Table 1.
Source table.
| No | Sourcea | RA (J2000) | Dec (J2000) | VLSR | Distance | Mass | Radius | Commentsb | Commentsc |
|---|---|---|---|---|---|---|---|---|---|
| (km s−1) | (kpc) | (103 M⊙) | (pc) | ||||||
| 1 | G008.684−00.367 | 18:06:23.35 | −21:37:05.2 | 37.6 | 4.4 | 2.2 | 1.7 | D8 | MSF |
| 2 | G008.706−00.414 | 18:06:36.72 | −21:37:18.6 | 38.5 | 11.8 | 5.3 | 2.9 | D24 | YSO |
| 3 | G010.444−00.017 | 18:08:44.59 | −19:54:36.4 | 72.4 | 10.2 | 4.3 | 2.3 | D24 | MSF |
| 4 | G013.178+00.059 | 18:14:01.32 | −17:28:38.6 | 48.5 | 4.5 | 1.0 | 1.6 | D8 | MSF |
| 5 | G014.114−00.574 | 18:18:13.14 | −16:57:20.0 | 20.1 | 1.9 | 0.8 | 1.3 | D8 | YSO |
| 6 | G014.194−00.194 | 18:16:58.77 | −16:42:17.5 | 39.4 | 3.1 | 2.7 | 1.4 | D8 | YSO |
| 7 | G014.492−00.139 | 18:17:22.09 | −16:24:59.4 | 39.7 | 3.2 | 2.0 | 2.7 | D24 | YSO |
| 8 | G014.632−00.577 | 18:19:15.22 | −16:30:02.3 | 18.2 | 1.9 | 0.5 | 1.0 | D8 | MSF |
| 9 | G018.876−00.489 | 18:27:07.69 | −12:41:36.4 | 65.5 | 5.0 | 1.2 | 1.5 | D8 | YSO |
| 10 | G309.382−00.134 | 13:47:24.03 | −62:18:09.5 | −49.5 | 6.7 | 2.4 | 3.2 | D8 | MSF |
| 11 | G317.867−00.151 | 14:53:16.60 | −59:26:33.9 | −40.2 | 2.5 | 0.3 | 0.7 | D8 | YSO |
| 12 | G318.779−00.137 | 14:59:33.06 | −59:00:33.5 | −37.5 | 10.2 | 13.5 | 5.2 | D8 | YSO |
| 13 | G320.881−00.397 | 15:14:33.18 | −58:11:28.5 | −-44.8 | 2.8 | 0.4 | 0.7 | D24 | YSO |
| 14 | G326.987−00.031 | 15:49:08.16 | −54:23:06.9 | −58.2 | 3.5 | 1.0 | 1.1 | D8 | Protostellar |
| 15 | G329.029−00.206 | 16:00:31.96 | −53:12:54.0 | −43.5 | 2.8 | 2.8 | 1.9 | D8 | MSF |
| 16 | G331.708+00.583 | 16:10:06.79 | −50:50:29.4 | −66.8 | 10.8 | 12.1 | 4.7 | D8 | YSO |
| 17 | G333.656+00.059 | 16:21:11.61 | −49:52:16.3 | −84.2 | 5.0 | 2.7 | 3.1 | D24 | Protostellar |
| 18 | G335.789+00.174 | 16:29:47.34 | −48:15:52.1 | −49.5 | 3.3 | 1.9 | 2.2 | D8 | MSF |
| 19 | G336.958−00.224 | 16:36:17.12 | −47:40:44.3 | −71.1 | 10.9 | 1.5 | 1.8 | D24 | MSF |
| 20 | G337.176−00.032 | 16:36:18.78 | −47:23:18.6 | −65.6 | 11.2 | 23.9 | 8.7 | D8 | MSF |
| 21 | G337.258−00.101 | 16:36:56.42 | −47:22:27.0 | −67.6 | 11.1 | 10.5 | 5.4 | D8 | MSF |
| 22 | G338.786+00.476 | 16:40:22.55 | −45:51:04.1 | −64.6 | 11.3 | 2.2 | 2.6 | D24 | Protostellar |
| 23 | G340.784−00.097 | 16:50:14.89 | −44:42:31.6 | −101.4 | 9.6 | 3.7 | 3.5 | D8 | MSF |
| 24 | G342.484+00.182 | 16:55:02.53 | −43:13:03.1 | −41.3 | 12.6 | 11.0 | 6.1 | D8 | MSF |
| 25 | G343.756−00.164 | 17:00:50.08 | −42:26:11.9 | −26.9 | 2.5 | 1.3 | 1.5 | D8 | MSF |
| 26 | G351.444+00.659 | 17:20:54.60 | −35:45:12.8 | −3.9 | 1.4 | 3.1 | 1.0 | D8 | MSF |
| 27 | G351.571+00.762 | 17:20:51.00 | −35:35:25.8 | −2.7 | 1.3 | 2.0 | 1.3 | D24 | YSO |
| 28 | G353.066+00.452 | 17:26:13.50 | −34:31:54.0 | 1.9 | 1.3 | 0.2 | 0.7 | D24 | YSO |
| 29 | G353.417−00.079 | 17:29:18.94 | −34:32:05.9 | −54.2 | 10.2 | 6.8 | 3.1 | D24 | Protostellar |
| 30 | G354.944−00.537 | 17:35:11.69 | −33:30:23.8 | −5.5 | 1.4 | 0.1 | 0.6 | D24 | YSO |
Notes. Kinematic distances, VLSR, mass and radius are taken from Urquhart et al. (2018) which provides the most updated values based on previous ATLASGAL studies and follow-up studies (e.g., Wienen et al. 2015; Giannetti et al. 2014). Urquhart et al. (2018) combined the solutions from HI self-absorption and HI absorption methods using molecular line observations, maser parallax and spectroscopic distance measurements when available. Masses are based on 870 μm dust continuum and NH3 lines. There might be large uncertainty in the mass due to uncertain dust emissivity as stated in Motte et al. (2007). Also, note that, the clumps are extended compared to the beam size, thus the mass values are above the sensitivity limit of ATLASGAL.
Massive clumps that were detected by the ATLASGAL survey (Giannetti et al. 2014) and classified as objects dark at 8.0 μm or 24.0 μm.
Giannetti et al. (2014) identified the sources as dark at 8.0 μm or 24.0 μm if the flux density is smaller than the average flux at the same wavelength in the vicinity of the source. These sources are marked as D8 or D24.
Urquhart et al. (2018) provides associated sources such as massive star forming (MSF) regions and young stellar objects (YSO) from the follow-up observations of these clumps.
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