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Table A.1.
Input parameters used in SED fitting with CIGALE.
Parameter | Values |
---|---|
Delayed star formation history | |
e-folding time of the main stellar population model (Myr) | 100, 300, 500, 1500 |
Age of the main stellar population | 300, 500, 800, 1000, 2500, |
in the galaxy (Myr) | 3500, 4500, 6000, 7000 |
e-folding time of the late starburst population model (Myr) | 10000 |
Age of the late burst (Myr) | 10 |
Mass fraction of the late burst population | 0 |
Normalise the SFH to produce one solar mass | True |
Stellar population synthesis Bruzual & Charlot (2003) | |
Initial mass function | Chabrier (2003) |
Metalicity | 0.02 |
Age of the separation between the young and the old star populations (Myr) | 10 |
Dust emission Dale et al. 2014 | |
AGN fraction | 0 |
α slope | 2.0 |
Dust attenuation Charlot & Fall (2000) | |
V-band attenuation in the interstellar medium | 0.0, 0.05, 0.1, 0.2, 0.4, 0.75, |
1.0, 1.5, 1.75, 2.0, 2.2, 2.5, 3.0 | |
μ | 0.8 |
Power law slope of the attenuation in the ISM | -0.7 |
Power law slope of the attenuation in the birth clouds | -0.7 |
Dust attenuation Calzetti et al. (2000) | |
E(B-V)l | 0.0,0.05, 0.1, 0.2, 0.3, 0.4, 0.5, |
0.6, 0.7, 0.8,0.9, 1.0 ,1.3, 1.5 | |
E_BV factor | 0.44 |
Central wavelength of the UV bump in nm | 217.5 |
Width (FWHM) of the UV bump in nm | 35.0 |
Amplitude of the UV bump | 0 |
Slope delta of the power law modifying the attenuation curve | 0 |
Extinction law to use for attenuating the emission lines flux | Milky Way |
Ratio A_V / E(B-V) | 3.1 |
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