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We describe the calculation of the stochastically heated dust emission usingthe 3D ray-tracing dust radiative transfer code DART-Ray, which is designed tosolve the dust radiative transfer problem for galaxies with arbitrarygeometries. In order to reduce the time required to derive the non-equilibriumdust emission spectra from each volume element within a model, we implementedan adaptive SED library approach, which we tested for the case of axisymmetricgalaxy geometries. To show the capabilities of the code, we applied DART-Ray toa high-resolution N-body+SPH galaxy simulation to predict the appearance of thesimulated galaxy at a set of wavelengths from the UV to the sub-mm. We analysethe results to determine the effect of dust on the observed radial and verticalprofiles of the stellar emission as well as on the attenuation and scatteringof light from the constituent stellar populations. We also quantify theproportion of dust re-radiated stellar light powered by young and old stellarpopulations, both bolometrically and as a function of infrared wavelength.

Predicting the stellar and non-equilibrium dust emission spectra of high-resolution simulated galaxies with DART-Ray