All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{images/structure.ps}\end{figure}$ Figure 1: Example of the physical structure of a model envelope with the density (solid), temperature (dashed), and abundance (dotted) displayed versus radius. The adopted parameters are $n_0(\rm {H}_2)=10^6$ cm^-3, p=1.5, and $L=2~L_{\rm{\odot}}$ .
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In the text

$\begin{figure} \par\includegraphics[scale=0.6]{images/combined1.ps}\end{figure}$ Figure 2: Contour plots of the integrated water line intensity for the L 483 models, plotted as functions of $X_{\rm {d}}$ and X₀. Left: the o-H₂O 1₁₀-1₀₁ line (557 GHz), showing a strong dependence on $X_{\rm {d}}$ ; middle: the p-H₂¹⁸O 2₀₂-1₁₁ line (995 GHz), showing a clear cut between the dependency on $X_{\rm {d}}$ or X₀, depending on the abundance profile; right: the p-H₂O 5₂₄-4₃₁ line (970 GHz), showing a strong dependence on X₀.
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In the text

$\begin{figure} \par\includegraphics[width=124pt]{images/_abundance_Xd_var_X_0_10... ...raphics[width=124pt]{images/_abundance_Xd_var_X_0_10_5_007_a.ps}\\ \end{figure}$ Figure 3: H₂O spectra for an abundance X₀ of 10^-5 for the 1₁₀-1₀₁ (557 GHz, left), 2₁₂-1₀₁ (1669 GHz middle), and 3₁₂-3₀₃ (1097 GHz right) lines. Lines are shown for $X_{\rm {d}}$ of 10^-6 (solid), 10^-7 (dot), and 10^-8 (dash).
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In the text

$\begin{figure} \par\includegraphics[width=124pt]{images/_abundance_Xd_10_7_X_0_v... ...udegraphics[width=124pt]{images/_abundance_Xd_10_7_X_0_var_007_a.ps}\end{figure}$ Figure 4: H₂O spectra for an abundance $X_{\rm {d}}$ of 10^-7 for the 1₁₀-1₀₁ (557 GHz left), 2₁₂-1₀₁ (1669 GHz middle), and 3₁₂-3₀₃ (1097 GHz right) lines. Lines are shown for X₀ of 10^-4 (solid), 10^-5 (dot), and 10^-6 (dash).
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In the text

$\begin{figure} \par\includegraphics[width=121pt]{images/new_luminosity_001.ps}\i... ...4_a.ps}\includegraphics[width=121pt]{images/new_luminosity_013_a.ps}\end{figure}$ Figure 5: Examples of the luminosity dependence of line profiles for a model with p=1.5, X₀=10^-4, $X_{\rm {d}}=10^{-8}$ , $n_0(\rm {H}_2)=10^6$ cm^-3. From left to right are shown the 1₁₁-0₀₀ 1113 GHz, 2₀₂-1₁₁ 988 GHz, 2₁₁-2₀₂ 752 GHz, and 3₃₁-4₀₄ 1893 GHz lines. Luminosities are 2 (solid), 7 (dot), and 25 (dash) $L_{\odot }$ . These lines reflect the different characteristic line profiles discussed in Sect. 3.4. It can be seen that the line shapes stay the same with increasing luminosity, while the line strengths and depths of the absorption are stronger at higher luminosities.
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In the text

$\begin{figure} \par\includegraphics[width=120pt]{images/new_density_001.ps}\incl... ..._004_a.ps}\includegraphics[width=120pt]{images/new_density_013_a.ps}\end{figure}$ Figure 6: Examples of the density dependence of line profiles for a model with p=1.5, X₀=10^-4, $X_{\rm {d}}=10^{-8}$ , $L=7~L_\odot$ . From left to right are shown the 1₁₁-0₀₀ 1113 GHz, 2₀₂-1₁₁ 988 GHz, 2₁₁-2₀₂ 752 GHz, and 3₃₁-4₀₄ 1893 GHz lines. Densities are $4\times 10^5$ (solid), 10⁶ (dot), and $5 \times 10^6$ (dash) cm^-3. For most lines, the higher density, and thus higher water column, increases the emission, although absorption features are also enhanced. For the 3₃₁-4₀₄ line at 1893 GHz, the dust becomes optically thick at lower temperatures (i.e. larger radii) within the envelope for higher densities.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{images/lum.ps}\end{figure}$ Figure 7: The modeled integrated intensity of the optically thin 2₂₀-2₁₁ 1228 GHz line for X₀=10^-4. Intensities are shown for the 3 different values of $X_{\rm {d}}$ for a constant density of 10⁶ cm^-3 ( left) and for a constant luminosity of 7 $L_{\odot }$ ( right). Power laws with indices of 0.8 ( left) and 0.75 ( right) are over-plotted. In the right panel, at $5 \times 10^6$ cm^-3, this line becomes optically thick for $X_{\rm {d}}=10^{-6}$ , with its intensity dropping below the relation.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=150pt]{images/duststructure_... ...udegraphics[angle=270,width=150pt]{images/duststructure_highdens.ps}\end{figure}$ Figure 8: Cartoon of protostellar envelope models. For two different models, the $\tau =1$ surfaces at 557 and 1669 GHz for the dust are shown. A model with low-density ( $n_0({\rm{H}_2})=4~~ \times 10^5$ cm^-3, $M=0.15~M_{\rm{\odot}}$ ) is shown in the top panel; here the 557 GHz line contour is absent, since dust is optically thin throughout the envelope at this frequency. A model with a high density ( $n_0({\rm {H}_2})=5\times 10^6$ cm^-3, $M=1.93~M_{\rm{\odot}}$ ) is shown in the bottom panel. The long-dashed line indicates the T=100 K contour. In both models, the 1669 GHz line is unable to probe the inner warm region, regardless of its own optical depth, since the dust $\tau =1$ surface lies far outside the T=100 K radius.
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In the text

