Table 3.
Summary of the physical properties and emission lines fluxes determined from the SED fitting analysis of the integrated E and W galaxies of SPT0311-58.
| Parameter | Units | E galaxy | W galaxy |
|---|---|---|---|
| Age Stars | Myr | 21±7 | 26±10 |
| M* | ×1010 M⊙ | 1.4±0.4 | 8.0±2.4 |
| SFR | M⊙ yr−1 | 740±100 | 3640±500 |
| sSFR | Gyr−1 | 53±22 | 45±20 |
| AV − ISM | mag | 1.3±0.3 | 5.0±0.4 |
| AV − BC | mag | 4.3±1.6 | 5.0±0.9 |
| FHα | ×10−18 ergs−1 cm−2 | 5.2±2.2 | 1.2±0.5 |
| FPaβ | ×10−18 ergs−1 cm−2 | 2.3±0.4 | 1.6±0.4 |
| EWPaβ | 10−3 μm (rest-frame) | 5±1 | 4±2 |
| FPaα | ×10−18 erg s−1 cm−2 | 8.8±1.3 | 10±2 |
| LIR | ×1012 L⊙ | 5.3±0.7 | 28±4 |
Notes. AV − BC and AV − ISM are the visual (λ = 550 nm) attenuation of the birth cloud and interstellar medium components of the dust attenuation curve, respectively. The nebular emission and young stars (< 10 Myr) are attenuated with an AV equal to the sum of the AV − BC and AV − ISM, and older stars (> 10 Myr) with an AV equal to AV − ISM. FHα, FPaβ, and FPaα are the Hα, Paβ, and Paα observed fluxes derived from the SED fitting analysis. The SFR, M*, and LIR were corrected for magnification.
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