Table 2
CO rotational temperature, the number of emitting molecules, and total line luminosities of CO and [O I] lines toward dense cores in Gy 3–7 and IM YSOs from Matuszak et al. (2015).
| Source | Trot(K)(a) | log𝒩tot(a) | LCO(warm)(b) | L[O I]63μm (10−3L⊙) | L[O I]45 μm |
|---|---|---|---|---|---|
| Dense cores in Gy 3–7 | |||||
| Core A | 305 ± 85 | 50.41 ± 0.34 | 73.31 ± 19.69 | 92.69 ± 5.01 | 8.38 ± 0.29 |
| Core B | 155 ± 20 | 50.96 ± 0.24 | 30.47 ± 6.10 | 76.17 ± 5.37 | 6.15 ± 0.37 |
| IM YSOs in the inner Milky Way | |||||
| AFGL 490(c) | 255 ± 25 | 51.11 ± 0.13 | 225.17 ± 19.85 | 336.65 ± 1.47 | 29.56 ± 0.24 |
| L1641 | 270 ± 35 | 50.06 ± 0.17 | 24.31 ± 2.74 | 14.69 ± 0.14 | 1.20 ± 0.05 |
| NGC 2071 | 295 ± 20 | 51.23 ± 0.10 | 425.38 ± 26.11 | 312.72 ± 0.91 | 21.59 ± 0.13 |
| Vela 17 | 215 ± 25 | 51.08 ± 0.17 | 125.56 ± 15.44 | 369.84 ± 1.33 | 77.85 ± 0.21 |
| Vela 19 | 255 ± 20 | 50.66 ± 0.10 | 86.00 ± 9.27 | 130.69 ± 0.70 | 13.60 ± 0.09 |
| NGC 7129 | 295 ± 35 | 50.84 ± 0.14 | 187.26 ± 19.16 | 66.03 ± 0.78 | 3.13 ± 0.88 |
Notes. (α)Trot and 𝒩tot calculated using only CO 14–13, CO 16-15, CO 18–17, and CO 22–21 transitions for more direct comparisons with the cores in Gy 3–7. (b)The CO line luminosity in the “warm” component is obtained using all transitions reported in Matuszak et al. (2015) with Jup from 14 to 24 (see Sect. 4.2). (c)We adopted the new distance of 0.97 kpc toward this source when calculating Trot, 𝒩tot, and luminositiy of CO and [OI] lines (see Table D.2 and references therein).
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