Table 3
Detection of outflows and jets as traced by CO (2−1), SO (56 − 45), and SiO (5−4) lines in the CALYPSO sample of Class 0 and I protostars.
| Source | Lint | COMs(a) | Disk(b) | Outflow/Jet(c) | PAjet/outflow (d) | ||
|---|---|---|---|---|---|---|---|
| (L⊙) | CO | SO | SiO | (°) | |||
| Class 0 | |||||||
| L1521-F | 0.035(0.01) | Y | + 260(B)(e) | ||||
| IRAM04191 | 0.05(0.01) | Y | + 20(R) | ||||
| (IRAS4B2) | <0.16 | Y* | Y* | Y* | − 99 | ||
| SerpS-MM22 | 0.4(0.2) | Y | + 230 | ||||
| L1527 | 0.9(0.1) | Y | Y | D | − 90 (e) | ||
| GF9-2 | 1.7 | Y | D/E? | 50 | |||
| SerpM-S68Nb | 1.8(0.2) | Y* | Y | + 108 | |||
| SerpM-SMM4a | 2.2(0.2) | Y | 0(B)(e) | ||||
| IRAS4B1 | 2.3(0.3) | Y | y | Y | Y | Y | + 165 |
| (SerpM-SMM4b) | <2.6 | Y | Y | Y | + 10(B)/ + 135(R) | ||
| SVS13B | 3.1(1.6) | y | Y* | Y* | Y | + 167 | |
| L1448-NB1 (+NB2) | 3.9 | y | Y | Y | Y | − 80 | |
| L1157 | 4.0(0.4) | y | Y | D/E? | Y | + 163 | |
| IRAS4A1 | <4.7 | Y | Y | Y | + 180 | ||
| IRAS4A2 | 4.7(0.5) | Y | Y | Y | Y | + 182 | |
| L1448-2A (+2Ab) | 4.7(0.5) | Y | D/E? | Y* | + 118 (f) | ||
| L1448-C | 11(1) | Y | Y | Y | Y | Y | − 17 |
| SerpM-S68N | 11(2) | y | Y | Y | Y | − 45 | |
| SerpS-MM18a | 13(4) | Y | y | Y | Y | Y | + 188 |
| (SerpS-MM18b) | 16(4) | Y | D/E? | + 205(R) | |||
| IRAS2A1 | 47(5) | Y | y | Y | Y | Y | + 205 |
| Class I | |||||||
| L1448-CS | 3.6 | Y | Y | Y | + 60(R) | ||
| L1448-NA | 6.4(0.6) | Ye | + 40 (e) | ||||
| SVS13A (+VLA3) | 44(5) | Y | Y | Y | Y | + 155 | |
Notes. (a) Emission from three (“y”) or more than three (“Y”) complex organic molecules (COMs) based on the CALYPSO survey (Belloche et al. 2020). (b) “y” indicates disk candidates, i.e., sources which show a velocity gradient perpendicular to the jet axis (within ± 45°) at a few hundred au scales in one of the disk tracers (13CO (2− 1), C18O (2− 1), and SO (56 −45)). “Y” indicates the detection of a Keplerian rotating disk (based on the CALYPSO survey, see Table 3 by Maret et al. 2020). (c) “Y” indicates outflow/jet blue- and/or red-shifted emission detected in CO (2− 1), SO (56 − 45), and SiO (5−4) at > 10σ in the integrated maps. The asterix (“Y*”) indicates emission at 5−10σ. For SO (56−45): “D” indicates emission from the disk, “D/E?” indicates compact emission at low blue- and red-shifted velocities, and with a velocity gradient perpendicular to the jet (except for L1448-2A), originating from the inner envelope or the disk. (d) The jet or outflow position angles are given for the blue-shifted lobe from North to East. If the blue- and red-shifted lobes have different PA or if only one of the two lobes is detected, this is indicated by the label (B) or (R). (e) For L1521-F, L1527, and SerpM-SMM4a, we do not detect SiO and SO, and CO emission does not show a clear structure. The reported PA are taken from Tokuda et al. (2016), Hogerheijde et al. (1998), Tobin et al. (2012), Aso et al. (2018). For L1448-NA we do not detect emission in any of the tracer, and the PA is from CO (2− 1) observations by Lee et al. (2015b). (f)The jet PA is taken to be in the middle of the CO cavities.
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