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We present a self-consistent three-dimensional Monte-Carlo radiative transfermodel of the stellar and dust emission in the Milky-Way, and have computedsynthetic observations of the 3.6 to 100 microns emission in the Galacticmid-plane. In order to compare the model to observations, we use the GLIMPSE,MIPSGAL, and IRAS surveys to construct total emission spectra, as well aslongitude and latitude profiles for the emission. The distribution of stars anddust is taken from the SKY model, and the dust emissivities includes anapproximation of the emission from polycyclic aromatic hydrocarbons in additionto thermal emission. The model emission is in broad agreement with theobservations, but a few modifications are needed to obtain a good fit. Firstly,by adjusting the model to include two major and two minor spiral arms ratherthan four equal spiral arms, the fit to the longitude profiles for |l|>30degrees can be improved. Secondly, introducing a deficit in the dustdistribution in the inner Galaxy results in a better fit to the shape of theIRAS longitude profiles at 60 and 100 microns. With these modifications, themodel fits the observed profiles well, although it systematicallyunder-estimates the 5.8 and 8.0 microns fluxes. One way to resolve thisdiscrepancy is to increase the abundance of PAH molecules by 50% compared tothe original model, although we note that changes to the dust distribution orradiation field may provide alternative solutions. Finally, we use the model toquantify which stellar populations contribute the most to the heating ofdifferent dust types, and which stellar populations and dust types contributethe most to the emission at different wavelengths.

A self-consistent model of Galactic stellar and dust infrared emission and the abundance of polycyclic aromatic hydrocarbons