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Table E.1.
Input parameters for the SED fitting code CIGALE.
| Parameter | Value |
|---|---|
| Exponential or Delayed star formation History | |
| e-folding time of the main stellar population model (Myr) | 50-15000 in step Δτ = 50 Myr |
| Age of the main stellar population (Myr) | 25-2000 in step Δ age = 5 Myr |
| Stellar population models: Bruzual & Charlot (2003) | |
| Initial mass function | Chabrier (2003) |
| Metallicities (in separate runs) | 0.008, 0.004, 0.020 |
| Age of the separation between the young and the old star population (Myr) | 10 |
| Dust attenuation law: Calzetti et al. (2000) | |
| E(B-V)l: color excess of the nebular lines | 0.0-0.75 in step ΔE(B−V)1 = 0.015 |
| E(B-V)f: reduction factor to compute the E(B-V) | |
| for the stellar continuum attenuation | 0.44 |
| Nebular Emission: Inoue (2011) | |
| Ionization parameter | -2.0 |
| Gas metallicity (set to be same as the stellar metallicity) | 0.008, 0.004, 0.020 |
| Fraction of Lyman continuum photons escaping the galaxy | 0.0 |
| AGN emission(a): Fritz et al. (2006) | |
| AGN fraction: contribution of the AGN to the total LIR | 0.0, 0.01, 0.1, 0.2, 0.3, |
| 0.4, 0.5, 0.6, 0.7, 0.8, 0.9 | |
| Opening angle of the dust torus | 10, 30, 60 |
| Angle between AGN axis and line of sight | 0.001, 89.9 |
| Optical depth at 9.7 | 1.0, 6.0 |
| X-ray emission(a): Yang et al. (2022) | |
| Photon index of the AGN intrinsic X-ray spectrum | 1.8 |
| Power-law slope connecting Lν at rest-frame 2500Å and 2keV (αox) | -1.9, -1.7, -1.5, -1.3, -1.1, -0.9 |
| Maximum allowed deviation of αox from the empirical αox − Lν (2500Å) | 0.2 |
| Deviation from the expected LMXB scaling relation (δLMXB) | 0.0 |
| Deviation from the expected HMXB scaling relation (δHMXB) | 0.0 |
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