Table 1.
ISM properties, star formation, and stellar masses for sources in SPT0311–58
| ID | Hα flux | SFR(Hα) | AV | SFR(Hα) (dust-corr.) | 12+log(O/H) | M⋆ |
|---|---|---|---|---|---|---|
| (10−18 ergs−1 cm−2) | (M⊙ yr−1) | (mag.) | (M⊙ yr−1) | (×109 M⊙) | ||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) |
| E | 18.8 ± 0.8 | 62. ± 2. | 1.7 ± 0.3 | 231. ± 10. | 8.37 ± 0.06 | 35.4 ± 4.3 |
| 2.4 ± 0.3 (1) | 377. ± 20. (2) | 21.0 ± 5.2 (5) | ||||
| Eext | 11 ± 2. | 32. ± 3. | (0.85) | (61.) (7) | ||
| W | 4.5 ± 0.9 | 8. ± 1. | 5.8 ± 0.6 (1) | 603. ± 121 (2) | (80. ± 24.) (6) | |
| Wext | 5.3 ± 1.4 | 9. ± 1. | (2.00) | (39.) (7) | ||
| C1 | 1.5 ± 0.3 | 5.5 ± 1. | 0.7 ± 0.6 | 9.2 ± 1.8 | 8.37 ± 0.10 | 1.60 ± 0.23 |
| C2 | 0.92 ± 0.25 | 2. ± 0.4 | 1.0 ± 0.9 | 4.2 ± 1.1 | 7.97 ± 0.20 | 2.88 ± 0.68 |
| C3 (3) | 1.3 ± 0.4 | 6.2 ± 1.2 | 2.2 ± 1.6 | 33. ± 10. | 8.56 ± 0.10 | 3.41 ± 0.94 |
| L1 | 1.2 ± 0.3 | 2.9 ± 0.4 | 1.9 ± 0.8 | 12. ± 3. | 7.86 ± 0.16 | 0.35 ± 0.04 |
| L2 | 0.51 ± 0.07 | |||||
| L3 (3) | 0.47 ± 0.25 | 1.2 ± 0.4 | (0.85) | (2.3) (7) | 1.48 ± 0.35 | |
| L4 | 0.64 ± 0.22 | 1.1 ± 0.3 | (0.85) | (2.1) (7) | 1.26 ± 0.19 | |
| L5 (3) | 1.6 ± 0.4 | 3.9 ± 0.6 | 0.8 ± 0.6 | 7.0 ± 1.7 | 7.79 ± 0.35 | 1.17 ± 0.18 |
| L6 | 0.49 ± 0.18 | 1.2 ± 0.3 | (0.85) | (2.0) (7) | 0.56 ± 0.12 | |
| L7 (4) | 0.85 ± 0.20 | 1.1 ± 0.3 | (0.85) | (2.0) (7) | (7.58 ± 0.46) | |
Notes. Column 1: Source identification. Column 2: Observed Hα flux obtained by averaging values from the R2700 and R100 spectra, if S/N > 3. The R100 fluxes were reduced by 10% to account for a known calibration factor (see Appendix A). For Eext, W and Wext, only R100 data were used due to the low S/N of their R2700 spectra. In addition, for Eext the fits could not resolve the Hα and the [NII] lines, and thus an average factor of 0.77 was applied to account for the [NII] emission when deriving the corresponding Hα flux. Further details are provided in Appendix A. Column 3: SFRs obtained with the relation of Kennicutt & Evans (2012). No dust correction is applied. For galaxies C2 and L1–L5 values have been corrected by a factor 0.5 to account for their metallicity (see text). Column 4: Visual attenuation inferred from the Balmer decrement (Hα/Hβ). For E and W the values inferred from Paα/Hα are also given. For C1 and C2, AV was obtained from the R100 spectra only, as the Hβ R2700 fluxes have significantly lower S/N. Column 5: SFR after correction for the visual attenuation in Col. 4. The SFRs in columns 3 and 5 are corrected for the lensing magnification factors (see Appendix B) and the finite apertures used (Appendix A). Column 6: Metallicities based on the Curti et al. (2017) calibration (see Sect. 4.4). For L7, the metallicity is not well constrained. Column 7: Stellar masses (see Sect. 4.1). They take into account aperture and magnification corrections. The uncertainties correspond to 16- and 84- percentiles taking into account the flux errors, but they do not include systematic uncertainties due to the model assumptions. (1)AV(Paα/Hα) using an aperture of 1″, as in Álvarez-Márquez et al. (2023). (2)Corrected with AV(Paα/Hα). (3)These sources are close the edge of the FoV, and subject to larger calibration uncertainties. (4)For this galaxy the values are derived from the 2D kinematic decomposition (see text in Sect. 3.3.3). (5)Stellar mass inferred with CIGALE (see text). (6)Stellar mass derived by Álvarez-Márquez et al. (2023). (7)Taking an average Av (see text).
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