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Table 1.
CIGALE grid parameter values adopted for the modelling described.
Parameter | Values | Description |
---|---|---|
Star formation history (SFH): Delayed | ||
τmain | 5–8000 (in steps of 10) | e-folding time of the main stellar population model (Myr). |
Age | 200–13 260 (in steps of 10) | Age of the oldest stars in the galaxy (Myr). |
Single-age stellar population (SSP): Bruzual & Charlot (2003) | ||
imf | 1 | Initial mass function Chabrier (2003) |
Metallicity | 0.02 | solar |
Separation Age | 10 | Age of the separation (to differentiate) between the young and the old star populations (Myr). |
Dust attenuation: Calzetti et al. (2000) | ||
E(B − V)young | 0.015, 0.02, 0.04, 0.06, 0.1, 0.2, 0.3, 0.9, 1.0 | Color excess of the stellar continuum light for the young population. |
Dust emission: dl2014 | ||
Qpah | 1.12, 1.77, 2.50, 3.19 | Mass fraction of PAH |
Umin | 5.0, 6.0, 7.0, 8.0, 10.0, 12.0, 15.0, 17.0, 20.0, 25.0 | Minimum radiation field |
Alpha | 2.0, 2.1, 2.2, 2.3, 2.4, 2.5, 2.6, 2.7, 2.8 | the power-law distribution (dMd ∝ U−αdU) |
Gamma | 0.02 | Fraction illuminated from Umin to Umax |
AGN model: Fritz et al. (2006) | ||
Rmax/Rmin | 30.0, 60.0, 100.0, 150.0 | Ratio of the maximum to minimum radii of the dust torus. |
τ | 0.3, 0.6, 1.0, 2.0, 3.0, 6.0, 10.0 | Optical depth at 9.7 μm. |
β | −1.00, −0.75, −0.50, −0.25, 0.00 | Beta from the power-law density distribution for the radial component of the dust torus (Eq. (3) of Fritz 2006). |
γ | 0.0, 2.0, 4.0, 6.0 | Gamma from the power-law density distribution for the polar component of the dust torus (Eq. (3) of Fritz et al. 2006). |
Opening angle (θ) | 60.0, 100.0, 140.0 | Full opening angle of the dust torus (Fig. 1 of Fritz et al. 2006). |
ψ | 0.001, 10.1, 20.1, 30.1, 70.1, 89.990 | Angle between equatorial axis and line of sight. |
fAGN | 0.0, 0.05, 0.1, 0.15, 0.2, 0.25, 0.3, 0.35, 0.4, 0.45, 0.5, 0.55, 0.6, 0.65, 0.7, 0.75, 0.8, 0.85, 0.9, 0.95, 0.99 | Fraction of AGN torus contribution to the IR luminosity (fracAGN in Eq. (1) of Ciesla et al. 2015) |
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