Table 4.
Properties of the H II regions outside the stellar disc.
| Region | log L(Hα) | log SFR | log Mstar | Age |
|---|---|---|---|---|
| Units | erg s−1 | M⊙ yr−1 | M⊙ | Myr |
| 1 | 37.80 ± 0.01 | −3.50 ± 0.01 | 3.94 ± 0.23 | 8.84 ± 1.76 |
| 2 | 37.59 ± 0.02 | −3.71 ± 0.02 | 3.92 ± 0.18 | 10.92 ± 1.50 |
| 3 | 37.43 ± 0.02 | −3.87 ± 0.02 | 4.42 ± 0.11 | 17.06 ± 1.26 |
| 4 | 37.23 ± 0.04 | −4.07 ± 0.04 | – | – |
| 5 | 36.79 ± 0.10 | −4.51 ± 0.10 | – | 11.34 ± 25.80 |
| 6 | 36.82 ± 0.09 | −4.48 ± 0.09 | – | – |
| 7 | 36.51 ± 0.19 | −4.79 ± 0.19 | – | – |
| 8 | 36.48 ± 0.20 | −4.82 ± 0.20 | – | – |
| 9 | 36.64 ± 0.14 | −4.66 ± 0.14 | – | 62.93 ± 87.34 |
| 10 | 37.08 ± 0.05 | −4.22 ± 0.05 | – | – |
| 11 | 36.94 ± 0.07 | −4.36 ± 0.07 | – | – |
| 12 | 36.71 ± 0.12 | −4.59 ± 0.12 | – | – |
Notes. Hα luminosity are derived after correcting the VESTIGE Hα fluxes for [NII] contamination (N[II]λ6583Å/Hα = 0.1) and dust attenuation (A(Hα) = 0.02 mag) as in Boselli et al. (2018b). Star formation rates are derived from the Hα luminosity using the calibration of Calzetti et al. (2010). Given the low star formation regime, these numbers should be taken as indicative (see Boselli et al. 2023 for details). Both SFR and Mstar have been derived assuming a Chabrier IMF.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.