Table 2.
CIGALE Spectral energy distribution fitting models and templates.
| Star formation history | ||
|---|---|---|
| Non-parametric: sfhNlevels (1) | ||
| age(a) [Myr] | [1578; 13753] | Age of the oldest stars in the galaxy in Myr; |
| 100 values linearly sampled. | ||
| 1st bin (b)[Myr] | 10 | Duration of the first bin in lookback time. |
| Nbins(c) | 10 | Number of bins in the SFH. |
| NSFH(d) | 2000 | Number of SFHs drawn for each age value. |
| Simple stellar population: BC03 (2) | ||
| IMF | Chabrier | Initial Mass Function |
| Z | 0.008, 0.02 | Metallicity |
| Attenuation: dust_att_modified_starburst (3) | ||
| E(B − V)s | [0, 1.8] | Color excess; 10 values linearly sampled |
| Dust emission: dale2014 (4) | ||
| α | 2.0 | Far-IR slope |
Notes.
This module selects an age from a linearly sampled range of 100 values between 1578 and 13753 Myr, which corresponds to the age of the Universe at the redshift of the galaxy.
For each sampled age value, 2000 SFHs are drawn, with the SFR amplitudes of each time-bin computed following a student-t distribution with continuity-burst priors (Leja et al. 2019; Tacchella et al. 2022).
References: (1) Ciesla et al. (2023); (2) Bruzual & Charlot (2003); (3) Calzetti et al. (2000); (4) Dale et al. (2014).
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