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We present the first detailed study of the spatially-resolved dust continuumemission of simulated galaxies at 1<z<5. We run the radiative transfer codeSKIRT on a sample of submillimeter-bright galaxies drawn from the Feedback inRealistic Environments (FIRE) project. These simulated galaxies reach Milky Waymasses by z=2. Our modelling provides predictions for the full rest-framefar-ultraviolet-to-far-infrared spectral energy distributions of thesesimulated galaxies, as well as 25-pc-resolution maps of their emission acrossthe wavelength spectrum. The derived morphologies are notably different indifferent wavebands, with the same galaxy often appearing clumpy and extendedin the far-ultraviolet yet an ordered spiral at far-infrared wavelengths. Theobserved-frame 870-$\mu$m half-light radii of our FIRE-2 galaxies are~0.5-4kpc, consistent with existing ALMA observations of galaxies withsimilarly high redshifts and stellar masses. In both simulated and observedgalaxies, the dust continuum emission is generally more compact than the coldgas and the dust mass, but more extended than the stellar component. The mostextreme cases of compact dust emission seem to be driven by particularlycompact recent star-formation, which generates steep dust temperaturegradients. Our results confirm that the spatial extent of the dust continuumemission is sensitive to both the dust mass and SFR distributions.

Predictions for the spatial distribution of the dust continuum emission in 1