Table 2
Outflow masses, the largest spatial extent of the outflow lobes (R), and the velocity intervals for which the physical parameters of the blue- and red-shifted outflow lobes for the CO J = 3–2 and J = 4–3 transitions were calculated.
| Source | Line | Tsys | Mblue | Mred | Rblue | Rred | Vblue | Vred |
|---|---|---|---|---|---|---|---|---|
| (K) | (M⊙) | (M⊙) | (AU) | (AU) | (km s−1) | (km s−1) | ||
| HOPS 340 | CO J = 3–2 | 229 | 0.11 | 0.05 | 2.9 × 104 | 2.9 × 104 | (−5, 6.1) | (13.6, 25) |
| CO J = 4–3 | 758 | 0.07 | 0.03 | 2.9 × 104 | 2.9 × 104 | (−5, 6.4) | (13.1, 25) | |
| HOPS 354 | CO J = 3–2 | 280 | 0.02 | 0.06 | 2.9 × 104 | 2.2 × 104 | (−15, −2.8) | (2.5, 15) |
| CO J = 4–3 | 1001 | 0.02 | 0.02 | 2.9 × 104 | 2.2 × 104 | (−15, −2.0) | (2.7, 15) | |
| HOPS 358 | CO J = 3–2 | 226 | 0.07 | 0.05 | 3.3 × 104 | 3.8 × 104 | (−5, 6.7) | (13.6, 25) |
| CO J = 4–3 | 701 | 0.04 | 0.05 | 3.3 × 104 | 3.8 × 104 | (−5, 6.8) | (12.7, 25) | |
| HOPS 373 | CO J = 3–2 | 318 | 0.06 | 0.09 | 3.2 × 104 | 3.3 × 104 | (−5, 8.0) | (12.7, 25) |
| CO J = 4–3 | 1671 | 0.03 | 0.04 | 3.2 × 104 | 3.3 × 104 | (−5, 7.7) | (13.3, 25) | |
| HOPS 394 | CO J = 3–2 | 219 | – | 0.05 | – | 2.9 × 104 | – | (14.6, 25) |
| CO J = 4–3 | 618 | – | 0.04 | – | 2.9 × 104 | – | (14.3, 25) | |
| HOPS 223 | CO J = 3–2 | 234 | 0.07 | 0.02 | 3.3 × 104 | 3.3 × 104 | (−10, 0.8) | (7.0, 20) |
| CO J = 4–3 | 716 | 0.03 | 0.01 | 3.3 × 104 | 3.3 × 104 | (−10, 1.0) | (6.5, 20) | |
| HOPS 399 | CO J = 3–2 | 331 | 0.06 | 0.05 | 3.6 × 104 | 3.3 × 104 | (−5, 6.8) | (13, 25) |
| CO J = 4–3 | 1785 | 0.03 | 0.03 | 3.6 × 104 | 3.3 × 104 | (−5, 7.0) | (12.8, 25) | |
| HOPS 401 | CO J = 3–2 | 225 | 0.03 | – | 3.3 × 104 | – | (−5, 6.1) | – |
| CO J = 4–3 | 676 | 0.02 | – | 3.3 × 104 | – | (−5, 6.8) | – |
Notes. The uncertainties of the outflow masses are about 40%, consisting of 20% calibration error and 20% error resulting from the uncertainty in the assumed excitation temperature. The system temperature (Tsys) is given to compare the sensitivity of observations. The outflow detected toward the Class 0 protostar HOPS 340 might have a contamination from the PBR HOPS 341, and the outflow detected toward the Class I protostar HOPS 223 might have a contamination from the PBR HOPS 397. We do not show the parameters of the outflow detected toward HOPS 372, as it is attributed to HOPS 399.
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