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Table 2.
CIGALE modules and input parameters used for all the fits.
| Parameters | Symbol | Range (Ph. 1, Hi-z LBGs) | Range (Ph. 2, | Range (Ph. 3, Hi-z | Range (Ph. 4, Hi-z |
|---|---|---|---|---|---|
| Low-zZ) | LBGs) | LBGs) | |||
| Target sample | Individual Hi-z LBGs | Individual Low-zZ | Combined Hi-z LBGs | Individual Hi-z LBGs | |
| Delayed SFH and recent burst | |||||
| e-folding timescale of the delayed SFH | τmain [Myr] | 25, 50, 100, 250, 500, 1000 | 25, 50, 100, 250, 500, 1000 | 25, 50, 100, 250, 500, 1000 | 25, 50, 100, 250 |
| Age of the main population | Agemain[Myr] | 61 log values in [2–1000] | 61 log values in | 17 log values in | 101 log values in |
| [2–1500] | [1, 800] | [50, 1260] | |||
| Burst | fburst | No burst | No burst | No burst | No burst |
| SSP | |||||
| SSP | BC03 | BC03 | BC03 | BC03 | |
| Initial mass function | IMF | Chabrier | Chabrier | Chabrier | Chabrier |
| Metallicity | Z | 0.004 | 0.004 | 0.004 | 0.004 |
| Nebular emission | |||||
| Ionisation parameter | logU | −1.5 | −1.5 | −1.5 | −1.5 |
| Line width [km s−1] | – | 100 | 100 | 100 | 100 |
| Dust attenuation law | |||||
| Colour excess for both the | E_BV_lines | 61 log values in [0.001, 0.3] | 61 log values in | 11 log values in | 101 log values in |
| old and young stellar popu | [0.001, 1.0] | [1e−3, 1e0] | [1e−3, 1e0] | ||
| lations | |||||
| Bump amplitude | uv_bump_amplitude | 0.0 | 0.0 | 0.0 | 0.0 |
| Power law slope | power law_slope | −0.7, −0.35, 0.0, 0.35, 0.7 | 0.0 | 0.0 | 0.0 |
| Dust emission | |||||
| Mass fraction of PAH | qPAH | 0.47,1.12, 1.77, 2.50, 3.19 | 0.47,1.12, 1.77, 2.50, 3.19 | 0.47 | 0.47 |
| Minimum radiation field | Umin | 0.1, 0.5, 1.0, 5.0, 10.0, 50.0 | 0.1, 0.5, 1.0, 5.0, 10.0, 50.0 | 4.0 | 4.0 |
| Power law slope dU/dM ≈ Uα | α | 2.0, 2.2, 2.4, 2.6, 2.8, 3.0 | 2.0, 2.2, 2.4, 2.6, 2.8, 3.0 | 2.2 | 2.2 |
| Dust fraction in PDRs | γ | 0.00, 0.01, 0.1, 0.2, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8, 0.9, 1.0 | 0.00, 0.01, 0.1, 0.2, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8, 0.9, 1.0 | 0.75 | 0.75 |
Notes. Note that we did not include any AGN emission.
References. BC03: Bruzual & Charlot (2003); Chabrier IMF: Chabrier (2003).
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