Table 2.
Models and the values for their free parameters used by CIGALE for the SED fitting of our X-ray samples.
| Parameter | Model/values |
|---|---|
| Stellar population synthesis model | |
| Initial mass function | Salpeter |
| Metallicity | 0.02 (Solar) |
| Single stellar population library | Bruzual & Charlot (2003) |
| Double exponentially decreasing (2τ dec) model | |
| τ | 100, 1000, 5000, 10 000 |
| Age | 500, 2000, 5000, 10 000, 12 000 |
| Burst age | 100, 200, 400 |
| Dust extinction | |
| Dust attenuation law | Calzetti et al. (2000) |
| Reddening E(B − V) | 0.01, 0.1, 0.3, 0.5, 0.8, 1.2 |
| E(B − V) reduction factor between old and young stellar population | 0.44 |
| Fritz et al. (2006) model for AGN emiussion | |
| Ratio between outer and inner dust torus radii | 10, 60, 150 |
| 9.7 μm equatorial optical depth | 0.1, 0.3, 1.0, 2.0, 6.0, 10.0 |
| β | −0.5 |
| γ | 0.0, 2.0, 6.0 |
| Θ | 100 |
| Ψ | 0.001, 10.10, 20.10, 30.10, 40.10, 50.10, 60.10, 70.10, 80.10, 89.99 |
| AGN fraction | 0.1, 0.2, 0.3, 0.5, 0.6, 0.8 |
Notes.τ is the e-folding time of the main stellar population model in Myr, age is the age of the main stellar population in the galaxy in Myr (the precision is 1 Myr), and burst age is the age of the late burst in Myr (the precision is 1 Myr). β and γ are the parameters used to define the law for the spatial behaviour of density of the torus density. The functional form of the latter is ρ(r, θ) ∝ rβe−γ|cosθ|, where r and θ are the radial distance and the polar distance, respectively. Θ is the opening angle and Ψ the viewing angle of the torus. Type-2 AGN have Ψ = 0 and Type-1 AGN have Ψ = 90. The AGN fraction is measured as the AGN emission relative to infrared luminosity (1 − 1000 μm).
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