Table 2.
Grids of input parameters used in CIGALE for the best-fit model computation of both the lens and submillimeter components of a SED.
| Parameter | Lens component | SMG component |
|---|---|---|
| SFH | delayedbq (Ciesla et al. 2017) | delayedbq (Ciesla et al. 2017) |
| e-folding time of the main stellar population, τmain (Myr) | 200, 500, 750, 1000, 1500 | 2000, 3000, 5000 |
| Age of the main stellar population, tmain (Myr) | 5000, 6000, 7000, 8000, 9000, 10000 | 1000, 1500, 2000, 3000, 4000 |
| Age of the late burst/quench episode, tbq (Myr) | 200 | 10, 20, 100 |
| Ratio of the SFR after/before tbq, rSFR | 0.01, 0.1, 0.3 | 1.5, 3, 10, 20, 30 |
| Stellar population model | Bruzual & Charlot (2003) | Bruzual & Charlot (2003) |
| IMF | Chabrier (2003) | Chabrier (2003) |
| Metallicity (Z⊙) | 0.02 | 0.008 |
| Dust attenuation | Calzetti et al. (2000) | Calzetti et al. (2000) |
| Color excess of the nebular lines light, E(B − V)lines | 0.001, 0.003, 0.0075 | 1.0, 1.2, 1.4, 1.6 |
| E(B − V)old/E(B − V)young | 0.25, 0.50, 0.75 | 0.25, 0.5, 0.75 |
| Slope of the power law modifying the attenuation curve, δ | –1.0, –0.5, –0.25, 0.0 | 0.0 |
| Dust grain model | Draine et al. (2014) | Draine et al. (2014) |
| Mass fraction of PAHs, qPAH (%) | 0.47, 1.12 | 1.12, 3.19, 5.26, 7.32 |
| Minimum radiation field, Umin | 20 | 10, 20, 25, 30 |
| Power-law slope dU/dM, Uα | 2.0 | 2.0 |
| Fraction illuminated from Umin to Umax, γ | 0.01 | 0.02 |
| AGN model | – | Fritz et al. (2006) |
| Ratio of the maximum to minimum radii of the dust torus | – | 60 |
| Optical depth at 9.7μm, τ9.7 | – | 3.0 |
| β | – | –0.5 |
| γ | – | 0.0 |
| Opening angle of the dust torus (deg) | – | 100 |
| Angle between equatorial axis and line of sight (deg) | – | 10.1, 60.1 |
| δ | – | –0.36 |
| AGN fraction | – | 0.0, 10, 30, 50 |
| E(B-V) | – | 0.03 |
| Temperature of the polar dust (K) | – | 100 |
| Emissivity index of the polar dust | – | 1.6 |
| Redshift | z = 0.01 to 1.0, with Δz = 0.01 | z = 1.0 to 4.5, with Δz = 0.1 |
Notes. This configuration gives us a set of 648 000 models for the lenses and 1 555 200 for the SMGs. Moreover, an additional set of 53 222 400 parameters was created to perform SED analysis over the entire SED range by combining values from the individual components, and an optional AGN component was added for an additional run of the unlensed SMGs.
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