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$\begin{figure} \par\includegraphics[angle=90,width=16.7cm,clip]{1301fig1.ps}\end{figure}$ Figure 1: The evolution of the SED for the single-sized dust size distribution. From left to right, the star formation rate (SFR) is 10, 30, and $100~M_\odot~\mbox{yr}^{-1}$ . The dotted, dashed, dot-dashed, long-dashed, and solid lines give the age of major star formation in a galaxy as $1.0\times 10^7~$ yr, $3.0\times 10^7~$ yr, $1.0\times 10^8~$ yr, $3.0\times 10^8~$ yr, $3.0\times 10^7~$ yr, and $1.0\times 10^9~$ yr, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.7cm,clip]{1301fig2.ps}\end{figure}$ Figure 2: The evolution of the SED for the power-law dust size distribution. In comparison with Fig. 1 we see a clear difference in the MIR.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=15.9cm,clip]{1301fig3.ps}\end{figure}$ Figure 3: Model spectral energy distribution (SED) of a lensed Lyman-break galaxy MS 1512-cB58 (cB58). The left panel shows the observed SED calculated based on the single-sized dust size distribution with silicate grain radius $a_{\rm sil}=6~\mbox{\AA}$ and carbon grain radius $a_{\rm C}=200~\mbox{\AA}$ . The observed SED is magnified by a factor of 30. The right panel shows the SED for a power-law grain size distribution. Symbols represent the measured flux densities reported by Sawicki (2001) (upper limits), Baker et al. (2001) (open triangles) and van der Werf et al. (2001) (open squares). In both panels, dotted lines represent the SED at the age of $t_{\rm SF}=35~$ Myr, and dashed lines at $t_{\rm SF} = 140~$ Myr, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1301fig4.ps}\end{figure}$ Figure 4: Effect of the size of the star-forming regions on the model SED of cB58. The solid line is the canonical model (same as the solid line in the left panel of Fig. 3). Dotted, dashed, and dot-dashed lines indicate the SED calculated with a radius of the star-forming region, $r_{\rm SF}=300~\mbox{pc}$ , 120 pc, and 30 pc, respectively. Note that the SED is presented here in the units of $\nu L_\nu~[L_\odot]$ .
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.85cm,clip]{1301fig5.ps}\end{figure}$ Figure 5: Prediction for the observed IR/submm SEDs of LBGs at z=2, 3, and 4. The star formation rate ( SFR) is $10~M_\odot ~{\rm yr}^{-1}$ , and the dust grains are single-sized. The dotted, dashed, dot-dashed, long-dashed, and solid lines represent, as in Fig. 1, ages of major star formation in a galaxy of $1.0\times 10^7~$ yr, $3.0\times 10^7~$ yr, $1.0\times 10^8~$ yr, $3.0\times 10^8~$ yr, $3.0\times 10^7~$ yr, and $1.0\times 10^9~$ yr, respectively. The confusion limits of Herschel and detection limits of an ALMA 8-h survey are also shown by gray and black thick horizontal lines, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.85cm,clip]{1301fig6.ps}\end{figure}$ Figure 6: The same as Fig. 5, but for an SFR of $30~M_\odot ~{\rm yr}^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.85cm,clip]{1301fig7.ps}\end{figure}$ Figure 7: The same as Fig. 5, but for an SFR of $100~M_\odot ~{\rm yr}^{-1}$ . The silicate feature finally appears in absorption.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.8cm,clip]{1301fig8.ps}\end{figure}$ Figure 8: Prediction for the observed IR/submm SEDs of LBGs at z=2, 3, and 4. The star formation rate (SFR) is $10~M_\odot ~{\rm yr}^{-1}$ , and the dust grains are power-law.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.8cm,clip]{1301fig9.ps}\end{figure}$ Figure 9: The same as Fig. 8, but for an SFR of $30~M_\odot ~{\rm yr}^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.8cm,clip]{1301fig10.ps}\end{figure}$ Figure 10: The same as Fig. 8, but for an SFR of $100~M_\odot ~{\rm yr}^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1301fig11.ps}\end{figure}$ Figure 11: The contribution of LBGs to the cosmic infrared background radiation (CIRB) (open symbols). Filled symbols and hatched area are the measured CIRB spectrum by COBE (Lagache et al. 1999; Fixsen et al. 1998; Hauser et al. 1998).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.7cm,clip]{1301fig2.ps}\end{figure}$	Figure 2: The evolution of the SED for the power-law dust size distribution. In comparison with Fig. 1 we see a clear difference in the MIR.
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$\begin{figure} \par\includegraphics[angle=90,width=16.85cm,clip]{1301fig6.ps}\end{figure}$	Figure 6: The same as Fig. 5, but for an SFR of $30~M_\odot ~{\rm yr}^{-1}$ .
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$\begin{figure} \par\includegraphics[angle=90,width=16.85cm,clip]{1301fig7.ps}\end{figure}$	Figure 7: The same as Fig. 5, but for an SFR of $100~M_\odot ~{\rm yr}^{-1}$ . The silicate feature finally appears in absorption.
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$\begin{figure} \par\includegraphics[angle=90,width=16.8cm,clip]{1301fig8.ps}\end{figure}$	Figure 8: Prediction for the observed IR/submm SEDs of LBGs at z=2, 3, and 4. The star formation rate (SFR) is $10~M_\odot ~{\rm yr}^{-1}$ , and the dust grains are power-law.
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$\begin{figure} \par\includegraphics[angle=90,width=16.8cm,clip]{1301fig9.ps}\end{figure}$	Figure 9: The same as Fig. 8, but for an SFR of $30~M_\odot ~{\rm yr}^{-1}$ .
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$\begin{figure} \par\includegraphics[angle=90,width=16.8cm,clip]{1301fig10.ps}\end{figure}$	Figure 10: The same as Fig. 8, but for an SFR of $100~M_\odot ~{\rm yr}^{-1}$ .
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1301fig11.ps}\end{figure}$	Figure 11: The contribution of LBGs to the cosmic infrared background radiation (CIRB) (open symbols). Filled symbols and hatched area are the measured CIRB spectrum by COBE (Lagache et al. 1999; Fixsen et al. 1998; Hauser et al. 1998).
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