$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig1.eps} \end{figure}$ Figure 1: Total number of ionizing photons produced from Pop III stars per baryon, cf. (Cen 2002, Fig. 14). The dotted line represents a simplified model with a constant photon production, from z=16, of 8 per unit z per baryon. The results are similar.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig2.eps} \end{figure}$ Figure 2: Production rate of ionizing photons from Pop III stars per baryon, $\frac{{\rm d}n_\gamma}{{\rm d}z}/n_{\rm b}$ . The odd form between each integer z is not physical but are due to the fact that the redshift z is a nonlinear function of time.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig3.eps} \end{figure}$ Figure 3: The co-moving relative dust density evolution $\Omega _{\rm d,0} = \rho _{\rm dust}/\rho _{\rm c}$ , for $f_{\rm d}=1$ . The minima at z=6 and 9 for $\Delta t \le 0.1$ Gyr is due to the fact that $\Delta z = 1$ is not a constant time interval.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig5.eps} \end{figure}$ Figure 5: The differential opacity d $\tau /{\rm d}z$ at $\lambda = 1$ mm for different dust lifetimes.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig6.eps} \end{figure}$ Figure 6: Energy density of ionizing photons compared to $u_{\rm CMB} = 4\sigma _{\rm S}T_{\rm CMB}^4/c$ , where $\sigma _{\rm S}$ is Stefan-Boltzmann's constant.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig7.eps} \end{figure}$ Figure 7: The dust temperature is plotted against the CMB temperature with the relative quatity $(T_{\rm d}-T_{\rm CMB})/T_{\rm CMB}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig8.eps} \end{figure}$ Figure 8: Comparison of the modeled intensity for the early dust emission in excess of the CMB with the observed FIRAS spectrum (dashed red curve) of the cosmic far IR background as detailed by Lagache et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig1.eps} \end{figure}$	Figure 1: Total number of ionizing photons produced from Pop III stars per baryon, cf. (Cen 2002, Fig. 14). The dotted line represents a simplified model with a constant photon production, from z=16, of 8 per unit z per baryon. The results are similar.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig2.eps} \end{figure}$	Figure 2: Production rate of ionizing photons from Pop III stars per baryon, $\frac{{\rm d}n_\gamma}{{\rm d}z}/n_{\rm b}$ . The odd form between each integer z is not physical but are due to the fact that the redshift z is a nonlinear function of time.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig3.eps} \end{figure}$	Figure 3: The co-moving relative dust density evolution $\Omega _{\rm d,0} = \rho _{\rm dust}/\rho _{\rm c}$ , for $f_{\rm d}=1$ . The minima at z=6 and 9 for $\Delta t \le 0.1$ Gyr is due to the fact that $\Delta z = 1$ is not a constant time interval.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig4.eps} \par\end{figure}$	Figure 4: Opacity $\tau$ with dust evolution taken into account.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig5.eps} \end{figure}$	Figure 5: The differential opacity d $\tau /{\rm d}z$ at $\lambda = 1$ mm for different dust lifetimes.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig6.eps} \end{figure}$	Figure 6: Energy density of ionizing photons compared to $u_{\rm CMB} = 4\sigma _{\rm S}T_{\rm CMB}^4/c$ , where $\sigma _{\rm S}$ is Stefan-Boltzmann's constant.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig7.eps} \end{figure}$	Figure 7: The dust temperature is plotted against the CMB temperature with the relative quatity $(T_{\rm d}-T_{\rm CMB})/T_{\rm CMB}$ .
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0448fig8.eps} \end{figure}$	Figure 8: Comparison of the modeled intensity for the early dust emission in excess of the CMB with the observed FIRAS spectrum (dashed red curve) of the cosmic far IR background as detailed by Lagache et al. (1999).
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