Table 1
Source sample.
| Source | α2000.0 | δ2000.0 | Tdust | n(H2) | Type |
|---|---|---|---|---|---|
| [h:m:s] | [°:′:′′] | [K] | [104 cm−3] | ||
| SMM 1 | 13 06 20.89 | −61 30 20.51 | 14.0 | 2.1 ± 1.1 | IR bright(a) |
| SMM 2 | 13 06 29.29 | −61 29 36.67 | 12.5 | 3.4 ± 1.8 | IR bright |
| SMM 3 | 13 06 36.56 | −61 28 52.79 | 13.7 | 5.1 ± 2.7 | IR bright |
| BLOB 2 | 13 06 40.44 | −61 29 52.84 | 14.9 | 5.1 ± 2.8 | IR dark |
| BLOB 1 | 13 06 40.46 | −61 29 20.84 | 11.5 | >2.5 | IR bright |
| SMM 4 | 13 06 46.06 | −61 28 40.90 | 13.2 | 5.4 ± 2.8 | IR dark |
| SMM 5 | 13 06 50.54 | −61 27 08.94 | 14.0 | 4.9 ± 2.3 | IR dark |
| IRAS 13037 | 13 06 51.65 | −61 27 56.95 | 20.0 | 4.9 ± 2.5 | IR bright |
| −6112 | |||||
| SMM 6 | 13 06 53.88 | −61 27 32.96 | 14.1 | >2.1 | IR bright |
| SMM 7 | 13 07 03.38 | −61 26 17.00 | 14.5 | 4.1 ± 2.1 | IR dark(b) |
| IRAS 13039 | 13 07 07.28 | −61 24 33.00 | 22.2 | 3.0 ± 1.6 | IR bright/ |
| −6108 | H II | ||||
| SMM 8 | 13 07 09.51 | −61 23 41.00 | 13.9 | >1.5 | IR bright(a) |
| SMM 9 | 13 07 12.85 | −61 22 44.99 | 16.3 | 6.3 ± 3.4 | IR dark |
| IRAS 13042 | 13 07 21.74 | −61 21 40.95 | 15.1 | >0.9 | IR bright |
| −6105 |
Notes. The coordinates refer to the LABOCA 870 μm peak positions of the sources (Miettinen 2018). The dust temperatures and volume-averaged H2 number densities are adopted from Miettinen (2018) but the latter are scaled upward by a factor of 1.41 (see Sect. 3.3). The source type in the last column is based on the source appearance in the WISE IR images (Miettinen 2018). (a) The clump is associated with a WISE IR source that appears to be a shock emission knot. (b) The clump appears to be associated with a weak WISE IR source but it is likely an extragalactic object (see Sect. 4.1).
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