Table D.2
FIR line cooling luminosity of the sample in the Milky Way (MW), LMC, and SMC used to compare with results of this study
| Source | D | D Ref. | RGCa | Zb | log(Lbol/L⊙) | Lbol Ref. | LCOc | L[O I]d | LCO/L[O I] | Llines Ref. |
|---|---|---|---|---|---|---|---|---|---|---|
| (kpc) | (kpc) | (Z⊙) | (10−2L⊙) | (10−2L⊙) | ||||||
| LMC YSOs | ||||||||||
| IRAS04514–6931 | 50.0 ± 1.1 | 1 | – | 0.4 | 4.8 | 16 | 5.3 | 8.8 | 0.605 | 16 |
| N113 YSO3 | 50.0 ± 1.1 | 1 | – | 0.4 | 5.4 | 16 | 29.5 | 57.8 | 0.511 | 16 |
| SAGE045400.9–691151.6 | 50.0 ± 1.1 | 1 | – | 0.4 | 5.1 | 16 | 14.6 | 29.2 | 0.5 | 16 |
| SAGE051351.5–672721.9 | 50.0 ± 1.1 | 1 | – | 0.4 | 5.1 | 16 | 5.5 | 15.4 | 0.357 | 16 |
| SAGE052202.7–674702.1 | 50.0 ± 1.1 | 1 | – | 0.4 | 4.5 | 16 | 4.3 | 9.4 | 0.459 | 16 |
| SAGE052212.6–675832.4 | 50.0 ± 1.1 | 1 | – | 0.4 | 5.5 | 16 | 14.9 | 25.4 | 0.585 | 16 |
| SAGE053054.2–683428.3 | 50.0 ± 1.1 | 1 | – | 0.4 | 4.9 | 16 | 6.8 | 5.4 | 1.24 | 16 |
| ST01 | 50.0 ± 1.1 | 1 | – | 0.4 | 4.6 | 16 | 7.1 | 8.5 | 0.833 | 16 |
| N113 YSO1 | 50.0 ± 1.1 | 1 | – | 0.4 | 5.4 | 16 | 47.5 | 47.5 | 1 | 16 |
| SMC YSOs | ||||||||||
| IRAS00464–7322 | 62.1 ± 2.0 | 2 | – | 0.2 | 4.1 | 16 | 3.0 | 2.8 | 1.077 | 16 |
| IRAS00430–7326 | 62.1 ± 2.0 | 2 | – | 0.2 | 4.9 | 16 | 1.9 | 10.9 | 0.176 | 16 |
| N81 | 62.1 ± 2.0 | 2 | – | 0.2 | 4.7 | 16 | 2. 4 | 36.4 | 0.067 | 16 |
| SMC012407-730904 | 62.1 ± 2.0 | 2 | – | 0.2 | 5.3 | 16 | 6.8 | 71.2 | 0.096 | 16 |
| MW IM YSOs | ||||||||||
| AFGL 490 | 0.97 ± 0.40 | 3 | 9.12 | 0.7 | 3.7 | 17 | 24.7 ± 2.5 | 36.6 ± 0.2 | 0.7 ± 0.1 | 32 |
| L 1641 | 0.428 ± 0.010 | 4 | 8.69 | 0.8 | 1.8 | 18 | 2.7 ± 0.4 | 1.6 ± 0.1 | 1.7 ± 0.3 | 32 |
| NGC 2071 | 0.422 ± 0.050 | 4 | 8.71 | 0.8 | 2.7 | 19 | 44.8 ± 4.3 | 33.4 ± 0.1 | 1.3 ± 0.1 | 32 |
| Vela 17 | 0.7 | 5 | 8.44 | 0.8 | 2.9 | 20 | 13.2 pm 2.0 | 44.8 ± 0.1 | 0.3 ± 0.1 | 32 |
| Vela 19 | 0.7 | 5 | 8.45 | 0.8 | 2.9 | 5 | 9.7 ± 2.0 | 14.4 ± 0.1 | 0.7 ± 0.1 | 32 |
| NGC 7129 | 1.25 | 6 | 8.75 | 0.8 | 2.6 | 21 | 20.9 ± 3.0 | 6.9 ± 0.1 | 3.0 ± 0.4 | 32 |
| MW HM YSOs | ||||||||||
| G327-0.6 | 3.3 | 7 | 5.84 | 1.0 | 4.7 | 22 | 180 ± 60 | 30 ± 10 | 6.0 ± 2.8 | 33 |
