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To explore the connection between the global physical properties of galaxiesand their far-infrared (FIR) spectral energy distributions (SEDs), we study thevariation in the FIR SEDs of a set of hydrodynamically simulated galaxies thatare generated by performing dust radiative transfer in post-processing. Oursample includes both isolated and merging systems at various stages of themerging process and covers infrared (IR) luminosities and dust masses that arerepresentative of both low- and high-redshift galaxies. We study the FIR SEDsusing principle component analysis (PCA) and find that 97\% of the variance inthe sample can be explained by two principle components (PCs). The first PCcharacterizes the wavelength of the peak of the FIR SED, and the second encodesthe breadth of the SED. We find that the coefficients of both PCs can bepredicted well using a double power law in terms of the IR luminosity and dustmass, which suggests that these two physical properties are the primarydeterminants of galaxies' FIR SED shapes. Incorporating galaxy sizes does notsignificantly improve our ability to predict the FIR SEDs. Our results suggestthat the observed redshift evolution in the effective dust temperature at fixedIR luminosity is not driven by geometry: the SEDs of $z \sim 2-3$ ultraluminousIR galaxies (ULIRGs) are cooler than those of local ULIRGs not because thehigh-redshift galaxies are more extended but rather because they have higherdust masses at fixed IR luminosity. Finally, based on our simulations, weintroduce a two-parameter set of SED templates that depend on both IRluminosity and dust mass.

What shapes the far-infrared spectral energy distributions of galaxies?