Table 2.
Spatially integrated measurements for the three starbursts.
| HATLASJ090750.0+010141 | HATLASJ114625.4−014511 | HATLASJ121446.0−011155 | |
|---|---|---|---|
| RA (J2000) | 09:07:50.07 | 11:46:25.01 | 12:14:46.47 |
| Dec (J2000) | +01:01:41.47 | −01:45:12.81 | −01:11:55.55 |
| zspec | 0.12834 | 0.16553 | 0.17981 |
| M⋆ (×1010 M⊙) | 1.4 ± 0.4 | 5.1 ± 1.2 | 6.6 ± 1.7 |
| LIR (×1010 L⊙) | 50 ± 1 | 53 ± 1 | 35 ± 1 |
| SFRIR | 50 ± 1 | 53 ± 1 | 35 ± 1 |
| fPaα (×10−17 erg s−1 cm−2) | – | 1069 ± 111 | 644 ± 96 |
| E(B − V)Neb | – | 1.35 ± 0.05 | 0.91 ± 0.06 |
| SFRPaα | – | 32 ± 4 | 25 ± 4 |
| SFRPaα, corr | – | 67 ± 8 | 40 ± 6 |
| SCOΔv (Jy km s−1) | 6.8 ± 0.6 | 6.6 ± 0.6 | 4.6 ± 0.6 |
 (×109 K km s−1 pc2) |
5.4 ± 0.5 | 8.6 ± 0.8 | 7.3 ± 0.9 |
Notes. The far-IR luminosities are calculated across the rest-frame 8−1000 μm wavelength range. E(B − V)Neb is the colour excess estimated by using the observed Hα-to-Paα flux ratio. SFRPaα and SFRPaα, corr correspond to the observed and attenuation-corrected Paα-based SFR estimates, respectively. SCOΔv is the velocity-integrated flux density. 
is the CO(1–0) line luminosity taken from Villanueva et al. (2017).
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