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Interstellar dust in galaxies can be traced either through its extinctioneffects on the star light, or through its thermal emission at infraredwavelengths. Recent radiative transfer studies of several nearby edge-ongalaxies have found an apparent inconsistency in the dust energy balance: theradiative transfer models that successfully explain the optical extinctionunderestimate the observed fluxes by an average factor of three. We investigatethe dust energy balance for IC4225 and NGC5166, two edge-on spiral galaxiesobserved by the Herschel Space Observatory in the frame of the H-ATLAS survey.We start from models which were constrained from optical data and extend themto construct the entire spectral energy distribution of our galaxies. Thesepredicted values are subsequently compared to the observed far-infrared fluxes.We find that including a young stellar population in the modelling is necessaryas it plays a non-negligible part in the heating of the dust grains. While themodelling approach for both galaxies is nearly identical, we find two verydifferent results. As is often seen in other edge-on spiral galaxies, thefar-infrared emission of our radiative transfer model of IC4225 underestimatesthe observed fluxes by a factor of about three. For NGC5166 on the other hand,we find that both the predicted spectral energy distribution as well as thesimulated images match the observations particularly well. We explore possiblereasons for this difference and conclude that it is unlikely that one singlemechanism is the cause of the dust energy balance problem in spiral galaxies.We discuss the different approaches that can be considered in order to get aconclusive answer on the origin this discrepancy.

Dust energy balance study of two edge-on spiral galaxies in the Herschel-ATLAS survey