$\begin{figure} \par\includegraphics[width=6.8cm,clip]{specfig2.eps} \end{figure}$ Figure 2: Hamilton spectra of HD 358623 B. To estimate the contamination from the primary, we took an empty sky spectrum with the same separation from the primary and opposite position angle. Equivalent width of the H $\alpha$ line is $\sim$ 4 Å.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{cmdplot.eps}\end{figure}$ Figure 3: Color-magnitude diagram showing (top to bottom) HD 199143 A, HD 358623 A, HD 199143 B, and HD 358623 B. Baraffe et al. (2002) isochrones, from left to right, are 100 Myr (dashed line) 32 Myr, 20 Myr (solid line), 10 Myr, and 3 Myr. Positions of main-sequence Gliese stars are indicated by the "+'' symbols. Colors are from the 2MASS catalogue.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{sedfig1.eps}\end{figure}$ Figure 4: Synthetic SEDs (Hauschildt et al. 1999) for HD 199143 A and B with overplotted mid-IR data. Effective temperatures for the models are $T_{\rm eff}$ (A) = 6400 K and $T_{\rm eff}$ (B) = 3700 K, with Z=0.02 and ${\rm log}~(g)=4.5$ for both models. Filled circles represent the photometric measurements of Section 2.1.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{sedfig2.eps}\end{figure}$ Figure 5: Synthetic SEDs (Hauschildt et al. 1999) for HD 358623 A and B with overplotted mid-IR data. $T_{\rm eff}$ (A) = 4400 K and $T_{\rm eff}$ (B) = 3300 K, with Z = 0.02 and ${\rm log}~(g)=4.5$ for both models. The plotted upper limits at 17.65 $\mu$ m are 1-sigma values. Filled circles represent the photometric measurements of Sect. 2.1.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{specfig.ps} \end{figure}$	Figure 1: Hamilton Echelle spectra of HD 199143 and HD 358623.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{specfig2.eps} \end{figure}$	Figure 2: Hamilton spectra of HD 358623 B. To estimate the contamination from the primary, we took an empty sky spectrum with the same separation from the primary and opposite position angle. Equivalent width of the H $\alpha$ line is $\sim$ 4 Å.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{cmdplot.eps}\end{figure}$	Figure 3: Color-magnitude diagram showing (top to bottom) HD 199143 A, HD 358623 A, HD 199143 B, and HD 358623 B. Baraffe et al. (2002) isochrones, from left to right, are 100 Myr (dashed line) 32 Myr, 20 Myr (solid line), 10 Myr, and 3 Myr. Positions of main-sequence Gliese stars are indicated by the "+'' symbols. Colors are from the 2MASS catalogue.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{sedfig1.eps}\end{figure}$	Figure 4: Synthetic SEDs (Hauschildt et al. 1999) for HD 199143 A and B with overplotted mid-IR data. Effective temperatures for the models are $T_{\rm eff}$ (A) = 6400 K and $T_{\rm eff}$ (B) = 3700 K, with Z=0.02 and ${\rm log}~(g)=4.5$ for both models. Filled circles represent the photometric measurements of Section 2.1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{sedfig2.eps}\end{figure}$	Figure 5: Synthetic SEDs (Hauschildt et al. 1999) for HD 358623 A and B with overplotted mid-IR data. $T_{\rm eff}$ (A) = 4400 K and $T_{\rm eff}$ (B) = 3300 K, with Z = 0.02 and ${\rm log}~(g)=4.5$ for both models. The plotted upper limits at 17.65 $\mu$ m are 1-sigma values. Filled circles represent the photometric measurements of Sect. 2.1.
Open with DEXTER