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Dust emission, an important diagnostic of star formation and ISM massthroughout the Universe, can be powered by sources unrelated to ongoing starformation. In the framework of the DustPedia project we have set out todisentangle the radiation of the ongoing star formation from that of the olderstellar populations. This is done through detailed, 3D radiative transfersimulations of face-on spiral galaxies. In this particular study, we focus onNGC 1068, which contains an active galactic nucleus (AGN). The effect ofdiffuse dust heating by AGN (beyond the torus) was so far only investigated forquasars. This additional dust heating source further contaminates the broadbandfluxes on which classic galaxy modelling tools rely to derive physicalproperties. We aim to fit a realistic model to the observations of NGC 1068 andquantify the contribution of the several dust heating sources. Our model isable to reproduce the global spectral energy distribution of the galaxy. Itmatches the resolved optical and infrared images fairly well, but deviates inthe UV and the submm. We find a strong wavelength dependency of AGNcontamination to the broadband fluxes. It peaks in the MIR, drops in the FIR,but rises again at submm wavelengths. We quantify the contribution of the dustheating sources in each 3D dust cell and find a median value of 83% for thestar formation component. The AGN contribution is measurable at the percentagelevel in the disc, but quickly increases in the inner few 100 pc, peaking above90%. This is the first time the phenomenon of an AGN heating the diffuse dustbeyond its torus is quantified in a nearby star-forming galaxy. NGC 1068 onlycontains a weak AGN, meaning this effect can be stronger in galaxies with amore luminous AGN. This could significantly impact the derived star formationrates and ISM masses for such systems.

High-resolution, 3D radiative transfer modelling IV. AGN-powered dust heating in NGC 1068