Table B.1
Details of individual sources.
| Name | αJ2000 | δJ2000 | Menv (a) | Lbol (a) | Lint (b) | Dist.(c) | Features(d) |
|---|---|---|---|---|---|---|---|
| (M⊙) | (L⊙) | (L⊙) | (pc) | ||||
| Serpens Emb 6 | 18:29:49.81 | 01:15:20.41 | 27.2 | 134.6 | 111.3(*) | 484 | C,E |
| Serpens Emb 8 | 18:29:48.09 | 01:16:43.30 | 12.8 | 7.3 | 13.6(†) | 484 | E |
| Serpens Emb 8(N) | 18:29:48.73 | 01:16:55.61 | 1.3(*) | C | |||
| BHR71 IRS1 | 12:01:36.51 | −65:08:49.31 | 4.6 | 14.7 | 11.8(*) | 200 | E |
| BHR71 IRS2 | 12:01:34.04 | −65:08:47.87 | – | 1.7 | C | ||
| B335 | 19:37:00.91 | 07:34:09.60 | 1.44 | 2.7 | 1.4 | 165 | C,E |
| IRAS 16293A | 16:32:22.87 | −24:28:36.63 | 4.3 | 30.2 | 19(*) | 144 | E |
| IRAS 16293B | 16:32:22.61 | −24:28:32.61 | |||||
| VLA1623A/B | 16:26:26.35 | −24:24:30.55 | 0.8 | 4.4 | 1.2(*) | 144 | E |
| L1448 IRS2 | 03:25:22.41 | 30:45:13.21 | 1.3 | 7.0 | 4.7 | 294 | C,E |
| OMC3 MMS6 | 05:35:23.42 | −05:01:30.53 | 36 | 38.4 | 27.3(*) | 432 | C,E |
| NGC1333 IRAS4A | 03:29:10.55 | 31:13:31.00 | 12.3 | 14.2 | 4.7 | 294 | C,E |
Notes. We scale the masses and luminosities found in the literature to the distances we adopt. (a) Envelope mass Menv and bolometric luminosity Lbol values for Serpens Emb 6 are from observations that encompass the whole Emb 6 core (Enoch et al. 2011; Kristensen et al. 2012). The values calculated for Serpens Emb 8 and Emb 8(N) include both sources together (Enoch et al. 2009, 2011). Tobin et al. (2019) for BHR71. Kurono et al. (2013) and Maury et al. (2018) for B335. Pineda et al. (2012) and Jørgensen et al. (2016) for IRAS 16293A/B. Froebrich (2005) and Karska et al. (2018) for VLA1623A/B. Sadavoy et al. (2014) and Karska et al. (2018) for L1448 IRS2. Karska et al. (2018) and Galametz et al. (2019) for IRAS4A. Chini et al. (1997) and Manoj et al. (2016) for OMC3 MMS6. (b) Internal luminosity. Values with (*)are calculated via the relation from Dunham et al. (2008) using fluxes from archival data of Herschel PACS at 70 μm. Galametz et al. (2019) for Serpens Emb 8. Yang et al. (2017) for BHR 71. Galametz et al. (2018) for B335. Galametz et al. (2019) for L1448 IRS2 and NGC1333 IRAS4A. In the cases where the internal luminosities is quoted for a core that actually consists of two binaries, we index the respective internal luminosity of each protostar with their respective peak in total intensity. (c) Distance reported in the literature. Zucker et al. (2019) for the Perseus, Ophiuchus, Serpens, and Orion sources. Watson (2020) for B335. Seidensticker & Schmidt-Kaler (1989); Bourke (2001) for BHR71. (d) Main features present in the maps of total and/or polarized intensity. C: Cavities, i.e., outflow cavity wall of the bipolar outflow. E: emission from the envelope that is not associated with the bipolar outflow. (†) For Serpens Emb 8 Lbol < Lint, which is unphysical. The two values are derived from studies using two different telescopes: Lbol from BOLOCAM (Enoch et al. 2009, 2011), and Lint from Herschel (Galametz et al. 2019). However, Enoch et al. (2011) mention the source was saturated at 70 μm, so Lbol is likely an underestimate.
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