Table 4
High-mass YSOs hosting hot cores in W51 Main.
| Source | RA (J2000) | Dec (J2000) | VLSR | Trota | N | Rcoreb | Mgasc | Outflow | Disk | |||
| name | (h:m:s) | (°:′:′′) | (km s-1) | (K) | (cm-3) | (AU) | (M⊙) | (Y/N) | (Y/N) | |||
|
|
||||||||||||
| W51e2-W | 19:23:43.9096 | 14:30:34.551 | 57.4 | 174 | 6.9 × 1013 | 320 | 5 | N | Y | |||
| W51e2-E | 19:23:43.9618 | 14:30:34.558 | 56.4 | 173 | 5.1 × 107 | 2430 | 18 | Y | N | |||
| W51e2-NW | 19:23:43.8900 | 14:30:35.630 | 55.2 | 144 | 1.6 × 107 | 4460 | 32 | Y | N | |||
| W51e8 | 19:23:43.9073 | 14:30:28.197 | 59.9 | 204 | 2.7 × 106 | 10200 | 69 | Y | N | |||
Notes.
In the case of emission lines, rotational temperatures are calculated in the optically thin assumption, therefore, the quoted values are lower limits to true kinetic temperature of the gas.
The radius is defined by the area where we integrated the spectra (see Table 2 and Sect. 3.2) except for W51e2-W, for which we used the deconvolved size of the compact continuum emission quoted by Shi et al. (2010a).
The gas mass is calculated in a sphere of radius Rcore for a given volume density ρ. For the emission, with poor estimates of the opacity, this is calculated in the optically thin assumption. Therefore, the quoted values are lower limits to the gas mass.The mass for absorption should instead be regarded as an upper limit (since we do not know the actual size of the HC HII region). These mass estimates assume [NH3]/[H2] = 10-7.
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