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(abridged) The majority of star-forming galaxies follow a simple empiricalcorrelation in the star formation rate (SFR) versus stellar mass ($M_*$) plane,usually referred to as the star formation Main Sequence (MS). Here we combine aset of hydro-dynamical simulations of interacting galactic disks withstate-of-the-art radiative transfer codes to analyze how the evolution ofmergers is reflected upon the properties of the MS. We present\textsc{Chiburst}, a Markov Chain Monte Carlo (MCMC) Spectral EnergyDistribution (SED) code that fits the multi-wavelength, broad-band photometryof galaxies and derives stellar masses, star formation rates, and geometricalproperties of the dust distribution. We apply this tool to the SEDs ofsimulated mergers and compare the derived results with the reference outputfrom the simulations. Our results indicate that changes in the SEDs of mergersas they approach coalescence and depart from the MS are related to an evolutionof dust geometry in scales larger than a few hundred parsecs. This is reflectedin a correlation between the specific star formation rate (sSFR), and thecompactness parameter $\mathcal{C}$, that parametrizes this geometry and hencethe evolution of dust temperature ($T_{\rm{dust}}$) with time. As mergersapproach coalescence, they depart from the MS and increase their compactness,which implies that moderate outliers of the MS are consistent with late-typemergers. By further applying our method to real observations of LuminousInfrared Galaxies (LIRGs), we show that the merger scenario is unable toexplain these extreme outliers of the MS. Only by significantly increasing thegas fraction in the simulations are we able to reproduce the SEDs of LIRGs.

Variations of the ISM Compactness Across the Main Sequence of Star-Forming Galaxies: Observations and Simulations