Table E.5.
Input parameter values used for the SED-fitting procedure in Appendix D.
| Template | Parameter | Value and range | Description |
|---|---|---|---|
| Stellar emission | IMF | Chabrier (2003) | |
| Z | 0.02 | Metallicity | |
| Separation age | 10 Myr | Separation age between the young | |
| and the old stellar populations | |||
| Delayed SFH | Age | 0.10, 0.25, 0.5, 1.0, 1.5, 2.0, 2.5 Gyr | Age of the oldest SSP |
| τ | 0.10, 0.25, 0.5, 1.0, 3.0, 5.0, 10.0 Gyr | e-folding time of the SFH | |
| Attenuation law | E(B − V) | 0.05, 0.1, 0.3, 0.5, 0.7, 0.9, 1.1, 1.3 | Attenuation of the |
| young stellar population | |||
| Modified Calzetti | Reduction factor | 0.93 | Differential reddening applied to |
| the old stellar population | |||
| δ | -0.6, -0.4, -0.2, 0.0 | Slope of the power law multiplying | |
| the Calzetti attenuation law | |||
| Dust emission | αSF | 0.5, 1.0, 1.5, 2.0, 2.5, 3.0 | Slope of the power law combining |
| the contribution of different dust templates | |||
| AGN emission | Rmax/Rmin | 60 | Ratio of the outer and inner radii |
| τ9.7 | 0.6, 3.0, 6.0 | Optical depth at 9.7 μm | |
| β | 0.00, -0.5, -1.0 | Slope of the radial coordinate | |
| γ | 0.0, 6.0 | Exponent of the angular coordinate | |
| Θ | 100 degrees | Opening angle of the torus | |
| ψ | 0, 10, 20, 30, 40, 50, 60, 70, 80, 90 degrees | Inclination of the observer’s line of sight | |
| fAGN | 0.05, 0.1, 0.15, 0.2, 0.25, 0.3, 0.35, 0.4, 0.45, | AGN fraction | |
| 0.5, 0.55, 0.6, 0.65, 0.7, 0.75, 0.8, 0.85, 0.9 | |||
| AGN intrinsic | Γ | 1.8a, b, 1.9a, b, 2.4a, b, 3a, b | Intrinsic X-ray photon index |
| X-ray emission | |||
| Nebular emission | U | 10−2 | Ionization parameter |
| fesc | 0% | Fraction of Lyman continuum | |
| photons escaping the galaxy | |||
| fdust | 10% | Fraction of Lyman continuum | |
| photons absorbed by dust | |||
Notes. We divided the sample in different runs of CIGALE based on the photon index value obtained from the X-ray catalogs or X-ray fits to reduce the computational time. b Input values used only for cdfs_313 and cdfs_794, which are AGN Type 1 with very steep intrinsic photon index (Luo et al. 2017).
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