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We compare observed far infra-red/sub-millimetre (FIR/sub-mm) galaxy spectralenergy distributions (SEDs) of massive galaxies ($M_{\star}\gtrsim10^{10}$$h^{-1}$M$_{\odot}$) derived through a stacking analysis with predictions froma new model of galaxy formation. The FIR SEDs of the model galaxies arecalculated using a self-consistent model for the absorption and re-emission ofradiation by interstellar dust based on radiative transfer calculations andglobal energy balance arguments. Galaxies are selected based on their positionon the specific star formation rate (sSFR) - stellar mass ($M_{\star}$) plane.We identify a main sequence of star-forming galaxies in the model, i.e. a welldefined relationship between sSFR and $M_\star$, up to redshift $z\sim6$. Thescatter of this relationship evolves such that it is generally larger at higherstellar masses and higher redshifts. There is remarkable agreement between thepredicted and observed average SEDs across a broad range of redshifts($0.5\lesssim z\lesssim4$) for galaxies on the main sequence. However, theagreement is less good for starburst galaxies at $z\gtrsim2$, selected here tohave elevated sSFRs$>10\times$ the main sequence value. We find that thepredicted average SEDs are robust to changing the parameters of our dust modelwithin physically plausible values. We also show that the dust temperatureevolution of main sequence galaxies in the model is driven by star formation onthe main sequence being more burst-dominated at higher redshifts.

The far infra-red SEDs of main sequence and starburst galaxies