Contribution the scattered dust emission at λ = 35.11 μm makes to the Y slice for τ_z(1 μm) = 10, θ = 90° is shown. The comparison between all the code results is shown on the left, where the DART-ray and TRADING results are significantly below the results from the other five codes. On the right, the results from DIRTY are shown decomposed into the three contributing components. For the back three quarters of the slab, the scattered dust emission dominates over the direct dust emission and scattered stellar emission. The differences between DART-ray and TRADING and the rest of the codes is due to not calculating the scattered dust emisison component.