All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3081fig1.ps} \end{figure}$ Figure 1: First energy levels for the HDO molecule.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3081fig2.ps} \end{figure}$ Figure 2: HDO line fluxes predicted for the test case IRAS 16293-2422 versus the upper level energy of the transition. The upper panel presents the transitions observable from the ground, the middle panel the transitions observable with HSO/HIFI and the lower panel the transitions observable with SOFIA. The frequencies of the transitions that are going to be studied in more detail are indicated in GHz.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3081fig3.ps} \end{figure}$ Figure 3: Contribution to the line intensity as function of the distance from the central source, for seven HDO lines observable from the ground ( upper panel) and six from space based telescopes ( lower panel).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.4cm,clip]{3081fig4.ps} \end{figure}$ Figure 4: Line intensity as a function of the HDO abundance in the outer and inner regions of the envelope, $x_{\rm cold}$ and $x_{\rm warm}$ respectively, for the eight HDO transitions at 464, 893, 509, 80, 241, 225, 919 and 995 GHz respectively. The first six lines are observable from the ground, whereas the last two ones will be observable with the Herschel telescope. Line fluxes are in erg s^-1 cm^-2. In these calculations the mantle evaporation temperature is 100 K.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3081fig5.ps} \end{figure}$ Figure 5: Predicted flux for the eight transitions depending on the assumed evaporation temperature and inner HDO abundance for an outer abundance $x_{\rm cold}$ fixed to 2 $\times$ 10^-10.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3081fig6.ps} \end{figure}$ Figure 6: Predicted flux for the eight transitions depending on the assumed evaporation temperature and outer HDO abundance for an inner abundance $x_{\rm warm}$ fixed to 10^-7.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3081fig7.ps} \end{figure}$ Figure 7: Evaporation temperature dependence in a $x_{\rm warm}$ - $x_{\rm cold}$ diagram. For each transition, the three groups of curves correspond to the contour for three different values of the line flux. The different curves for each group correspond to different values of the evaporation temperature. A narrow group of curves implies that the uncertainty on the evaporation temperature value will not affect much the estimation of $x_{\rm warm}$ and $x_{\rm cold}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3081fig8.ps} \end{figure}$ Figure B.1: HDO line fluxes predicted for the case of the low-luminosity source L1448 mm, for an assumed HDO abundance of 10^-10 and 10^-7 in the cold and warm parts of the envelope respectively. The upper panel presents the transitions observable from the ground, the middle panel the transitions observable with HSO/HIFI and the lower panel the transitions observable with SOFIA. The frequencies of the transitions that are going to be studied in more detail are indicated in GHz.

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3081fig9.ps} \end{figure}$ Figure B.2: Line intensity as a function of the HDO abundance in the outer and inner regions of the envelope, $x_{\rm cold}$ and $x_{\rm warm}$ respectively, for the eight HDO transitions at 464, 893, 509, 80, 241, 225, 919 and 995 GHz respectively towards the low-luminosity source L1448 mm. Line fluxes are in erg s^-1 cm^-2. In these calculations the mantle evaporation temperature is 100 K.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3081fi10.ps} \end{figure}$ Figure B.3: Line intensity as a function of the inner HDO abundance and the evaporation temperature, for the eight HDO transitions at 464, 893, 509, 80, 241, 225, 919 and 995 GHz respectively towards the low-luminosity source L1448 mm. Line fluxes are in erg s^-1 cm^-2. In these calculations the outer HDO abundance is 10^-10.

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3081fig1.ps} \end{figure}$	Figure 1: First energy levels for the HDO molecule.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{3081fig3.ps} \end{figure}$	Figure 3: Contribution to the line intensity as function of the distance from the central source, for seven HDO lines observable from the ground ( upper panel) and six from space based telescopes ( lower panel).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3081fig5.ps} \end{figure}$	Figure 5: Predicted flux for the eight transitions depending on the assumed evaporation temperature and inner HDO abundance for an outer abundance $x_{\rm cold}$ fixed to 2 $\times$ 10^-10.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3081fig6.ps} \end{figure}$	Figure 6: Predicted flux for the eight transitions depending on the assumed evaporation temperature and outer HDO abundance for an inner abundance $x_{\rm warm}$ fixed to 10^-7.
Open with DEXTER