Table 3.
SF clumps properties.
| rx × ry | SFR | VHα | V* | σHα | σ* | E(B − V)gas | 12 + log(O/H)C17 | log UD16 | Ne | |
|---|---|---|---|---|---|---|---|---|---|---|
| (M⊙ yr−1) | (km s−1) | (km s−1) | (km s−1) | (km s−1) | (cm−3) | |||||
| SC1 | 1.6″ × 1.5″ | 0.1 | +127 ± 4 | +77 ± 7 | 62 ± 2 | 120 ± 13 | 0.77 ± 0.03 | 8.8 ± 0.1 | −3.1 ± 0.2 | 60 ± 20 |
| SC2 | 1.1″ × 1.1″ | 0.2 | +130 ± 8 | −19 ± 8 | 65 ± 5 | 90 ± 31 | 1.60 ± 0.10 | 8.7 ± 0.2 | −3.0 ± 0.2 | 55 ± 10 |
| SC3 | 1.7″ × 1.3″ | 0.5 | −232 ± 4 | +32 ± 7 | 70 ± 6 | 130 ± 10 | 1.29 ± 0.03 | 8.6 ± 0.2 | −3.7 ± 0.2 |
 |
| SC4 | 2.3″ × 1.7″ | 2.8 | −65 ± 4 | −9 ± 7 | 90 ± 3 | 175 ± 10 | 1.17 ± 0.02 | 8.8 ± 0.1 | −3.1 ± 0.2 | 240 ± 20 |
Notes. rx and ry are derived from 2D Gaussian fits. Stellar velocities and velocity dispersions were obtained from pPXF analysis, considering the integrated spectra over individual SCs (Appendix F). Hα velocity and velocity dispersion, colour excess E(B − V)gas, metallicity, and log UD16 were derived from the spectral fit analysis of the integrated spectra for the only kinematic component associated with SF ionisation. Stellar and gas velocity dispersions are not corrected for the instrumental broadening. Log UD16 refers to the ionisation parameters derived following the approach described in Dopita et al. (2016); the ionisation parameters derived from [S III]/[S II] ratios are consistent with those reported in the table, within a few ∼0.1 dex. The metallicities were derived from N2 line ratios following Curti et al. (2017); slightly higher values (still consistent within uncertainties) can be derived following Dopita et al. (2016).
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