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Within the framework of the DustPedia project we investigate the propertiesof cosmic dust and its interaction with the stellar radiation (originating fromdifferent stellar populations) for 814 galaxies in the nearby Universe, allobserved by the Herschel Space Observatory. We take advantage of the widelyused galaxy SED fitting code CIGALE, properly adapted to include thestate-of-the-art dust model THEMIS. Using the DustPedia photometry we determinethe physical properties of the galaxies, such as, the dust and stellar mass,the star-formation rate, the bolometric luminosity as well as the unattenuatedand the absorbed by dust stellar light, for both the old (> 200 Myr) and young(<= 200 Myr) stellar populations. We show how the mass of stars, dust, andatomic gas, as well as the star-formation rate and the dust temperature varybetween galaxies of different morphologies and provide recipes to estimatethese parameters given their Hubble stage (T). We find a mild correlationbetween the mass fraction of the small a-C(:H) grains with the specificstar-formation rate. On average, young stars are very efficient in heating thedust, with absorption fractions reaching as high as ~77% of the total,unattenuated luminosity of this population. On the other hand, the maximumabsorption fraction of old stars is ~24%. Dust heating in early-type galaxiesis mainly due to old stars, up to a level of ~90%. Young stars progressivelycontribute more for `typical' spiral galaxies and they become the dominantsource of dust heating for Sm type and irregular galaxies, donating up to ~60%of their luminosity to this purpose. Finally, we find a strong correlation ofthe dust heating fraction by young stars with morphology and the specificstar-formation rate.

Old and young stellar populations in DustPedia galaxies and their role in dust heating