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Table 2.
Input parameters for the code CIGALE.
| Parameters | Values |
|---|---|
| Star formation history: | |
| Delayed star formation history + additional burst | |
| e-folding time of the main stellar population model (Myr) | 1000, 3000, 5000 |
| e-folding time of the late starburst population model (Myr) | 50.0, 100 |
| Mass fraction of the late burst population | 0.0, 0.005, 0.015, 0.02, 0.05, 0.1, 0.15, 0.20 |
| Age (Myr) | 8000, 9000, 10 000, 11 000, 12 000 |
| Age of the late burst (Myr) | 100, 150 |
| Single stellar population Bruzual & Charlot (2003) | |
| Initial mass function | Chabrier (2003) |
| Metallicities (solar metallicity) | 0.02 |
| 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 | 0.1, 0.3, 0.5, 0.7, 0.9 |
| E(B − V)f: reduction factor to compute the E(B − V) for the stellar continuum attenuation | 0.3, 0.5, 0.8, 1 |
| Dust emission: Dale et al. (2014) | |
| Fraction of AGN | 0 |
| α slope | 2.0 |
| AGN (UV-to-IR): Stalevski et al. (2016) | |
| Inclination, i.e., viewing angle (i) | 30, 70 |
| AGN contribution to UV luminosity (f0.25 μm) | 0.0, 0.001, 0.0025, 0.005, 0.0075, 0.01, |
| 0.025, 0.05, 0.075, 0.1, 0.2, 0.3, 0.4, | |
| 0.5, 0.6, 0.7 | |
| Polar-dust color excess (E(B − V)) | 0, 0.2, 0.4 |
| X-ray emission: Yang et al. (2020, 2022) | |
| Photon index of the AGN intrinsic X-ray spectrum (gam) | 1.8 |
| Power-law slope connecting Lν at rest-frame 2500 Å and 2 keV (αox) | −1.9, −1.7, −1.5, −1.3, −1.1, −0.9 |
| Maximum allowed deviation of αox from the empirical αox − Lν (2500 Å) | 0.2 |
| Deviation from the expected LMXB scaling relation (δLMXB) | 0.0 |
| Deviation from the expected HMXB scaling relation (δHMXB) | 0.0 |
Notes. The input values used for better sampling the f0.25 μm are in boldface type (see Sect. 5.1).
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