Table B.1.
CIGALE parameters used for the SED fitting.
| Parameter | Values | Description |
|---|---|---|
| SFH (sfhdelayedbq) | ||
| τmain | 0.2, 0.3, 0.5, 0.7, 1.0, 1.5, 2.0, 3.0, 4.0, 5.0 [Gyr] | e-folding time of the main stellar population |
| 0.15, 0.2, 0.3, 0.5, 0.7, 1.0, 1.5 [Gyr] | ||
| agemain | 0.5, 0.7, 1.0, 1.5, 2.0, 3.0, 4.0, 5.0 [Gyr] | Age of the main stellar population in the galaxy |
| 0.2, 0.3, 0.5, 0.7, 1.0, 1.5 [Gyr] | ||
| agebq | 0.01, 0.03, 0.05, 0.1 [Gyr] | Age of the burst/quench episode |
| rsfr | 0.1, 0.2, 0.5, 1, 2, 5 | Ratio of the SFR after/before age_bq |
| 0.1, 0.5, 1, 2, 5, 10, 30, 50 | ||
| Stellar component (bc03) | ||
| IMF | 1 | Initial mass function: 1 (Chabrier 2003) |
| Z | 0.008, 0.02 | Metallicity |
| 0.0004, 0.008, 0.02 | ||
| Separation age | 10 [Myr] | Age of the separation between |
| the young and the old star populations | ||
| Nebular emission (nebular) | ||
| logU | -3.0, -2.0, -1.0 | Ionization parameter |
| -2.0, -1.0 | ||
| zgas | 0.008, 0.02 | Gas metallicity |
| 0.0004, 0.008, 0.02 | ||
| ne | 100 | Electron density |
| 100, 1000 | ||
| Dust attenuation (dustatt_modified_cf00) | ||
A |
0.01, 0.1, 0.3, 0.5, 0.7, 1.0, 1.5, 2.0, 3.0, 4.0 | V-band attenuation in the interstellar medium |
| μ | 0.44 | Ratio of the BC-to-ISM attenuation |
| slope ISM | -0.7 | Power law slope of the attenuation in the ISM |
| slope BC | -1.3 | Power law slope of the attenuation in the BC |
| Dust emission (dale2014) | ||
| fracAGN | 0.0 | AGN fraction |
| α | 2.0 | Slope of the dust emission |
| AGN component (skirtor2016) | ||
| rratio | 20.0 | Ratio of the outer to inner radius of the dusty torus |
| τ | 3.0 | Equatorial optical depth at 9.7 μm |
| i | 50, 60, 70, 80 | Angle between equatorial axis and line of sight |
| fAGN | 0.1, 0.2, 0.3, 0.4, 0.5, 0.6, 0.7 | AGN fraction at 0.1-1.0 μm |
| EBV | 0.04 | E(B-V) for the extinction in the polar direction in magnitudes |
Notes. The first column reports the name of the templates as well as each individual parameter. In the second column, the parameters are listed, and in the third column, the descriptions of the parameters are provided. In cases where the grid is different for galaxies at z > 3, the values are reported in italics.
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