Table 4
Overview of the analyzed mm cores.
| Core | Coordinates | CO | Herschel | |||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| α | δ | vLSR | Ipeak | F1300 | rout | Tkin | Mcore | N(H2) | τcont | Outflow | Clump | |
| (J2000) | (J2000) | (km s−1) | (mJy | (mJy) | (au) | (K) | (M⊙) | (1022 | (10−3) | |||
| beam−1) | cm−2) | |||||||||||
| ISOSS J22478+6357 1 | 22:47:51.08 | +63:56:43.7 | − 39.8 | 7.69 | 12.59 | 5007 | 42 | 1.84 | 27.4 | 7.0 | ✓ | … |
| ISOSS J22478+6357 2 | 22:47:52.68 | +63:56:34.5 | − 39.7 | 2.38 | 5.14 | 3967 | 13 | 3.33 | 37.5 | 9.8 | ✓ | … |
| ISOSS J22478+6357 3 | 22:47:46.56 | +63:56:49.1 | − 39.0 | 1.80 | 4.02 | 3841 | 33 | 0.78 | 8.5 | 2.2 | ✓ | … |
| ISOSS J22478+6357 4 | 22:47:46.42 | +63:56:49.8 | − 39.1 | 1.25 | 3.49 | 3915 | 22 | 1.1 | 9.6 | 2.5 | ✓ | Clump 1 |
| ISOSS J22478+6357 5 | 22:47:48.15 | +63:56:44.3 | − 40.1 | 0.89 | 2.02 | 3108 | 37 | 0.34 | 3.7 | 0.9 | ✓ | Clump 3 |
| ISOSS J22478+6357 6 | 22:47:50.39 | +63:56:57.1 | − 40.5 | 0.78 | 4.08 | 4986 | 27 | 0.97 | 4.5 | 1.2 | ✗ | Clump 5 |
| ISOSS J22478+6357 7 | 22:47:50.67 | +63:57:00.6 | − 41.0 | 0.73 | 0.79 | 2096 | 10 | 0.76 | 17.1 | 4.5 | ✗ | … |
| ISOSS J22478+6357 8 | 22:47:50.88 | +63:56:41.2 | − 39.0 | 0.68 | 1.90 | 3326 | 27 | 0.47 | 4.1 | 1.0 | ✗ | … |
| ISOSS J22478+6357 9 | 22:47:50.42 | +63:56:46.6 | − 40.7 | 0.62 | 3.91 | 4891 | 10 | 3.76 | 14.5 | 3.8 | ✗ | … |
| ISOSS J22478+6357 10 | 22:47:45.65 | +63:56:27.1 | − 39.5 | 0.56 | 1.38 | 3060 | 10 | 1.32 | 13.1 | 3.5 | ✗ | … |
| ISOSS J22478+6357 11 | 22:47:49.40 | +63:56:52.1 | − 39.3 | 0.47 | 1.07 | 2768 | 18 | 0.45 | 4.8 | 1.2 | ✗ | … |
| ISOSS J22478+6357 12 | 22:47:51.22 | +63:56:38.4 | − 38.8 | 0.40 | 0.40 | 1510 | 57 | 0.04 | 1.0 | 0.3 | ✗ | … |
| ISOSS J22478+6357 13 | 22:47:50.02 | +63:56:45.0 | − 40.4 | 0.37 | 0.37 | 1510 | 15 | 0.19 | 4.7 | 1.2 | ✗ | Clump 4 |
| ISOSS J22478+6357 14 | 22:47:51.18 | +63:57:00.3 | − 40.9 | 0.36 | 0.52 | 2039 | 27 | 0.13 | 2.2 | 0.6 | ✗ | … |
| ISOSS J22478+6357 15 | 22:47:49.87 | +63:56:45.8 | − 39.9 | 0.35 | 0.35 | 1510 | 20 | 0.12 | 3.0 | 0.8 | ✗ | … |
| ISOSS J23053+5953 1 | 23:05:21.62 | +59:53:43.2 | − 52.2 | 18.38 | 62.67 | 8063 | 186 | 3.29 | 13.2 | 4.1 | ✓ | Clump 2 |
| ISOSS J23053+5953 2 | 23:05:23.54 | +59:53:54.7 | − 52.0 | 9.82 | 35.39 | 8018 | 139 | 2.51 | 9.5 | 3.0 | ✗ | Clump 3 |
