Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1899fig1.eps} \end{figure}$ Figure 1: HDO 464.9 GHz line observed on-source (IRAS 16293 "B'') at the JCMT.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{1899fig2.ps} \end{figure}$ Figure 2: HDO lines observed at the 30 m on the outflow and on-source (IRAS 16293 "B'').
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1899fig3.ps} \end{figure}$ Figure 3: Rereduction of the HDO 225.9 and 241.6 GHz lines observed by Stark et al. in 2001 at JCMT on IRAS 16293 "A''.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1899fig4.ps} \end{figure}$ Figure 4: $x{^{\tiny\rm{HDO}}_{\rm in}}$ and $x{^{\tiny\rm{HDO}}_{\rm out}}$ contours (1, 2 and 3 $\sigma$ ) for the reduced $\chi ^2$ . The "+'' corresponds to the best fit model. $x{^{\tiny\rm{HDO}}_{\rm in}}$ is very well constrained, ( $1\pm 0.3\times 10^{-7}$ ), as well as the upper limit of $x{^{\tiny\rm{HDO}}_{\rm out}}$ ( $\leq$ $1\times 10^{-9}$ , 3 $\sigma$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1899fig5.eps} \end{figure}$ Figure 5: Radial emission profiles of the five HDO lines, using $x{^{\tiny\rm {HDO}}_{\rm in}} = 1\times10^{-7}$ and $x{^{\tiny\rm {HDO}}_{\rm out}} = 1.5\times10^{-10}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1899fig6.eps} \end{figure}$ Figure 6: Ratios between the observations on IRAS 16293 "B'' and the model predictions for three cases: a) the jump model with $x{^{\tiny\rm {HDO}}_{\rm in}} = 1\times10^{-7}$ and $x{^{\tiny\rm {HDO}}_{\rm out}} = 1.5\times10^{-10}$ , b) a model with a constant abundance throughout the envelope, and c) a case of no enhancement at all of the emission associated with the outer envelope (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1899fig1.eps} \end{figure}$	Figure 1: HDO 464.9 GHz line observed on-source (IRAS 16293 "B'') at the JCMT.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{1899fig2.ps} \end{figure}$	Figure 2: HDO lines observed at the 30 m on the outflow and on-source (IRAS 16293 "B'').
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1899fig3.ps} \end{figure}$	Figure 3: Rereduction of the HDO 225.9 and 241.6 GHz lines observed by Stark et al. in 2001 at JCMT on IRAS 16293 "A''.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1899fig4.ps} \end{figure}$	Figure 4: $x{^{\tiny\rm{HDO}}_{\rm in}}$ and $x{^{\tiny\rm{HDO}}_{\rm out}}$ contours (1, 2 and 3 $\sigma$ ) for the reduced $\chi ^2$ . The "+'' corresponds to the best fit model. $x{^{\tiny\rm{HDO}}_{\rm in}}$ is very well constrained, ( $1\pm 0.3\times 10^{-7}$ ), as well as the upper limit of $x{^{\tiny\rm{HDO}}_{\rm out}}$ ( $\leq$ $1\times 10^{-9}$ , 3 $\sigma$ ).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1899fig5.eps} \end{figure}$	Figure 5: Radial emission profiles of the five HDO lines, using $x{^{\tiny\rm {HDO}}_{\rm in}} = 1\times10^{-7}$ and $x{^{\tiny\rm {HDO}}_{\rm out}} = 1.5\times10^{-10}$ .
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