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We present the first systematic comparison of ultraviolet-millimeter spectralenergy distributions (SEDs) of observed and simulated interacting galaxies. Oursample is drawn from the Spitzer Interacting Galaxy Survey, and probes a rangeof galaxy interaction parameters. We use 31 galaxies in 14 systems which havebeen observed with Herschel, Spitzer, GALEX, and 2MASS. We create a suite ofGADGET-3 hydrodynamic simulations of isolated and interacting galaxies withstellar masses comparable to those in our sample of interacting galaxies.Photometry for the simulated systems is then calculated with the SUNRISEradiative transfer code for comparison with the observed systems. For most ofthe observed systems, one or more of the simulated SEDs match reasonably well.The best matches recover the infrared luminosity and the star formation rate ofthe observed systems, and the more massive systems preferentially match SEDsfrom simulations of more massive galaxies. The most morphologically distortedsystems in our sample are best matched to simulated SEDs close to coalescence,while less evolved systems match well with SEDs over a wide range ofinteraction stages, suggesting that an SED alone is insufficient to identifyinteraction stage except during the most active phases in strongly interactingsystems. This result is supported by our finding that the SEDs calculated forsimulated systems vary little over the interaction sequence.

Simulated Galaxy Interactions as Probes of Merger Spectral Energy Distributions