  We describe the calculation of the stochastically heated dust emission using
the 3D ray-tracing dust radiative transfer code DART-Ray, which is designed to
solve the dust radiative transfer problem for galaxies with arbitrary
geometries. In order to reduce the time required to derive the non-equilibrium
dust emission spectra from each volume element within a model, we implemented
an adaptive SED library approach, which we tested for the case of axisymmetric
galaxy geometries. To show the capabilities of the code, we applied DART-Ray to
a high-resolution N-body+SPH galaxy simulation to predict the appearance of the
simulated galaxy at a set of wavelengths from the UV to the sub-mm. We analyse
the results to determine the effect of dust on the observed radial and vertical
profiles of the stellar emission as well as on the attenuation and scattering
of light from the constituent stellar populations. We also quantify the
proportion of dust re-radiated stellar light powered by young and old stellar
populations, both bolometrically and as a function of infrared wavelength.