| ISOSS J23053+5953 3 | 23:05:23.15 | +59:53:54.9 | − 51.3 | 7.55 | 30.09 | 7324 | 67 | 4.61 | 15.8 | 5.0 | ✗ | … |
| ISOSS J23053+5953 4 | 23:05:19.99 | +59:53:55.2 | − 51.5 | 5.88 | 11.76 | 4916 | 33 | 3.95 | 27.0 | 8.6 | ✗ | … |
| ISOSS J23053+5953 5 | 23:05:21.84 | +59:53:46.1 | − 51.0 | 4.92 | 18.08 | 7055 | 112 | 1.61 | 6.0 | 1.9 | ✗ | … |
| ISOSS J23053+5953 6 | 23:05:23.79 | +59:54:01.0 | − 52.2 | 4.57 | 13.02 | 5793 | 88 | 1.5 | 7.2 | 2.2 | ✗ | … |
| ISOSS J23053+5953 7 | 23:05:24.57 | +59:53:59.4 | − 52.4 | 2.32 | 3.53 | 3349 | 54 | 0.69 | 6.2 | 1.9 | ✗ | … |
| ISOSS J23053+5953 8 | 23:05:20.34 | +59:53:43.2 | − 51.9 | 2.29 | 2.94 | 2993 | 38 | 0.84 | 9.0 | 2.8 | ✗ | … |
| ISOSS J23053+5953 9 | 23:05:22.41 | +59:53:46.2 | − 51.8 | 1.88 | 2.52 | 2970 | 92 | 0.28 | 2.8 | 0.9 | ✓ | … |
| ISOSS J23053+5953 10 | 23:05:20.74 | +59:53:52.1 | − 51.8 | 1.73 | 4.76 | 4264 | 30 | 1.8 | 9.0 | 2.8 | ✓ | … |
| ISOSS J23053+5953 11 | 23:05:21.38 | +59:53:53.0 | − 51.8 | 1.50 | 1.50 | 1737 | 26 | 0.67 | 9.1 | 2.9 | ✗ | … |
| ISOSS J23053+5953 12 | 23:05:19.82 | +59:54:02.6 | − 51.7 | 1.46 | 1.89 | 2681 | 39 | 0.53 | 5.6 | 1.8 | ✗ | … |
| ISOSS J23053+5953 13 | 23:05:23.78 | +59:53:51.7 | − 52.4 | 1.39 | 2.56 | 3262 | 61 | 0.44 | 3.2 | 1.0 | ✗ | … |
| ISOSS J23053+5953 14 | 23:05:24.42 | +59:54:01.7 | − 52.3 | 1.29 | 3.51 | 3808 | 116 | 0.3 | 1.5 | 0.5 | ✗ | … |
Notes. The coordinates, peak intensity Ipeak, integrated flux F1300, outer radius rout, Tkin obtained from the H2CO rotation temperature map, core mass Mcore, and molecular hydrogen column density N(H2) are taken from Beuther et al. (2021). The systemic velocity vLSR of each core is estimated from the optically thin C18O 2− 1 line (Sect. 4.6). The continuum optical depth τcont is calculated according to Eq. (1) in Sect. 3.1. The presence of protostellar outflows are investigated in Sect. 4.1 using CO 2−1 line wing emission. Cores with an associated bipolar outflow are marked with a ✓, whereas cores with no or no clear bipolar outflow signature are marked with a ✗. The last column lists Herschel clumps studied by Ragan et al. (2012) associated with the mm cores (Fig. 2). We note that due to poor angular resolutions at FIR wavelengths, multiple mm cores can be embedded within a Herschel clump. Here we list for the mm cores the closest clump considering the clump peak intensity.
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