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Table 3
Parameter ranges used in the blind fitting procedure.
| Parameter | Symbol | Values |
|
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||
| Star formation history | ||
| Metallicity | Z | 0.02 |
| IMF | Salpeter | |
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| Double exponentially decreasing | ||
| τ of old stellar population models (Gyr) | τ1 | 1, 3, 5 |
| Age of old stellar population models (Gyr) | t1 | 1, 2, 3, 4, 5 |
| τ of young stellar population models (Gyr) | τ2 | 10 |
| Age of young stellar population models (Gyr) | t2 | 0.01, 0.03, 0.1, 0.3 |
| Mass fraction of young stellar population | fySP | 0.001, 0.01, 0.1, 0.2 |
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| Single exponentially decreasing | ||
| τ of stellar population models (Gyr) | τ | 0.5, 1, 3, 5, 10 |
| Age of stellar population models (Gyr) | t | 1, 2, 3, 4, 5 |
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| Delayed SFH | ||
| τ of stellar population models (Gyr) | τ | 0.5, 1, 3, 5, 10 |
| Age (Gyr) | t | 4, 5, 5.5 |
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| Dust Attenuation | ||
| Colour excess of stellar continuum light for the young population | E(B − V)∗ | 0.05, 0.1, 0.15, 0.2, 0.25, 0.3, 0.35, 0.4, 0.5, 0.6 |
| E(B − V)∗ reduction factor between old and young populations | fatt | 0.44 |
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| Dust template | ||
| IR power-law slope | α | 1.5, 2, 2.5 |
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| AGN emission | ||
| Ratio of dust torus radii | Rmax/Rmin | 30, 100 |
| τ9.7 | 0.3, 3.0, 6.0, 10.0 | |
| β | –0.5 | |
| γ | 0.00 | |
| ψ | 0.001, 50.100, 89.990 | |
| Opening angle of the torus | θ | 100 |
| Fraction of LIR due to the AGNa | frac AGN | –0.2, –0.15, –0.1, –0.05, 0.0, 0.05, 0.1, 0.15, 0.2 |
| 0.25, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8 | ||
Notes.
(a)
We use low negative values of fracAGN in order to minimize a bias due to PDF analysis, as explained in Sect. 3.2.1.
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