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Table 3.
Input parameters for the code CIGALE.
| Parameters | Values |
|---|---|
| Star formation history | |
| Double exponential (delayed with additional burst) | |
| e-folding time of the main stellar population model (Myr) | 500, 1000, 3000, 5000, 8000, 10 000, 15 000, 20 000 |
| e-folding time of the late starburst population model (Myr) | 20 000 |
| Mass fraction of the late burst population | 0, 0.05, 0.1, 0.15, 0.2, 0.25, 0.3, 0.35,0.4, 0.45, 0.5 |
| Age of the main stellar population (Myr) | 6500 |
| Age of the late burst (Myr) | 10, 30 ( * ), 100 ( * ), 300, 1000, 3000, 5000 |
| 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 |
| Nebular | |
| Ionisation parameter | −3.0 |
| FULL–run: Dust attenuation law Calzetti et al. (2000) | |
| E(B − V): the colour excess of the stellar continuum light for the young population | 0, 0.01, 0.02, 0.05, 0.1, 0.15, 0.2, 0.25, 0.3, 0.35, 0.4, 0.5, 0.6, 0.7, 0.8 |
| Amplitude of the UV bump at 217.5 nm | 0, 2.0, 4.0, 6.0 |
| Slope of the power law modifying the attenuation curve | 0.4, 0.2, 0, −0.2, −0.4, −0.6, −0.8, −1., −1.2 |
| LIGHT–run: Dust attenuation law Calzetti et al. (2000) | |
| E(B − V): the colour excess of the stellar continuum light for the young population | 0, 0.05, 0.15, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8 |
| Amplitude of the UV bump at 217.5 nm | 0 |
| Slope of the power law modifying the attenuation curve | 0 |
Notes. ( * )Values 30 and 100 was removed from the LIGHT–run.
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