Fig. 11.

Distribution of the physical properties of the Brown et al. (2014) sample. We see that in a single run CIGALE can model galaxies with a wide range of properties: FUV attenuation, UV slope, IR-to-UV luminosity, dust luminosity, stellar mass, and SFR. This is only a small excerpt of the numerous physical properties that can also be estimated with CIGALE (see Appendix C).
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