Table D.1
Properties of Class 0 and I protostars within the field of view.
| Source | Class | Rdisk(a) (au) | PAout flow(b) (deg) | Other Name | Ref. |
|---|---|---|---|---|---|
| NGC 1333 IRAS4A1(c) | 0 | 49.7 | 19.2 | Per-emb-12 | (1, 5) |
| NGC 1333 IRAS4A2(c) | 0 | – | 20 | Per-emb-12 | (1, 7) |
| NGC 1333 IRAS4B(c) | 0 | – | 176 | Per-emb-13 | (1, 2, 5) |
| NGC 1333 IRAS4B2(c) | 0 | – | 76 | Per-emb-13 | (1, 8) |
| NGC 1333 IRAS2B | I | – | 24 | Per-emb-36 | (1, 9) |
| NGC 1333 IRAS4C | 0 | 37.2 | 96 | Per-emb-14 | (2, 6) |
| SVS13 VLA4A(d) | 0/I | 12 | 8 | SVS13A, Per-emb-44 | (3, 4) |
| SVS13 VLA4B(d) | 0/I | 9 | −50 | SVS13A, Per-emb-44 | (3, 4) |
| SVS13 VLA17 | 0 | 31.7 | 170 | SVS13B | (2, 5) |
| SVS13C | 0 | 42.9 | 8 | – | (1, 4) |
| Per-emb-15 | 0 | – | −35 | SK14 | (4) |
| Per-emb-3 | 0 | – | 97 | – | (1, 9) |
References. (1) Segura-Cox et al. (2018), (2) Segura-Cox et al. (2016), (3) Diaz-Rodriguez et al. (2022), (4) Plunkett et al. (2013), (5) Lee et al. (2016), (6) Zhang et al. (2018), (7) Chuang et al. (2021), (8) Hull et al. (2014), (9) Stephens et al. (2017)
Notes. (a)The disk radius measurements are dust based, and they were recomputed to the same 300 pc distance, if needed. (b)Outflow PA was measured using the red lobe from due east from north. (c)These objects form a binary system but do not share circumbinary material. (d)These objects belong to a close binary system surrounded by circumbinary material or disk.
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