All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2219fig1.eps} \end{figure}$ Figure 1: The lower panel shows the best fit to the CO first bandhead toward 08576nr292. In the upper part the observed spectrum is shown. The spectrum is continuum-subtracted and normalized to the peak of the 2-0 bandhead. The best fit of the CO-bandhead is plotted in the lower part. The parameters of the fit are discussed in Bik & Thi (2004). Features shortward of 2.2935 $\mu$ m are shown in detail in the upper panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2219fig2.eps} \end{figure}$ Figure 2: Best fit to the hot water lines with the slab model. The upper spectrum is a blowup of the spectrum showed in Fig. 1 between 2.278 and 2.292 $\mu$ m, normalized to the maximum strength at $\simeq$ 2.280 $\mu$ m. The middle one represents the best fit, while the lower curve is the synthetic spectrum before degradation at the resolution of the observed spectrum. The characteristic of the strong detected lines, which are labeled 1 to 10, are given in Table 2. The H₂ 3-2 S(1) emission line is located at position 6.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{2219fig3.ps} \end{figure}$ Figure 3: Typical line optical depth for the hot water lines with dv=5 km s^-1, $T_{\rm gas}=1500$ K, and N(CO $)=3 \times 10 ^{18}$ cm^-2.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2219fig4.eps} \end{figure}$ Figure 4: Best fit to the water lines toward 08576nr292 using the disk model. The upper curve is the observed normalized and continuum subtracted spectrum. The middle one represents the best fit, while the lower curve is the synthetic spectrum before degradation at the resolution of the observed spectrum. Notice the double-peak profile for lines which are not blended.
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In the text

$\begin{figure} \par\includegraphics[height=16cm,angle=90]{2219fig5.ps} %\end{figure}$ Figure 5: Relative abundance of various species as a function of time and enhanced interstellar UV field $I_{{\rm UV}}$ . The gas is free of dust grains has a temperature of 1600 K and has a density of 10¹² cm^-3 as deduced from the fitting to the CO and H₂O emission lines. CO self-shielding was not included in these models.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2219fig6.eps} \end{figure}$ Figure 6: Schematic representation of the proposed chemical network. OH radicals play a central role in this network. $\nu$ means photodissociation by ultraviolet photons and M a third body (M = H, He). The main routes leading to CO and H₂O are shown here.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16cm,clip]{2219fig7.ps} \end{figure}$ Figure 7: Relative abundance of various species as a function of $I_{{\rm UV}}/n_{{\rm H}}$ for gas at temperature 1600 K, 2000 K, 3000 K, 4000 K.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90]{2219fig8.eps}} \end{figure}$ Figure 8: Effect of CO self-shielding on abundance ratios. The left panel shows the addition of a strong self-shielding on the chemistry, while the right panel is the same as the upper right panel in Fig. 7. As expected the changes happen only on the H₂O/CO and CO/H ratios. The observed value of H₂O/CO ( $\sim$ $5.4\times 10^{-4}$ ) is indicated by a gray strip.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90]{2219fig9.ps}} \end{figure}$ Figure 9: H₂O/CO versus H₂O/OH diagram for various $I_{{\rm UV}}/n_{{\rm H}}$ and gas temperature.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90]{2219fig10.ps}} \end{figure}$ Figure 10: Effect of the CO self-shielding on the relative abundances. The self-shielding factor depends on the CO column density N(CO). The parameters of the model are $T_{{\rm gas}}$ =1600 K, $n_{{\rm H}}=10^{12}$ cm^-3, and $I_{{\rm UV}}=10^{8}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90]{2219fig11.ps}} \end{figure}$ Figure 11: Effect of the oxygen elemental abundance on the relative abundance of CO, OH, and H2O. $X_{{\rm o}}$ (O) is the nominal value of the Oxygen elemental abundance. The parameters of the model are $T_{{\rm gas}}=1600$ K, $n_{{\rm H}}=10^{12}$ cm^-3, and $I_{{\rm UV}}=10^{8}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{2219fig3.ps} \end{figure}$	Figure 3: Typical line optical depth for the hot water lines with dv=5 km s^-1, $T_{\rm gas}=1500$ K, and N(CO $)=3 \times 10 ^{18}$ cm^-2.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2219fig4.eps} \end{figure}$	Figure 4: Best fit to the water lines toward 08576nr292 using the disk model. The upper curve is the observed normalized and continuum subtracted spectrum. The middle one represents the best fit, while the lower curve is the synthetic spectrum before degradation at the resolution of the observed spectrum. Notice the double-peak profile for lines which are not blended.
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$\begin{figure} \par\includegraphics[height=16cm,angle=90]{2219fig5.ps} %\end{figure}$	Figure 5: Relative abundance of various species as a function of time and enhanced interstellar UV field $I_{{\rm UV}}$ . The gas is free of dust grains has a temperature of 1600 K and has a density of 10¹² cm^-3 as deduced from the fitting to the CO and H₂O emission lines. CO self-shielding was not included in these models.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{2219fig6.eps} \end{figure}$	Figure 6: Schematic representation of the proposed chemical network. OH radicals play a central role in this network. $\nu$ means photodissociation by ultraviolet photons and M a third body (M = H, He). The main routes leading to CO and H₂O are shown here.
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$\begin{figure} \par\includegraphics[angle=90,width=16cm,clip]{2219fig7.ps} \end{figure}$	Figure 7: Relative abundance of various species as a function of $I_{{\rm UV}}/n_{{\rm H}}$ for gas at temperature 1600 K, 2000 K, 3000 K, 4000 K.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90]{2219fig8.eps}} \end{figure}$	Figure 8: Effect of CO self-shielding on abundance ratios. The left panel shows the addition of a strong self-shielding on the chemistry, while the right panel is the same as the upper right panel in Fig. 7. As expected the changes happen only on the H₂O/CO and CO/H ratios. The observed value of H₂O/CO ( $\sim$ $5.4\times 10^{-4}$ ) is indicated by a gray strip.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90]{2219fig9.ps}} \end{figure}$	Figure 9: H₂O/CO versus H₂O/OH diagram for various $I_{{\rm UV}}/n_{{\rm H}}$ and gas temperature.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90]{2219fig10.ps}} \end{figure}$	Figure 10: Effect of the CO self-shielding on the relative abundances. The self-shielding factor depends on the CO column density N(CO). The parameters of the model are $T_{{\rm gas}}$ =1600 K, $n_{{\rm H}}=10^{12}$ cm^-3, and $I_{{\rm UV}}=10^{8}$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=90]{2219fig11.ps}} \end{figure}$	Figure 11: Effect of the oxygen elemental abundance on the relative abundance of CO, OH, and H2O. $X_{{\rm o}}$ (O) is the nominal value of the Oxygen elemental abundance. The parameters of the model are $T_{{\rm gas}}=1600$ K, $n_{{\rm H}}=10^{12}$ cm^-3, and $I_{{\rm UV}}=10^{8}$ .
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