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Table 3.
Input parameters used to fit the SEDs of our sample.
| Parameter | Values |
|---|---|
| Star formation history | |
| Delayed with a recent burst | |
| Stellar age (a) | Redshift-dependent (0.5, 1, 2, 3, 5, 6, 8 Gyr) |
| e-folding time | 1, 3, 6 Gyr |
| Age of recent burst | 5, 10, 50, 100, 200, 300 Myr |
| Strength of the burst | 0.001,0.005,0.01,0.2,0.3 |
| Dust attenuation laws | |
| (Calzetti et al. 2000) | |
| Colour excess of young stars E(B − V) | 0.1 – 1 by a bin of 0.1 |
| fatt(b) | 0.3, 0.5, 0.8, 1.0 |
| (Charlot & Fall 2000), (Lo Faro et al. 2017) | |
V-band attenuation in the ISM  |
0.3 – 6 by a bin of 0.1 |
Av /( ) |
0.3, 0.5, 0.8, 1 |
| Power law slope of the ISM | −0.7, −0.48 (c) |
| Power law slope of the BC | −0.7 |
| Dust emission | |
| (Draine et al. 2014) | |
| Mass fraction of PAH | 1.77, 2.50, 3.19 |
| Minimum radiation field Umin | 10, 25, 30, 40 |
| Power law slope α | 2 |
| Synchrotron emission | |
| FIR/radio correlation coefficient | 2.2, 2.4. 2.6 |
| Power law slope slope | 0.3, 0.6, 0.9 |
Notes.
(c)
Power law slope of LF17.
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