Table 3.
Input parameters used to fit the SEDs of Astarte and Adonis with CIGALE.
| Parameter | Values | |
|---|---|---|
| Star formation history Ciesla et al. (2017) | ||
| Stellar age (i) | agemain | 0.8–3.2 Gyr by a bin of 0.2 Gyr |
| e-folding time (ii) | τmain | 0.8, 1, 3, 5, 8 Gyr |
| Age of burst/quench episode | tflex | 5, 10, 50, 100 Myr |
| SFR ratio after/before | rSFR | 10−2, 10−1, 0, 101, 102, 103 |
| Stellar synthesis population (Bruzual & Charlot 2003) | ||
| Initial mass function | IMF | (Chabrier 2003) |
| Metallicity | Z | 0.02 |
| Separation age | 10 Myr | |
| Dust attenuation laws | ||
| (Calzetti et al. 2000) | ||
| Colour excess of young stars | E(B − V) | 0.1–1 by a bin of 0.1 |
| Reduction factor (iii) | fatt | 0.3, 0.5, 0.8, 1.0 |
| (Charlot & Fall 2000), (Lo Faro et al. 2017) | ||
| V-band attenuation in the ISM |  |
0.3–3 by a bin of 0.1 |
 |
μ | 0.3, 0.5, 0.8, 1 |
| Power law slope of the ISM | −0.7, –0.48 | |
| Power law slope of the BC | −0.7 | |
| Dust emission model (Draine et al. 2014) | ||
| Mass fraction of PAH | qPAH | 1.77, 2.50, 3.19 |
| Minimum radiation field | Umin | 10, 25, 30, 40 |
| Power law slope | α | 2 |
| Synchrotron emission | ||
| Far-IR/radio correlation coefficient | 2.3–2.9 by a bin of 0.1 | |
| Power law slope slope | αsynchrotron | 0.4–0.9 by a bin of 0.1 |
Notes. (i) The stellar age is the age of the main stellar population. (ii) The e-folding time is the time required for the assembly of the majority of the stellar population. (iii) The reduction factor fatt is the color excess in old relative to young stars.
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.