Open Access
Table A.1.
Parameters used for the CIGALE model SEDs used to estimate M★ and SFR. All ages and times are in Myr.
| Parameter | Value | Description |
|---|---|---|
| Star Formation History | ||
| τmain | 1000, 1800, 3000, 5000, 7000 | e-folding time (main) |
| τburst | 9, 13 | e-folding time (burst) |
| fburst | 0.00, 0.10, 0.20, 0.30 | Burst mass fraction |
| Age | 1000, 1500, 2000, 2500, 3000, 3500, | Population age (main) |
| 4000, 4500, 5000, 5500, 6000, 6500, | ||
| 7000, 7500, 8000, 8500, 9000, 9500, | ||
| 10000, 10500, 11000, 11500, 12000, | ||
| 13000 | ||
| Burst Age | 1, 10, 30, 100, 300 | Population age (burst) |
| Stellar Emission (Bruzual & Charlot 2003) | ||
| IMF | Chabrier (2003) | Initial Mass Function |
| Z | 0.02 | Metallicity (0.02 is Solar) |
| Separation Age | 10 | Separation between young and old stellar populations |
| Dust Attenuation (Modified Charlot & Fall 2000) | ||
| AVBC | 0.3, 1.2, 2.3, 3.3, 3.8 | V-band attenuation of the birth clouds |
| μ | 0.23, 0.33, 0.44, 0.5 | AvISM / (AvBC+AvISM) |
| SlopeBC | -0.7 | Birth cloud attenuation power law slope |
| SlopeISM | -0.7 | ISM attenuation power law slope |
| Dust Emission (Draine et al. 2014) | ||
| qPAH | 0.47, 1.12, 2.50, 3.9 | Mass fraction of PAH |
| Umin | 5.0, 10.0, 25.0 | Minimum scaling factor of the radiation field intensity |
| α | 2.0 | Dust power law slope |
| γ | 0.02 | Illuminated fraction |
| AGN (Fritz et al. 2006) | ||
| rratio | 60 | Ratio of the maximum to minimum radii of the dust torus |
| τ | 1.0, 6.0 | Optical depth at 9.7 microns |
| β | -0.5 | Beta |
| γ | 0.0 | Gamma |
| openingangle | 100 | Opening angle of the dust torus |
| psy | 0.001, 89.990 | Angle between equatorial axis and line of sight |
| disktype | 1 | Disk spectrum (1 is Schartmann et al. 2005) |
| δ | -0.36 | Power-law of index δ modifying the optical slop of the disk. |
| fracAGN | 0.0, 0.1, 0.3, 0.5, 0.7 | AGN fraction |
| lambdafracAGN | 0/0 | Wavelength range in microns where to compute the AGN fraction |
| law | 0 | Extinction law of the polar dust (0 = Small Magellanic Cloud) |
| EBV | 0.03 | E(B-V) for the extinction in the polar direction in magnitudes |
| temperature | 100 | Temperature of the polar dust in K |
| emissivity | 1.6 | Emissivity index of the polar dust |
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