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Table 2:

Best-fit radiative transfer model parameters for Orion H$_2^{\;18}$O emission components.
  $\Delta v$ $T_{\rm gas}$ $n({\rm H_2})$ $T_{\rm dust}$ $^{\dagger }$   N(ortho/para-H$_2^{\;18}$O)  Total Inferred 
Source (km s-1) (K) (cm-3) (K) $\theta_{\rm source}$ (cm-2) H2O Abundance $^{\ddagger}$
Extended warm gas 2-8   75 2 $\times$ 106 30 20 $^{\prime\prime}$   7.4 $\times$ 1015 (ortho) / 2.0 $\times$ 1015 (para)   1.6 $\times$ 10-5
Plateau  20-34    188     2 $\times$ 106   113.6 24 $^{\prime\prime}$ 1.2 $\times$ 1016 (ortho) / 2.8 $\times$ 1015 (para) 7.4 $\times$ 10-5
Hot core 10  150  1 $\times$ 107  180    5 $^{\prime\prime}$ 1.5 $\times$ 1016 (ortho) / 5.0 $\times$ 1015 (para) 1.0 $\times$ 10-5

Notes.  $^{(\dagger)}$ Greybody fit to the Orion continuum of the form:  $B_{\tilde{\nu~}}(T_{\rm dust}) \times\ (0.0233~\tilde{\nu})^{0.486}$, where $\tilde{\nu}$ is wavelength in wavenumbers. $^{(\ddagger)}$ Assumes 16O/18O = 500 and N(H$_2)~=\:$3 $\times$ 1023, 1 $\times$ 1023, and 1 $\times$ 1024 cm-2 in a 30 $^{\prime\prime}$ beam for the extended ridge, plateau, and hot core, respectively (Blake et al. 1987).


Source LaTeX | All tables | In the text

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