Table 4.
Parameters used in CIGALE to model the SFH.
| Model | Parameter | Value |
|---|---|---|
| SFH | Age (Myr) | 11 000, 12 000, 13 000 |
| τmain (Myr) | 1000, 3000, 5000, 7000, 9000 | |
| Agebq (Myr) | 20, 50, 100, 300 | |
| rSFR | 0, 0.25, 0.5, 0.75, 1, 1.5, 2, 5, 10 | |
| Dust attenuation | E(B − V)lines (mag) | 0.005, 0.01, 0.025, 0.05, 0.075, 0.10, |
| 0.15, 0.20, 0.25, 0.30, 0.35, 0.40, | ||
| 0.45, 0.50, 0.55, 0.60, 0.65, 0.70 | ||
| E(B − V)factor | 0.25, 0.5, 0.75 | |
| UV bump wavelength (nm) | 217.5 | |
| UV bump width (nm) | 35.0 | |
| UV bump amplitude | 0.0, 1.5, 3.0 | |
| Δδ | −1.2, −1.1, −1.0,−0.9,−0.8,−0.7,−0.6,−0.5, | |
| −0.4,−0.3,−0.2,−0.1, 0, 0.1, 0.2 | ||
Notes. Parameters used in CIGALE to model the SFH (upper rows) and dust attenuation (lower rows). Meaning of the parameters: (a) SFH: Age – Age of the main stellar population in the galaxy, in Myr; τmain – e-folding time of the main stellar population model, in Myr; Agebq – Age of the burst or quench episode, in Myr; and rSFR – Ratio of the SFR after or before Agebq, values larger than one correspond to an enhancement of the SFR whereas values lower than one will correspond to a decrease; (b) Dust attenuation: E(B − V)lines – Colour excess of the nebular lines light for both the young and old population; E(B − V)factor – Reduction factor to apply on E(B − V)lines to compute E(B − V)s the stellar continuum attenuation. Both young and old populations are attenuated by E(B − V)s; UV bump wavelength – Central wavelength of the UV bump in nm; UV bump width – Width (FWHM) of the UV bump in nm; UV bump amplitude – Amplitude of the UV bump. For the Milky Way: 3; Δδ – Slope delta of the power law that modifies the attenuation curve.
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