Table 2
Grid of spectral energy distributions.
| Parameter | Values |
|
|
|
| Stellar population: | BC03 (Bruzual & Charlot 2003) based on |
| STELIB (Le Borgne et al. 2003) | |
| (BC03 based on BaSeL3.1 | |
| (Westera et al. 2002)) | |
| Nebular emission: | Recipe based on Schaerer & de Barros (2009); |
| Ono et al. (2010) | |
| IMF | Salpeter 0.1 − 100 M⊙ |
| Metallicities Za | 0.008, 0.02, 0.05 (0.004, 0.008, 0.02, 0.05) |
| log 10(Age [ yr ]) b | 6–9.9 with 14 steps |
| (7–9.8 in steps of 0.1) | |
| f cov c | 0 (0.7,1) |
| ES(B − V) d | 0.2 (0.0 − 1.0 in steps of 0.02) |
| SFH: log 10(τ [ yr ]) | 8,∞ (7.9 − 10.5 in steps of 0.2) |
| α e | None (1.75) |
Notes. Two different grids are listed. One was used for testing biases from the continuum estimation. The other one was used for SED fitting and is given in parentheses.
We assume that the covering fraction of the gas, fcov, is related to the escape of the ionizing radiation, fesc;ion, through fesc;ion = 1 − fcov.
Stellar extinction assuming Calzetti et al. (2000) extinction law. The stellar extinction is assumed to be a factor 0.7 lower than the nebular extinction.
Parameter α of Dale & Helou (2002) models used for dust emission.
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