Table 1
Initial source sample.
| Source | α2000.0 | δ2000.0 | Type |
|---|---|---|---|
| [h:m:s] | [°:′:′′] | ||
| SMM 1a | 13 06 19.38 | –61 30 19.42 | IR dark |
| SMM 1b | 13 06 23.36 | –61 30 10.37 | IR bright(a) |
| SMM 2 | 13 06 28.82 | –61 29 43.43 | IR bright |
| SMM 3 | 13 06 37.00 | –61 28 51.00 | IR bright |
| BLOB 2 | 13 06 39.50 | –61 30 01.51 | IR dark |
| SMM 4a | 13 06 46.21 | –61 28 48.04 | IR bright |
| SMM 4b | 13 06 46.84 | –61 28 22.54 | IR bright |
| SMM 4c | 13 06 42.86 | –61 28 33.03 | IR dark |
| IRAS 13037 | 13 06 51.45 | –61 28 24.04 | IR bright |
| –6112a | |||
| IRAS 13037 | 13 06 51.24 | –61 27 51.04 | IR bright |
| –6112b | |||
| SMM 6a | 13 06 55.42 | –61 27 27.03 | IR bright |
| SMM 6b | 13 06 52.08 | –61 27 40.54 | IR bright(a) |
| SMM 7 | 13 07 04.20 | –61 26 15.00 | IR bright(b) |
| IRAS 13039 | 13 07 06.49 | –61 24 32.98 | IR bright/H II(c) |
| –6108a | |||
| IRAS 13039 | 13 07 08.58 | –61 23 56.97 | IR dark |
| -6108b | |||
| SMM 9 | 13 07 12.53 | –61 22 46.43 | IR dark |
| IRAS 13042 | 13 07 20.66 | –61 21 52.33 | IR bright |
| –6105 |
Notes. The coordinates refer to the SABOCA 350 μm peak positions of the sources (Miettinen 2018). The source type in the last column is based on the source appearance in the WISE IR images (Miettinen 2018). (a)The core is associated with a WISE IR source that could be a shock emission knot. (b) The weak WISE IR source seen towards SMM 7 was considered a candidate extragalactic object in our previous studies (Miettinen 2018, 2020), but it could be an embedded YSO associated with a secondary 350 μm peak position at α2000.0 = 13h07m04. s21, δ2000.0 = −61°26′ 22′′. 50 (2′′. 8 or 0.03 pc offset; see Appendix A). Hence, SMM 7 is considered an IR bright core in the present study. (c) The core is associated with an optically thin H II region (Sánchez-Monge et al. 2013).
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