All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5290fig1.eps} \end{figure}$ Figure 1: m₈₅₆-m₉₁₄ index versus effective temperature relation derived from the corresponding WFI intermediate-band filters and the synthetic low-resolution StarDusty spectra for low-mass stars and BDs by Allard et al. (2000). The two solid lines show the relation for $\log g$ = 5.0 (lower boundary) and $\log g$ = 3.5 (upper boundary); the dashed line represents the $T_{\rm eff}$ -color relation for $\log g$ = 4.0. The point represents the observed color index for ISO-CHA II 13.
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In the text

$\begin{figure} \par\includegraphics[width=8.85cm,clip]{5290fig2.eps} \end{figure}$ Figure 2: Optical spectrum of ISO-CHA II 13 (thin line). Note the strong H $\alpha$ emission. Overplotted with a thick line is the best-fitted average M7 template, reddened at $A_{\rm V}=5.0$ . The spectra are normalized to the flux at 7550 Å.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5290fig3.eps} \end{figure}$ Figure 3: Spectral energy distribution of ISO-CHA II 13. The StarDusty spectrum with the same temperature as the BD is over-plotted. The continuous line is the sum of the star and disk emissions assuming black-body emission from the disk, while the dashed line is the result of the fit performed with the FitCGplus tool by Dullemond et al. (2001).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{5290fig4.ps} \end{figure}$ Figure 4: Zoom of the spectrum in Fig. 2 showing the Ca II infrared triplet lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.85cm,clip]{5290fig2.eps} \end{figure}$	Figure 2: Optical spectrum of ISO-CHA II 13 (thin line). Note the strong H $\alpha$ emission. Overplotted with a thick line is the best-fitted average M7 template, reddened at $A_{\rm V}=5.0$ . The spectra are normalized to the flux at 7550 Å.
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5290fig3.eps} \end{figure}$	Figure 3: Spectral energy distribution of ISO-CHA II 13. The StarDusty spectrum with the same temperature as the BD is over-plotted. The continuous line is the sum of the star and disk emissions assuming black-body emission from the disk, while the dashed line is the result of the fit performed with the FitCGplus tool by Dullemond et al. (2001).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{5290fig4.ps} \end{figure}$	Figure 4: Zoom of the spectrum in Fig. 2 showing the Ca II infrared triplet lines.
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