Table 4.
Stellar masses for MIRI/F1000W clumps with different star-forming histories.
| Region | M*[10 Myr] | M*[20 Myr] | M*[50–100 Myr] |
|---|---|---|---|
| (109 M⊙) | (109 M⊙) | (109 M⊙) | |
| (1) | (2) | (3) | (4) |
| EA | 1.4±0.5 | 1.9±0.7 | 4.2±1.8 |
| EB | 1.5±0.4 | 2.0±0.6 | 4.4±1.7 |
| EC | 1.6±0.5 | 2.2±0.7 | 4.9±1.9 |
| ED | 1.1±0.3 | 1.5±0.5 | 3.2±1.3 |
| EE | 1.1±0.3 | 1.5±0.5 | 3.2±1.3 |
| WA | 1.1±0.4 | 1.4±0.6 | 3.2±1.5 |
| WB | 1.0±0.3 | 1.4±0.4 | 3.1±1.2 |
| WC | 1.3±0.4 | 1.8±0.5 | 4.0±1.5 |
| WD | 1.5±0.4 | 2.0±0.6 | 4.5±1.6 |
Notes. Columns (2)–(4) give the extinction-corrected stellar mass based on the LJ luminosity and constant M/L ratios for a constant SFR over 10 Myr, 20 Myr, and 50−100 Myr, respectively. Extinction has been corrected assuming an AV of 2.4 and 2.2 for the E and W stellar components (see Sect. 4.3) and Calzetti’s extinction law (Calzetti et al. 2000).
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