$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4173fig1.eps}\end{figure}$ Figure 1: The observed bright and weak stars in the galactic center and anti-center fields of view of the CoRoT space telescope.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,height=6.7cm,clip]{4173fig2.ps} \end{figure}$ Figure 2: The observed spectrum of SW Mon (dots) with the template spectrum of the M5 III star HD 130144 (solid line) overplotted.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,height=6.3cm,clip]{4173fig3.ps}\end{figure}$ Figure 3: HR diagram of program stars (asterisks) with known parallax. Bullets indicate the H $\alpha$ emission stars. The ZAMS and a sample of evolutionary tracks for Z=0.019 from Girardi et al. (2000) are also plotted.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,height=6.3cm,clip]{4173fig4.ps}\end{figure}$ Figure 4: $L_{\rm X}$ / $L_{\rm bol}$ vs. H $\alpha$ EW for H $\alpha$ emission stars. The solid line is a linear fit to the data. The linear correlation coefficient (r) and its significance level ( $\alpha$ ) are given in the label. A logarithmic scale is used for the X-axis.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{4173fig5.ps}\end{figure}$ Figure 5: Top panels: normalized spectra of program stars with evidence of the Li 6708 Å line (continuous line) and non-active template spectra (small filled circles) used for SST. Bottom panels: the residual flux from the spectral subtraction technique.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4173fig1.eps}\end{figure}$	Figure 1: The observed bright and weak stars in the galactic center and anti-center fields of view of the CoRoT space telescope.
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$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,height=6.7cm,clip]{4173fig2.ps} \end{figure}$	Figure 2: The observed spectrum of SW Mon (dots) with the template spectrum of the M5 III star HD 130144 (solid line) overplotted.
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$\begin{figure} \par\includegraphics[angle=90,width=8cm,height=6.3cm,clip]{4173fig3.ps}\end{figure}$	Figure 3: HR diagram of program stars (asterisks) with known parallax. Bullets indicate the H $\alpha$ emission stars. The ZAMS and a sample of evolutionary tracks for Z=0.019 from Girardi et al. (2000) are also plotted.
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$\begin{figure} \par\includegraphics[width=7.4cm,height=6.3cm,clip]{4173fig4.ps}\end{figure}$	Figure 4: $L_{\rm X}$ / $L_{\rm bol}$ vs. H $\alpha$ EW for H $\alpha$ emission stars. The solid line is a linear fit to the data. The linear correlation coefficient (r) and its significance level ( $\alpha$ ) are given in the label. A logarithmic scale is used for the X-axis.
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$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{4173fig5.ps}\end{figure}$	Figure 5: Top panels: normalized spectra of program stars with evidence of the Li 6708 Å line (continuous line) and non-active template spectra (small filled circles) used for SST. Bottom panels: the residual flux from the spectral subtraction technique.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{4173fig6.eps}\end{figure}$	Figure 6: Results of the spectral subtraction.
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