All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2855fig1.eps} \end{figure}$ Figure 1: Equivalent width (EW) for various H₂ lines as a function of H₂ column density. The solid, dotted, dashed, and dot-dashed lines represent the line wavelengths of $\lambda =2.12$ , 2.22, 17, and 28 $\mu$ m, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2855fig2.eps}\end{figure}$ Figure 2: The 2.12 $\mu$ m line absorption flux as a function of the column density of hydrogen molecules, and various continuum fluxes of the background sources. The solid, dotted, dashed, and dot-dashed curves correspond to the continuum fluxes of 30, 10, 3, and 1 mJy, respectively. The horizontal thin solid line shows the expected detection limit of future cooled space telescopes such as SPICA (5 $\sigma$ for an integration of $\sim$ 1 h).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2855fig3.eps} \end{figure}$ Figure 3: Observed flux of a gamma-ray burst afterglow as a function of redshift. The solid and dotted lines correspond to the restframe wavelengths of 2.12 and 17 $\mu$ m, i.e., observational wavelengths of 2.12(1+z) and $17(1+z)~\mu$ m, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2855fig4.eps} \end{figure}$ Figure 4: Same as Fig. 2, but for various dust-to-gas ratios ( $\kappa$ is the dust-to-gas ratio normalized to the Galactic value). The continuum fluxes of the background sources is assumed to be 10 mJy. The solid, dotted, dashed, and dot-dashed lines correspond to $\kappa =0.01$ , 0.1, 1, and 0.001, respectively. The lower dotted line represents the result with the H05b extinction curve, while the other lines adopt the Galactic extinction curve.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2855fig5.eps} \end{figure}$ Figure 5: Probability distribution function of the molecular fraction ( $\log f_{\rm H_2}$ ) for various hydrogen column densities. The solid, dotted, dashed, dot-dashed, and dot-dot-dot-dashed lines correspond to $\log N_{\rm H}~({\rm cm}^{-2})=21$ , 22, 22.5, 23, and 23.5, respectively. The dust-to-gas ratio normalized to the Galactic value is assumed to be $\kappa =0.01$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2855fig1.eps} \end{figure}$	Figure 1: Equivalent width (EW) for various H₂ lines as a function of H₂ column density. The solid, dotted, dashed, and dot-dashed lines represent the line wavelengths of $\lambda =2.12$ , 2.22, 17, and 28 $\mu$ m, respectively.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2855fig3.eps} \end{figure}$	Figure 3: Observed flux of a gamma-ray burst afterglow as a function of redshift. The solid and dotted lines correspond to the restframe wavelengths of 2.12 and 17 $\mu$ m, i.e., observational wavelengths of 2.12(1+z) and $17(1+z)~\mu$ m, respectively.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2855fig5.eps} \end{figure}$	Figure 5: Probability distribution function of the molecular fraction ( $\log f_{\rm H_2}$ ) for various hydrogen column densities. The solid, dotted, dashed, dot-dashed, and dot-dot-dot-dashed lines correspond to $\log N_{\rm H}~({\rm cm}^{-2})=21$ , 22, 22.5, 23, and 23.5, respectively. The dust-to-gas ratio normalized to the Galactic value is assumed to be $\kappa =0.01$ .
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