All Tables

Table 1: Parameters for low-mass protostellar envelopes.
Table 2: The masses and inner radii of the model envelopes.
Table 3: Key water lines observable with Herschel HIFI and PACS.
Table 4: Integrated intensities, $\int T_{\rm{MB}}{\rm d}V$ [K km s^-1], for H₂O and H₂¹⁸O lines for L 483 models with various abundances. Negative values indicate strong (self-) absorbed lines.
Table 5: Peak temperatures [K] of H₂O lines for L 483 models of various abundances. Negative values primarily indicate absorption into the dust continuum.
Table 6: Integrated intensities, $\int T_{\rm{MB}}\Delta V$ [K km s^-1], for H₂O lines in the wide parameter grid for an abundance combination of X₀=10^-4 and $X_{\rm d}=10^{-7}$ .
Table 7: Integrated intensity and peak brightness of lines with and without dust for a model with p=1.5, $L=7~L_{\rm{bol}}$ and $n_{\rm {H}_2}=1\times 10^6$ cm^-3.
Table 8: The dust properties at selected water line frequencies for four typical models. The column density $N_{\rm {H_2}}$ required to produce $\tau =1$ for the dust at each frequency is given with the corresponding radii and temperatures.
Table 9: Integrated intensities, $\int T_{\rm{MB}}\Delta V$ [K km s^-1], for H₂O lines in the wide parameter grid for all abundances. Ortho lines for p=1.5.
Table 10: Integrated intensities, $\int T_{\rm{MB}}\Delta V$ [K km s^-1], for H₂O lines in the wide parameter grid for all abundances, Ortho lines for p=2.0.
Table 11: Integrated intensities, $\int T_{\rm{MB}}\Delta V$ [K km s^-1], for H₂O lines in the wide parameter grid for all abundances. Para lines for p=1.5.
Table 12: Integrated intensities, $\int T_{\rm{MB}}\Delta V$ [K km s^-1], for H₂O lines in the wide parameter grid for all abundances for para p =2.0.