Table B.1
Observational parameters and physical properties of the sources.
| Source | R.A. (J2000) a | Dec. (J2000) a | Beam | Line rms b | d c | DGCd | Lbole |
|---|---|---|---|---|---|---|---|
| (hh:mm:ss.s) | (dd:mm:ss.s) | (″) | (K) | (kpc) | (kpc) | (L⊙) | |
| 126348 | 18:42:51.98 | -03:59:54.37 | 1.26 × 1.08 | 0.16 | 4.41 | 4.67 | 6798 |
| 615590 | 09:24:41.96 | -52:02:08.04 | 0.68 × 0.59 | 0.50 | 2.70 | 8.31 | 5470 |
| 644284A | 10:31:29.78 | -58:02:19.27 | 0.96 × 0.80 | 0.32 | 4.75 | 8.20 | − |
| 693050 | 12:35:35.05 | -63:02:31.19 | 1.03 × 0.94 | 0.19 | 4.31 | 6.89 | 12200 |
| 705768 | 13:12:36.17 | -62:33:34.43 | 0.93 × 0.81 | 0.24 | 6.88 | 6.93 | 91728 |
| 707948 | 13:16:43.19 | -62:58:32.83 | 0.94 × 0.80 | 0.26 | 7.14 | 6.97 | 196800 |
| 717461A | 13:43:01.68 | -62:08:51.42 | 1.34 × 1.21 | 0.22 | 4.29 | 6.31 | 3323 |
| 721992 | 13:51:58.27 | -61:15:41.04 | 0.90 × 0.79 | 0.37 | 5.38 | 6.16 | 2630 |
| 724566 | 13:59:30.92 | -61:48:38.27 | 0.87 × 0.78 | 0.34 | 4.93 | 6.10 | 226 |
| 732038 | 14:13:15.05 | -61:16:53.19 | 0.87 × 0.78 | 0.40 | 5.64 | 5.93 | 74930 |
| 744757A | 14:45:26.35 | -59:49:15.55 | 1.31 × 1.27 | 0.15 | 2.51 | 6.45 | 12381 |
| 767784 | 15:29:19.31 | -56:31:22.02 | 1.31 × 1.24 | 0.16 | 4.04 | 5.37 | 139400 |
| 865468A | 17:05:10.90 | -41:29:06.99 | 1.32 × 1.14 | 0.22 | 3.04 | 5.17 | 47824 |
| 876288 | 17:11:51.02 | -39:09:29.18 | 0.92 × 0.69 | 0.29 | 5.95 | 2.58 | 58410 |
| 881427C | 17:20:06.12 | -38:57:15.84 | 1.31 × 1.13 | 0.56 | 1.50 | 6.59 | 458 |
| G023.3891p00.1851 | 18:33:14.32 | -08:23:57.82 | 1.43 × 1.07 | 0.18 | 10.86 | 4.72 | 91560 |
| G025.6498p01.0491 | 18:34:20.92 | -05:59:42.08 | 1.24 × 1.07 | 0.15 | 12.20 | 6.05 | 424000 |
| G305.2017p00.2072A1 | 13:11:10.45 | -62:34:38.60 | 1.38 × 1.21 | 0.21 | 4.00 | 6.61 | 20301 |
| G314.3197p00.1125 | 14:26:26.25 | -60:38:31.26 | 1.36 × 1.23 | 0.21 | 8.25 | 6.33 | 66440 |
| G316.6412-00.0867 | 14:44:18.35 | -59:55:11.28 | 1.32 × 1.25 | 0.15 | 2.73 | 6.35 | 8080 |
| G318.0489p00.0854B | 14:53:42.64 | -59:08:53.02 | 1.31 × 1.27 | 0.15 | 3.18 | 6.07 | 36480 |
| G318.9480-00.1969A1 | 15:00:55.28 | -58:58:52.60 | 1.30 × 1.27 | 0.15 | 10.40 | 6.83 | 209000 |
| G323.7399-00.2617B2 | 15:31:45.45 | -56:30:49.84 | 1.29 × 1.25 | 0.15 | 3.20 | 5.79 | 1529 |
| G327.1192p00.5103 | 15:47:32.72 | -53:52:38.60 | 0.90 × 0.72 | 0.34 | 4.74 | 4.81 | 54270 |
| G343.1261-00.0623 | 16:58:17.22 | -42:52:07.54 | 1.33 × 1.15 | 0.21 | 2.00 | 6.16 | 33800 |
| G345.5043p00.3480 | 17:04:22.89 | -40:44:23.06 | 1.34 × 1.15 | 0.20 | 2.00 | 6.13 | 29498 |
b Line rms as computed by Nazari et al. (2022).
c Distance to the source (Lumsden et al. 2013; Mège et al. 2021). Typical uncertainties are of ~0.5 kpc.
d Distance to the galactic center assuming the Sun’s DGC as 8.05 kpc (Honma et al. 2015).
e Bolometric luminosities corrected to the distances d (Lumsden et al. 2013; Elia et al. 2017). For regions with multiple cores, the fraction of each individual source was estimated by dividing the total luminosity over all the cores weighted by their peak continuum flux (see also van Gelder et al. 2022b and Nazari et al. 2022). No estimations for 644284A are available, so a generic Lbol ~ 104 L⊙ is assumed.
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