All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2979_01.eps} \end{figure}$ Figure 1: Observational data used for this paper. The wavelength coverage of the different instruments is shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2979_02.eps} \end{figure}$ Figure 2: The contribution of different molecules to the formation of the synthetic spectrum of in $T_{\rm eff}$ /log g = 2800/5.0 model atmosphere.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2979_03.eps} \end{figure}$ Figure 3: Partition functions of molecules H₂O and HDO. Our data for H₂O are compared with Vidler & Tennyson (2000), data for HDO are compared with Hewitt et al. (2005). Our partition function for HDO is computed for s₁ =1. The differences in the HDO partition functions at higher temperatures (T > 4000 K) are due to the use of more complete sets of deuterated water levels in the UCL model compared with the AMES model.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2979_04.eps} \end{figure}$ Figure 4: Molecular densities of H₂O computed for NextGen model atmospheres 2800/5.0 and 3800/5.0 for the cases of partition functions computed with s_i = 1, 4 and s_i =1/4, 3/4.
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In the text

$\begin{figure} \par\includegraphics[width=13.7cm,clip]{2979_05.eps} \end{figure}$ Figure 5: Responses of computed spectra to variations of input parameters. A model atmosphere of 3000/5.0/0.0 was used as the reference model.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2979_06.eps}\par\includegraphics[width=8.6cm,clip]{2979_07.eps} \end{figure}$ Figure 6: Top: temperature structure of model NextGen, DUSTY and COND model atmospheres of 2800/5.0/0. Bottom: ratio of fluxes computed for these model atmospheres.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2979_08.eps} \end{figure}$ Figure 7: Ratio of fluxes computed for 2800/5.0 NextGen model atmosphere with TiO line lists by Plez (1998) and Schwenke (1998).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2979_09.eps} \end{figure}$ Figure 8: Min $F(f_{\rm s}, f_{\rm n}$ ) found for different model atmospheres.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,height=6.4cm]{2979_10.eps} % \par\vspace*{3mm} \includegraphics[width=14cm,height=6.4cm]{2979_11.eps} \end{figure}$ Figure 9: Fits with linear and logarithmic flux scales to our GJ406 spectrum with a theoretical spectrum computed for a solar composition NextGen model atmosphere 2800/5.0.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2979_12.eps} \end{figure}$ Figure 10: A comparison of $f(x_{\rm s}, x_{\rm n}$ ) computed for the fitting ofobserved spectra by NextGen and Cond synthetic spectra.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{2979_13.eps}\par\vspace*{3mm} \includegraphics[width=7.7cm,clip]{2979_14.eps} \end{figure}$ Figure 11: Top: location of GJ 406 in respect to the Baraffe et al. (1998) evolutionary tracks and $T_{\rm eff}$ = 2800, 2600 K and $L = L_*/L_\odot =-2.90$ , -3.00 planes. The planes shown on plot determine the cuboid of our errors of $T_{\rm eff}$ and L. Bottom: location of GJ 406 in respect to evolutionary tracks in coordinates L, t, M. The thick lines shown on plot determine the cuboid of our errors of age, luminosity $L_*/L_\odot$ and mass M_*.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2979_01.eps} \end{figure}$	Figure 1: Observational data used for this paper. The wavelength coverage of the different instruments is shown.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2979_02.eps} \end{figure}$	Figure 2: The contribution of different molecules to the formation of the synthetic spectrum of in $T_{\rm eff}$ /log g = 2800/5.0 model atmosphere.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2979_04.eps} \end{figure}$	Figure 4: Molecular densities of H₂O computed for NextGen model atmospheres 2800/5.0 and 3800/5.0 for the cases of partition functions computed with s_i = 1, 4 and s_i =1/4, 3/4.
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$\begin{figure} \par\includegraphics[width=13.7cm,clip]{2979_05.eps} \end{figure}$	Figure 5: Responses of computed spectra to variations of input parameters. A model atmosphere of 3000/5.0/0.0 was used as the reference model.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2979_06.eps}\par\includegraphics[width=8.6cm,clip]{2979_07.eps} \end{figure}$	Figure 6: Top: temperature structure of model NextGen, DUSTY and COND model atmospheres of 2800/5.0/0. Bottom: ratio of fluxes computed for these model atmospheres.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2979_08.eps} \end{figure}$	Figure 7: Ratio of fluxes computed for 2800/5.0 NextGen model atmosphere with TiO line lists by Plez (1998) and Schwenke (1998).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2979_09.eps} \end{figure}$	Figure 8: Min $F(f_{\rm s}, f_{\rm n}$ ) found for different model atmospheres.
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$\begin{figure} \par\includegraphics[width=14cm,height=6.4cm]{2979_10.eps} % \par\vspace*{3mm} \includegraphics[width=14cm,height=6.4cm]{2979_11.eps} \end{figure}$	Figure 9: Fits with linear and logarithmic flux scales to our GJ406 spectrum with a theoretical spectrum computed for a solar composition NextGen model atmosphere 2800/5.0.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2979_12.eps} \end{figure}$	Figure 10: A comparison of $f(x_{\rm s}, x_{\rm n}$ ) computed for the fitting ofobserved spectra by NextGen and Cond synthetic spectra.
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