Table 1
Catalogue of source properties.
| No. | Source | ATLASGAL name(a) | RA (J2000) | Dec (J2000) | Vlsr(b) (km s−1) | D(c) (kpc) | Lbol(d) (L⊙) | Mclump (e) (M⊙) | DGC (kpc) | Type(f) |
|---|---|---|---|---|---|---|---|---|---|---|
| 1 | G351.16+0.7 | AGAL351.161+00.697 | 17:19:56.69 | −35:57:53.0 | −6.0 | 1.3 | 8.8 × 103 | 1.2 × 103 | 6.7 | IRb |
| 2 | G351.25+0.7 | AGAL351.244+00.669 | 17:20:18.86 | −35:54:42.5 | −2.8 | 1.3 | 4.9 × 104 | 3.7 × 102 | 6.7 | IRb |
| 3 | G351.44+0.7 | AGAL351.444+00.659 | 17:20:55.20 | −35:45:08.0 | −3.8 | 1.3 | 2.0 × 104 | 1.0 × 103 | 6.7 | 24d |
| 4 | G351.58−0.4 | AGAL351.581−00.352 | 17:25:25.03 | −36:12:45.4 | −95.6 | 8.0 | 4.6 × 105 | 2.3 × 103 | 2.0 | IRb |
| 5 | G351.77−0.5 | AGAL351.774−00.537 | 17:26:42.54 | −36:09:20.1 | −2.8 | 1.3 | 3.7 × 104 | 3.3 × 102 | 7.8 | IRb |
| 6 | G12.81−0.2 | AGAL012.804−00.199 | 18:14:13.54 | −17:55:32.0 | 34.6 | 2.6 | 2.5 × 105 | 1.9 × 103 | 6.2 | HII |
| 7 | G14.19−0.2 | AGAL014.194−00.194 | 18:16:58.63 | −16:42:16.4 | 39.7 | 3.1 | 3.7 × 103 | 5.1 × 102 | 4.8 | 24d |
| 8 | G13.66−0.6 | AGAL013.658−00.599 | 18:17:24.09 | −17:22:10.3 | 48.5 | 4.5 | 2.4 × 104 | 2.7 × 102 | 4.3 | IRb |
| 9 | G14.63−0.6 | AGAL014.632−00.577 | 18:19:14.65 | −16:30:02.7 | 18.5 | 1.5 | 1.6 × 103 | 1.6 × 102 | 6.3 | 24d |
| 10 | G34.41+0.2 | AGAL034.411+00.234 | 18:53:18.13 | +01:25:23.7 | 57.9 | 2.9 | 3.1 × 103 | 4.4 × 102 | 7.2 | IRb |
| 11 | G34.26+0.15 | AGAL034.258+00.154 | 18:53:18.51 | +01:14:57.6 | 58.0 | 2.9 | 6.1 × 104 | 1.7 × 103 | 6.9 | HII |
| 12 | G34.40−0.2 | AGAL034.401+00.226 | 18:53:18.63 | +01:24:40.4 | 57.1 | 2.9 | 3.2 × 103 | 7.9 × 102 | 7.2 | HII |
| 13 | G35.20−0.7 | AGAL035.197−00.742 | 18:58:12.94 | +01:40:40.6 | 33.5 | 2.2 | 2.4 × 104 | 4.6 × 102 | 6.8 | IRb |
Notes. (a)Source names from the ATLASGAL Compact Source Catalogue (Contreras et al. 2013; Urquhart et al. 2014). (b)Source velocities (Vlsr) estimated from proxy lines (see Appendix D).(c) Heliocentric distances estimated in Urquhart et al. (2022). (d)Source bolometric luminosities, Lbol, estimated from greybody fit to dust emission in Urquhart et al. (2018). Lbol of source 1, 6, and 13 were estimated in König et al. (2017). (e)Clump masses, Mclump, were estimated from cold dust emission at 870 µm in Urquhart et al. (2022). Mclump of source 1, 6, and 13 were obtained from König et al. (2017). (f)Source classification using the criteria is from König et al. (2017), and refers to IR-bright sources (IRb), IR-weak sources (24d), and HII regions (HII).
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