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We present a Monte Carlo (MC) radiative transfer code for complex threedimensional dust distributions and include transiently heated PAH. Thecorrectness of the code is confirmed by comparison with benchmark results. Themethod makes use of the parallelization capabilities of modern vectorizedcomputing units like graphic cards. The computational speed grows linearly withthe number of graphical processing units (GPU). On a conventional desktop PC,our code is up to a factor 100 faster when compared to other MC algorithms. Asan example, we compute the dust emission of proto-planetary disks. We simulatehow a mid-IR instrument mounted at a future 42m ELT will detect such disks. Twocases are distinguished: a homogeneous disk and a disk with an outwardmigrating planet, producing a gap and a spiral density wave. We find that theresulting mid-IR spectra of both disks are almost identical. However, they canbe distinguished at those wavelengths by coronographic, dual-band imaging.Finally, the emission of PAHs exposed to different radiation fields iscomputed. We demonstrate that PAH emission depends not only on the strength butalso strongly on the hardness of the radiation, a fact which has often beenneglected in previous models. We find that hard photons (>20eV) easilydissociate all PAHs in the disks of T Tauri stars. To explain the low, but notnegligible detection rate (<10%) of PAHs in T Tau disks, we suggest thatturbulent motions act as a possible path for PAH survival.

PAH in three dimensional Monte Carlo radiativtive transfer