$\begin{figure} \par\includegraphics[width=128pt]{images/dust_ortho.ps}\includegr... ...ortho_002.ps}\includegraphics[width=128pt]{images/dust_ortho_007.ps}\end{figure}$ Figure 9: Example spectra of the 1₁₀-1₀₁ 557 GHz line ( left), 2₁₂-1₀₁ 1669 GHz line ( middle) and 3₁₂-3₀₃ 1097 GHz line ( right) for a model with p=1.5, $L=7~L_{\rm{\odot}}$ and $n_{\rm {H}_2}=1\times 10^6$ cm^-3. The solid lines represent the spectra with no dust within the envelope, while the dotted line shows the same line with dust included in the model. The influence of dust can be clearly seen. The peaks of the optically thick lines are reduced in strength, the depth of the absorption changes, and the optically thin lines are significantly pumped by far-infrared radiation.
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In the text

$\begin{figure} \par\includegraphics[width=128pt]{images/turb_ortho_001.ps}\inclu... ...ortho_002.ps}\includegraphics[width=128pt]{images/turb_ortho_007.ps}\end{figure}$ Figure 10: Example spectra of the 1₁₀-1₀₁ 557 GHz line ( left), 2₁₂-1₀₁ 1669 GHz line ( middle), and 3₁₂-3₀₃ 1097 GHz line ( right) for a model with p=1.5, $L=7~L_{\rm{\odot}}$ , and $n_{\rm {H}_2}=1\times 10^6$ cm^-3. The dotted line is for a model with $\Delta V= 0.83$ km s^-1. The solid line for $\Delta V= 1.67$ km s^-1, and the dashed line for $\Delta V= 3.34$ km s^-1. The large effect of micro-turbulence for all lines can be seen clearly.
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In the text

$\begin{figure} \par\includegraphics[width=140pt]{pictures/p31_c.ps}\includegraph... ...s}\includegraphics[width=140pt]{pictures/p1_c.ps}\hspace*{2.5cm}} \end{figure}$ Figure 11: Contour plots of the integrated intensity of the L 483 models as a function of inner (X₀) and outer ( $X_{\rm {d}}$ for all para-H₂O lines. Upper row ( from left to right): 5₂₄-4₃₁, 4₂₂-4₁₃ and 4₂₂-3₃₁. Middle row: 3₃₁-4₀₄, 2₂₀-2₁₁ and 2₁₁-2₀₂. Lower row: 2₀₂-1₁₁ and 1₁₁-0₀₀.
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In the text

$\begin{figure} \par\includegraphics[width=140pt]{pictures/o9_c.ps}\includegraphi... ...t]{pictures/o2_c.ps}\includegraphics[width=140pt]{pictures/o1_c.ps} \end{figure}$ Figure 12: Contour plots of the integrated intensity of the L 483 models as a function of inner (X₀) and outer ( $X_{\rm {d}}$ for all ortho-H₂O lines. Upper row (from left to right): 3₂₁-3₁₂, 3₁₂-3₀₃ and 3₁₂-2₂₁. Lower row: 2₂₁-2₁₂, 2₁₂-1₀₁ and 1₁₀-1₀₁.
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In the text

$\begin{figure} \par\includegraphics[width=140pt]{pictures/18p31_c.ps}\includegra... ...}\includegraphics[width=140pt]{pictures/18p1_c.ps}\hspace*{2.5cm}}\end{figure}$ Figure 13: Contour plots of the integrated intensity of the L 483 models as a function of inner (X₀) and outer ( $X_{\rm {d}}$ for all para-H₂¹⁸O lines. Upper row ( from left to right): 5₂₄-4₃₁, 4₂₂-4₁₃ and 4₂₂-3₃₁. Middle row: 3₃₁-4₀₄, 2₂₀-2₁₁ and 2₁₁-2₀₂. Lower row: 2₀₂-1₁₁ and 1₁₁-0₀₀.
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In the text

