Table 2
Flux densities obtained by integrating the emission over the HC H II region G24 A1.
| ν | Sν | HPBW | Telescope (a) | Reference |
|---|---|---|---|---|
| (GHz) | (mJy) | (arcsec) | ||
| 1.435 | 1.7 ± 0.25 | 1.26 | VLA-A | (1) |
| 4.835 | 13 ± 1.4 | 1.5 | VLA-B | (2) |
| 4.860 | 14 ± 0.1 | 0.397 | VLA-AB | (1) |
| 5.758 | 11 ± 1.6 | 0.060 | e-MERLIN | (1) |
| 8.460 | 33 ± 0.68 | 0.237 | VLA-A | (1) |
| 22.214 | 72 ± 1.2 | 0.0963 | VLA-A+PT | (3) |
| 23.738 | 85 ± 3.4 | 0.265 | VLA-B | (4) |
| 25.056 | 77 ± 1.4 | 0.0858 | VLA-A | (1) |
| 44.022 | 98 ± 5.5 | 0.0535 | VLA-A+PT | (3) |
| 214.300 | 76 ± 3.0 | 0.498 | PdBI-B | (5) |
| 216.933 | 87 ± 5.7 | 0.157 | ALMA | (6) |
| 225.300 | 86 ± 2.7 | 0.466 | SMA | (5) |
Notes. The new measurements obtained by us are highlighted in bold. The errors do not take into account the calibration uncertainty, which we conservatively assume to be 20% at all frequencies. (a) Letters after name of telescope indicate the interferometer configuration.
References.(1) This article; (2) CORNISH survey (Hoare et al. 2012; Purcell et al. 2013); (3) Beltrán et al. (2007); (4) Vig et al. (2008); (5) Beltrán et al. (2011); (6) M2018.
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