Table 1
Properties of detected Class 0 and I protostellar sources.
| Source | Lbol L⊙ | Lint L⊙ | Tbol K | Class | Mprot M⊙ | Cloud | Nearest protostar sep. au | FAUST line paper |
|---|---|---|---|---|---|---|---|---|
| RCrA IRS7B a,b | 5.4 | 7.4 | 122 | I | 2.1–3.2 (a) | RCrA | 103 (a–b) | Sabatini et al. (2024) |
| RCrA SMM1C | 4.7 | <0.6 | 27 | 0 | − | RCrA | 803 (IRS7A) | " |
| RCrA SMM2 a, ba | 0.6 | 0.7 | 164 | I | − | RCrA | 14 (a-b) | " |
| RCrA IRS7A | 13.9 | 12.9 | 125 | I | − | RCrA | 803 (SMM1C) | " |
| CrA-24a | 0.1 | − | 370 | I | − | RCrA | 3846 (SMM1C) | " |
| CXO 34 | − | − | − | I | − | RCrA | 1069 (IRS7B b) | " |
| Elias 29 | 28.9 | 4.9 | 391 | I | 0.8–1 | Oph | >7000c | Oya et al. (2025) |
| VLA 1623 A,B | 3.6 | 1.1 | 35 | 0 | 0.3–0.5 (Aa+Ab) | Oph | 30 (Aa–Ab) | Ohashi et al. (2022a) |
| 0.4–1.7 (B) | 146 (Ab–B) | Codella et al. (2024) | ||||||
| VLA 1623 W | 0.14 | 0.3 | 84 | I | 0.5 | Oph | 1271 (VLA 1623B) | Mercimek et al. (2023) |
| Oph A SM1 a | <1 | <1 | 40b | 0 | − | Oph | 2686 (VLA1623-N1 c) | − |
| IRAS 16293 A,B | 29 | 19.2 | 45 | 0 | 2–4 (A1+A2) | Oph | 52 (A1–A2) | − |
| 0.2–0.8 (B) | 734 (A2–B) | − | ||||||
| Oph IRS 63 | 1.2 | 0.7 | 351 | I | 0.5 | Oph | >7000 c | Podio et al. (2024) |
| L1551 IRS5 N,S | 26.6 | 21.4 | 106 | I | 1–1.7 (N+S) | Tau | 54 (N–S) | Bianchi et al. (2020) |
| Durán et al. (2025) |
Notes. RCrA IRS7B a,b: Sandell et al. (2021); Ohashi et al. (2023a); RCrA SMM1C, RCrA IRS7B SMM2, RCrA IRS7A: Sandell et al. (2021); RCrA CrA-24: Dunham et al. (2015); CXO 34: Peterson et al. (2011); Elias 29: Green et al. (2013); Oya et al. (2019); VLA 1623 A/B: Green et al. (2013); Hsieh et al. (2020); Ohashi et al. (2022a); VLA 1623 W: Dunham et al. (2015); Murillo et al. (2018); Mercimek et al. (2023), SM1: Kawabe et al. (2018); Friesen et al. (2018) IRAS 16293 A/B: Dunham et al. (2015); Jørgensen et al. (2016); Maureira et al. (2020); Oya et al. (2018); IRS 63: Lommen et al. (2008); Flores et al. (2023); L1551 IRS5: Green et al. (2013); Hernández Garnica et al. (2024). Second to last column provides the information about the projected separation to the closest protostar.
(a)Observed only at 3 mm. (b)This value is for reference only and comes from a modified blackbody fit to the SED (Kawabe et al. 2018). (c)No other protostar within the ALMA 3 mm field of view. (d)Chen & Hirano (2018).
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