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Table 2

Range of values of the input parameters for dust and stellar emission, used for the SED fitting with CIGALE.

Parameter Range
Amount of dust attenuation E(B − V)a 0.1−1 mag
Attenuation curve B12, C00, SMC-like
IR templatesb, α 1−3
AGN fraction, fracAGN 0–0.5
Stellar populations
Age (old stellar population) tfc 2−11 Gyr
e-folding rate (old stellar population) τ 1−5 Gyr
Age (young stellar population) tySP 50−500 Myr
Stellar mass fractiondfySP 0.01−0.2

Notes.

(a)

E(B − V) corresponds to the attenuation of the youngest population and a reduction factor of 0.5 is applied to the color excess of stellar populations older than 107 years.

(b)

α is the exponent of the power-law distribution of dust mass over heating intensity (Dale et al. 2014).

(c)

tf is always lower than the age of the universe at the redshift of the source.

(d)

Stellar mass fraction produced with the young stellar population.

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