Table 4
Properties of the cores associated with methanol masers.
| GLOSTAR | Common | ΔVD | ΔVB | Lmaser, D | Lmaser, B | Size | Mcore | Tcore | LFIR | LBol |
|---|---|---|---|---|---|---|---|---|---|---|
| name | name | (km s−1) | (km s−1) | (L⊙) | (L⊙) | (″) | (M⊙) | (K) | (L⊙) | (L⊙) |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
| G76.0932+0.1580 | – | 1.3 | 1.6 | 5.8 × 10−9 | 5.9 × 10−9 | 18 | 27 ± 3 | 20.4 ± 0.9 | 189 | 227 |
| G76.8437+0.1233 | – | 2.2 | 0.5 | 3.8 × 10−8 | 1.0 × 10−9 | 25 | 12 ± 2 | 16.0 ± 0.7 | 19 | 26 |
| G78.8870+0.7087 | AFGL2591 | 0.7 | 0.9 | 2.3 × 10−8 | 2.4 × 10−8 | 24 | 937 ± 72 | 30.2 ± 1.9 | 67 750 | 66 262 |
| G78.9690+0.5410 | IRAS 20286+3959 | 1.4 | 1.4 | 1.3 × 10−8 | 1.4 × 10−8 | 22 | 72 ± 9 | 13.0 ± 0.4 | 33 | 42 |
| G78.9884+0.2211(a) | – | 3.6 | 0.7 | 1.8 × 10−8 | 2.9 × 10−9 | 25 | 8 ± 1 | 21.3 ± 1.2 | 69 | 176 |
| G79.7358+0.9904 | IRAS 20290+4052 | 3.4 | 3.2 | 2.4 × 10−7 | 2.4 × 10−7 | 19 | 42 ± 4 | 17.7 ± 0.5 | 122 | 233 |
| G80.8617+0.3834 | DR20 | 4.7 | 1.4 | 1.0 × 10−7 | 3.7 × 10−8 | 23 | 122 ± 11 | 20.9 ± 0.8 | 972 | 1328 |
| G81.7219+0.5711 | DR21(OH) | 2.3 | 2.5 | 5.2 × 10−8 | 4.9 × 10−8 | 16 | 930 ± 140 | 20.9 ± 1.3 | 7344 | 7299 |
| G81.7444+0.5910 | W75S-FIR1 | 2.2 | 2.2 | 1.3 × 10−7 | 1.3 × 10−7 | 11 | 74 ± 5 | 21.9 ± 0.6 | 776 | 1487 |
| G81.7523+0.5908 | W75S-FIR2 | 5.4 | 5.4 | 1.8 × 10−7 | 2.0 × 10−7 | 9 | 298 ± 34 | 16.4 ± 0.6 | 552 | 955 |
| G81.7655+0.5972 | CygX-N53 | 1.3 | 1.6 | 2.3 × 10−8 | 2.2 × 10−8 | 11 | 325 ± 27 | 14.5 ± 0.3 | 294 | 221 |
| G81.8713+0.7807 | W75N(B) | 10.3 | 7.2 | 5.8 × 10−6 | 5.8 × 10−6 | – | 1020 ± 91 | 27.3 ± 1.3 | 40 588 | 32 930 |
| G82.3079+0.7296 | – | 2.3 | 1.3 | 1.2 × 10−7 | 1.3 × 10−7 | 16 | 24 ± 3 | 19.7 ± 0.8 | 139 | 183 |
Notes. Columns 1 and 2 report the maser name, which is based on Galactic coordinates, and its common label; Cols. 3 and 4 are the velocity ranges of the maser emission in D- and B-configurations; Cols. 5 and 6 are the maser integrated luminosities; Col. 7 is the deconvolved size at 160 μm band, where the dust is optically thin. It corresponds to the intensity-weighted diameter given by
, where ri is the distance of the ith pixel to the center of the source and Ai is the pixel intensity (Purcell et al. 2013); Cols. 8–11 are the mass, temperature, integrated FIR luminosity, and bolometric luminosity of the associated dust cores. (a)The mass, FIR luminosity, and bolometric luminosity of this core must be rescaled to 347 M⊙, 3093 L⊙, and 6237 L⊙, respectively,for a distance of 9.35 kpc (see Sect. 4.4).
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