$\begin{figure} \par\includegraphics[width=140pt]{pictures/18o9_c.ps}\includegrap... ...ictures/18o2_c.ps}\includegraphics[width=140pt]{pictures/18o1_c.ps} \end{figure}$ Figure 14: Contour plots of the integrated intensity of the L 483 models as a function of inner (X₀) and outer ( $X_{\rm {d}}$ for all ortho-H₂¹⁸O lines. Upper row ( from left to right): 3₂₁-3₁₂, 3₁₂-3₀₃ and 3₁₂-2₂₁. Lower row: 2₂₁-2₁₂, 2₁₂-1₀₁ and 1₁₀-1₀₁.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{images/structure.ps}\end{figure}$	Figure 1: Example of the physical structure of a model envelope with the density (solid), temperature (dashed), and abundance (dotted) displayed versus radius. The adopted parameters are $n_0(\rm {H}_2)=10^6$ cm^-3, p=1.5, and $L=2~L_{\rm{\odot}}$ .
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$\begin{figure} \par\includegraphics[width=124pt]{images/_abundance_Xd_var_X_0_10... ...raphics[width=124pt]{images/_abundance_Xd_var_X_0_10_5_007_a.ps}\\ \end{figure}$	Figure 3: H₂O spectra for an abundance X₀ of 10^-5 for the 1₁₀-1₀₁ (557 GHz, left), 2₁₂-1₀₁ (1669 GHz middle), and 3₁₂-3₀₃ (1097 GHz right) lines. Lines are shown for $X_{\rm {d}}$ of 10^-6 (solid), 10^-7 (dot), and 10^-8 (dash).
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$\begin{figure} \par\includegraphics[width=124pt]{images/_abundance_Xd_10_7_X_0_v... ...udegraphics[width=124pt]{images/_abundance_Xd_10_7_X_0_var_007_a.ps}\end{figure}$	Figure 4: H₂O spectra for an abundance $X_{\rm {d}}$ of 10^-7 for the 1₁₀-1₀₁ (557 GHz left), 2₁₂-1₀₁ (1669 GHz middle), and 3₁₂-3₀₃ (1097 GHz right) lines. Lines are shown for X₀ of 10^-4 (solid), 10^-5 (dot), and 10^-6 (dash).
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$\begin{figure} \par\includegraphics[width=140pt]{pictures/p31_c.ps}\includegraph... ...s}\includegraphics[width=140pt]{pictures/p1_c.ps}\hspace*{2.5cm}} \end{figure}$	Figure 11: Contour plots of the integrated intensity of the L 483 models as a function of inner (X₀) and outer ( $X_{\rm {d}}$ for all para-H₂O lines. Upper row ( from left to right): 5₂₄-4₃₁, 4₂₂-4₁₃ and 4₂₂-3₃₁. Middle row: 3₃₁-4₀₄, 2₂₀-2₁₁ and 2₁₁-2₀₂. Lower row: 2₀₂-1₁₁ and 1₁₁-0₀₀.
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$\begin{figure} \par\includegraphics[width=140pt]{pictures/o9_c.ps}\includegraphi... ...t]{pictures/o2_c.ps}\includegraphics[width=140pt]{pictures/o1_c.ps} \end{figure}$	Figure 12: Contour plots of the integrated intensity of the L 483 models as a function of inner (X₀) and outer ( $X_{\rm {d}}$ for all ortho-H₂O lines. Upper row (from left to right): 3₂₁-3₁₂, 3₁₂-3₀₃ and 3₁₂-2₂₁. Lower row: 2₂₁-2₁₂, 2₁₂-1₀₁ and 1₁₀-1₀₁.
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$\begin{figure} \par\includegraphics[width=140pt]{pictures/18p31_c.ps}\includegra... ...}\includegraphics[width=140pt]{pictures/18p1_c.ps}\hspace*{2.5cm}}\end{figure}$	Figure 13: Contour plots of the integrated intensity of the L 483 models as a function of inner (X₀) and outer ( $X_{\rm {d}}$ for all para-H₂¹⁸O lines. Upper row ( from left to right): 5₂₄-4₃₁, 4₂₂-4₁₃ and 4₂₂-3₃₁. Middle row: 3₃₁-4₀₄, 2₂₀-2₁₁ and 2₁₁-2₀₂. Lower row: 2₀₂-1₁₁ and 1₁₁-0₀₀.
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$\begin{figure} \par\includegraphics[width=140pt]{pictures/18o9_c.ps}\includegrap... ...ictures/18o2_c.ps}\includegraphics[width=140pt]{pictures/18o1_c.ps} \end{figure}$	Figure 14: Contour plots of the integrated intensity of the L 483 models as a function of inner (X₀) and outer ( $X_{\rm {d}}$ for all ortho-H₂¹⁸O lines. Upper row ( from left to right): 3₂₁-3₁₂, 3₁₂-3₀₃ and 3₁₂-2₂₁. Lower row: 2₂₁-2₁₂, 2₁₂-1₀₁ and 1₁₀-1₀₁.
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