| W51N-e1 | 5.1 ± 2.2 | 8 | 12.42 | 0.5 | 5.0 | 23 | 2530 ± 680 | 760 ±180 | 3.3 ± 1.2 | 33 |
| DR21(OH) | 1.50 ± 0.08 | 9 | 8.26 | 0.8 | 4.1 | 24 | 120 ± 30 | 9 ± 3 | 13.3 ± 5.6 | 33 |
| W33A | 2.40 ± 0.16 | 10 | 6.02 | 1.0 | 4.6 | 25 | 60 ± 20 | 5 ± 2 | 12.0 ± 6.2 | 33 |
| G34.26+0.15 | 3.30 | 11 | 5.91 | 1.0 | 5.5 | 26 | 770 ± 240 | 190 ± 50 | 4.1 ± 1.7 | 33 |
| NGC6334I | 1.7 ± 0.3 | 12 | 6.66 | 0.9 | 5.4 | 27 | 340 ±100 | 4 ± 3 | 85.0 ± 68.5 | 33 |
| NGC7538-IRS1 | 2.7 ± 0.1 | 13 | 9.66 | 0.7 | 5.1 | 28 | 280 ± 50 | 1100 ± 250 | 0.2 ± 0.1 | 33 |
| AFGL2591 | 3.3 ± 0.08 | 9 | 8.36 | 0.9 | 5.3 | 29 | 160 ± 50 | 340 ± 90 | 0.5 ± 0.2 | 33 |
| W3-IRS5 | 2.00 ± 0.07 | 14 | 9.83 | 0.7 | 5.2 | 30 | 1050 ± 250 | 420 ± 10 | 2.5 ± 0.8 | 33 |
| G5.89-0.39 | 1.30 ± 0.09 | 15 | 7.05 | 0.9 | 4.7 | 31 | 390 ± 90 | 370 ± 90 | 1.1 ± 0.4 | 33 |
References: (1) Pietrzyński et al. (2013), (2) Graczyk et al. (2014)), (3) Purser et al. (2021), (4) Wilson et al. (2005), (5) Liseau et al. (1992),(6) Shevchenko & Yakubov (1989), (7) Minier et al. (2009), (8) Xu et al. (2009), (9) Rygl et al. (2012), (10) Immer et al. (2013), (11) Kuchar & Bania (1994), (12) Neckel (1978), (13) Moscadelli et al. (2009), (14) Hachisuka et al. (2006), (15) Motogi et al. (2011), (16) Oliveira et al. (2019),(17) Navarete et al. (2015), (18) Stanke et al. (2000), (19) Butner et al. (1990), (20) Giannini et al. (2005), (21)Johnstone et al. (2010), (22) Urquhart et al. (2012), (23) van Dishoeck et al. (2011),(24) Jakob et al. (2007), (25) Faúndez et al. (2004), (26) Hatchell & van der Tak (2003), (27) Sandell (2000), (28) Sandell & Sievers (2004), (29) van der Tak et al. (1999), (30) Ladd et al. (1993), (31) van der Tak (2012), (32) Matuszak et al. (2015), (33) Karska et al. (2014a).
a Galactocentric radius toward the sources in the Milky Way is calculated using the information from their coordinate and distance to the Sun, assuming the distance from the Sun to the Galactic center is 8.34 kpc.
b Metallicity towards the sources in the Milky Way is calculated using the relation of O/H gradients inferred from the HII regions: 12 + log (O/H) = -0.0446RGC + 8.962 (Balser et al. 2011).
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