Table 1
Observed 114 rising spectra H II regions.
| Name | S1.4 GHz | S5 GHz | Dist | Lbol | [Ref.] |
|---|---|---|---|---|---|
| (mJy) | (mJy) | (kpc) | (L⊙) | ||
| (2) | (3) | (4) | (5) | (6) | |
| G010.3009−00.1477 | 426.2 | 631.4 | 3.5 | 5.2 | [1] |
| G010.4724+00.0275 | 31.3 | 38.4 | 8.5 | 5.7 | [1] |
| G010.6223−00.3788† | 327.6 | 483.3 | 2.4 | 5.7 | [1] |
| G010.6234−00.3837 | 571.3 | 1952.2 | 5.0 | 5.7 | [1] |
| G010.9584+00.0221 | 47.9 | 196.0 | 2.9 | 4.0 | [1] |
| G027.9782+00.0789 | 89.3 | 124.0 | 4.8 | 4.2 | [2] |
| G028.2003−00.0494 | − | 161.0 | 6.1 | 5.1 | [1] |
| G028.2879−00.3641 | 410.9 | 552.8 | 11.6 | 5.9 | [1] |
| G028.6082+00.0185 | 168.2 | 210.2 | 7.4 | 5.0 | [1] |
| G029.9559−00.0168 | 1610.8 | 3116.2 | 5.2 | 5.7 | [1] |
| G049.3704−00.3012 | 252.9 | 414.4 | 5.4 | 5.1 | [3] |
| G048.6099+00.0270 | 56.5 | 131.2 | 9.8 | 5.1 | [4] |
Notes. Columns, inorder, show source name, flux density at 1.4 and 5 GHz respectively (see Yang et al. 2019 for details), heliocentric distance, and bolometric luminosity, and the reference these values are drawn from. Uncertainties on the fluxes and distances are estimated to be 10%, and those on luminosity, 20%. Only a small portion of the data is provided here, the full table is available in electronic form at the CDS. Source names appended with a † refers to the sources observed that could not be imaged.
References. [1] Urquhart et al. (2018), [2] Cesaroni et al. (2015), [3] Urquhart et al. (2013), [4] Kalcheva et al. (2018).
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