Table 2.
Physical properties of LH-SBC3 members.
| ID | S150 MHz | log10M⋆ | SFR |
|---|---|---|---|
| (μJy) | (M⊙) | (M⊙ yr−1) | |
| a | 1519 ± 46 | 11.10 |
1247 ± 82 |
| b | 68 ± 33 | 10.58 |
1947 ± 128s |
| c | 59 ± 33 | 10.75 |
392 ± 26 |
| d | < 66 | 10.23 |
734 ± 48 |
Notes. Fluxes at 150 MHz are measured by LeBail et al. (in prep.) using PYBDSF1. Stellar masses are derived from optical to mid-IR SED fitting assuming a delayed star formation history using FAST++. SFRs are obtained by scaling the total SFR of the structure with the 3 mm fluxes of individual members. See details in Sect. 3.1 (https://pybdsf.readthedocs.io/en/latest/).
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