  We investigate the formation of methane line at 2.3 ${\rm \mu m}$ in Brown Dwarf Gliese 229B. Two sets of model parameters with (a) $T_{\rm eff}=940 $K and $\log (g) =5.0$, (b) $T_{\rm eff}=1030 $K and $ \log(g)=5.5$ are adopted both of which provide excellent fit for the synthetic continuum spectra with the observed flux at a wide range of wavelengths. In the absence of observational data for individual molecular lines, we set the additional parameters that are needed in order to model the individual lines by fitting the calculated flux with the observed flux at the continuum. A significant difference in the amount of flux at the core of the line is found with the two different models although the flux at the ontinuum remains the same. Hence, we show that if spectroscopic observation at $2.3{\rm \mu m}$ with a resolution as high as $R \simeq 200,000$ is possible then a much better constraint on the surface gravity and on the metallicity of the object could be obtained by fitting the theoretical model of individual molecular line with the observed data. 
Line Formation in the Atmosphere of Brown Dwarf Gliese 229B: $CH_4$ at   2.3 micron