Table A.1
Choices of the SED model components and parameters in the 16 CIGALE runs.
| star-formation history | ||
| delayed τ+starburst | e-folding time of the main population | 500, 1000, 3000, 5000, 8000 Myrs |
| age the main population | 500, 1000-13 000 (step 1000) Myrs | |
| e-folding time of the late starburst population | 9000, 13 000 Myrs | |
| age of the late starburst population | 1, 30, 100, 500 Myrs | |
| mass fraction of the late starburst population | 0.01, 0.05, 0.1, 0.2 | |
| double exponential | e-folding time of the main population | 1000-9000 (step 2000) Myrs |
| age the main population | 500, 1000-13 000 (step 1000) Myrs | |
| e-folding time of the late starburst population | 10000 Myrs | |
| age of the late starburst population | 1, 30, 100, 500 Myrs | |
| mass fraction of the late starburst population | 0.01, 0.05, 0.1, 0.2 | |
| dust attenuation | ||
| modified Charlot and Fall 2000 | V-band attenuation in the interstellar medium | 0.1, 0.5-3.5 (step 0.5) |
| AvISM/ Av BC+AvISM | 0.25, 0.5, 0.75 | |
| power-law slope of the attenuation in the birth clouds | -0.7 | |
| power-law slope of the attenuation in the ISM | -0.7 | |
| modified Calzetti 2000 | color excess | 0.01, 0.05, 0.1, 0.2, 0.3, 0.4,0.5 |
| reduction factor | 0.25, 0.5, 0.75 | |
| Slope of the power law modifying the attenuation curve | -0.5, -0.4, -0.3, -0.2, −0.1, 0 | |
| Extinction law | Milky Way | |
| dust emission | ||
| Draine et al. 2014 | Mass fraction of PAH | 0.47 |
| minimum radiation field | 5, 15, 25 | |
| power-law slope α in dM/dU ∝ Uα | 2 | |
| Fraction illuminated from min to max radiation field | 0.02 | |
| Dale et al. 2014 | alpha slope | 1.5-4 (step 0.5) |
| AGN templates | ||
| Fritz et al. 2006 | Full opening angle of the dust torus (degree) | 100 |
| viewing angle (degree) | 0.001, 50.1, 89.990 | |
| AGN fraction | 0, 0.1, 0.3, 0.5, 0.7 | |
| optical depth at 9.7 μm | 0.3, 1, 6 | |
| linked to the radial dust distribution in the torus | -0.5 | |
| linked to the angular dust distribution in the torus | 0 | |
| SKIRTOR | optical depth at 9.7 μm | 7 |
| torus density radial parameter p | 1 | |
| torus density angular parameter q | 1 | |
| half opening angle (degree) | 40 | |
| viewing angle (degree) | 30, 70 | |
| AGN fraction | 0, 0.1, 0.3, 0.5, 0.7 | |
| extinction law of polar dust | SMC | |
| E(B-V) of polar dust | 0, 0.1, 0.2, 0.3, 0.4 | |
| temperature of polar dust | 100 | |
| emissivity of polar dust | 1.6 | |
Notes. The 16 CIGALE runs involve all possible combinations of two star-formation history models (delayed τ + starburst or double exponential), two dust attenuation models (modified Charlot & Fall (2000) or modified Calzetti et al. (2000) attenuation law), two dust emission models (IR SED templates from the Draine et al. (2014) model or the Dale et al. (2014) model), and two AGN models (smooth AGN templates from Fritz et al. (2006) or clumpy AGN templates from the SKIRTOR model in Stalevski et al. (2012)).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.