The points without errors represent the background emission.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{5544f8.ps}\end{figure}$ Figure 8: X-ray luminosities versus masses for the 48 candidates with mass estimates. Crosses refer to the candidates with higher probability of membership. $L_{\rm X}$ values joined by a dotted segment refer to luminosities derived for the same source in two different XEST observations. The dashed line is the relation $\log L_{\rm X}=1.53\log M + 30.3$ best-fitting the data for known TMC members (Güdel et al. 2007a) and the dotted lines bracket the region where known members are found.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5544f7a.ps}\hspace*{4mm} \... ...4f7e.ps}\hspace*{4mm} \includegraphics[width=6.9cm,clip]{5544f7f.ps}\end{figure}$ Figure 7: EPIC PN spectra of the brightest candidate members (points) with the best-fit coronal models (see Table 2 for the parameters of the models). The lower panel in each plot shows the residuals in unit of $\chi$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5544f7g.ps}\hspace*{4mm} \... ...7cm}\includegraphics[width=6.9cm,clip]{5544f7k.ps}\hspace*{3.7cm}}\end{figure}$ Figure 7: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5544f4a.ps}\hspace*{7mm} \includegraphics[width=7.6cm,clip]{5544f4b.ps}\end{figure}$	Figure 4: Same as the previous figure, but for sources with more than 80 net counts in the PN. The error bars are generally smaller than those shown in the lower right part of the plots, typical of sources with about 80 counts.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5544f5.ps}\end{figure}$	Figure 5: IR color-magnitude diagram for the TMC members shown in the left panel of Fig. 3: filled and open diamonds refer to stars lying, in the quantile space, at $\log_{10} [Q_{50}/(1-Q_{50})]$ greater and lower than -0.8, respectively.
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$\begin{figure} \par\includegraphics[width=13.15cm,clip]{5544f6.ps}\end{figure}$	Figure 6: Background-subtracted light curves (points with error bars) of six sources showing flares, obtained adding the PN, MOS1 and MOS2 counts. The points without errors represent the background emission.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5544f7a.ps}\hspace{4mm} \... ...4f7e.ps}\hspace{4mm} \includegraphics[width=6.9cm,clip]{5544f7f.ps}\end{figure}$	Figure 7: EPIC PN spectra of the brightest candidate members (points) with the best-fit coronal models (see Table 2 for the parameters of the models). The lower panel in each plot shows the residuals in unit of $\chi$ .
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5544f7g.ps}\hspace{4mm} \... ...7cm}\includegraphics[width=6.9cm,clip]{5544f7k.ps}\hspace{3.7cm}}\end{figure}$	Figure 7: continued.
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