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We present predictions of Spectral Energy Distributions (SEDs), from the UVto the FIR, of simulated galaxies at $z=0$. These were obtained bypost-processing the results of an N-body+hydro simulation of a smallcosmological volume, that uses the Multi-Phase Particle Integrator (MUPPI) forstar formation and stellar feedback, with the GRASIL-3D radiative transfercode, that includes reprocessing of UV light by dust. Physical properties ofgalaxies resemble observed ones, though with some tension at small and largestellar masses. Comparing predicted SEDs of simulated galaxies with differentsamples of local galaxies, we find that these resemble observed ones, whennormalised at 3.6 $\mu$m. A comparison with the Herschel Reference Survey showsthat, when binning galaxies in Star Formation Rate (SFR), average SEDs arereproduced to within a factor of $\sim2$ even in normalization, while binningin stellar mass highlights the same tension that is present in the stellar mass-- SFR plane. We use our sample to investigate the correlation of IR luminosityin Spitzer and Herschel bands with several galaxy properties. SFR is thequantity that best correlates with IR light up to $160\ \mu$m, while at longerwavelengths better correlations are found with molecular mass and, at $500\\mu$m, with dust mass. However, using the position of the FIR peak as a proxyfor cold dust temperature, we assess that heating of cold dust is mostlydetermined by SFR, with stellar mass giving only a minor contribution. Wefinally show how our sample of simulated galaxies can be used as a guide tounderstand the physical properties and selection biases of observed samples.

Panchromatic Spectral Energy Distributions of simulated galaxies: results at redshift $z=0$