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We have fit the far-ultraviolet (FUV) to sub-millimeter (850 micron) spectralenergy distributions (SEDs) of the 61 galaxies from the "Key Insights on NearbyGalaxies: A Far-Infrared Survey with Herschel" (KINGFISH). The fitting has beenperformed using three models: the Code for Investigating GALaxy Evolution(CIGALE), the GRAphite-SILicate approach (GRASIL), and the Multi-wavelengthAnalysis of Galaxy PHYSical properties (MAGPHYS). We have analyzed the resultsof the three codes in terms of the SED shapes, and by comparing the derivedquantities with simple "recipes" for stellar mass (Mstar), star-formation rate(SFR), dust mass (Mdust), and monochromatic luminosities. Although thealgorithms rely on different assumptions for star-formation history, dustattenuation and dust reprocessing, they all well approximate the observed SEDsand are in generally good agreement for the associated quantities. However, thethree codes show very different behavior in the mid-infrared regime, inparticular between 25 and 70 micron where there are no observationalconstraints for the KINGFISH sample. We find that different algorithms givediscordant SFR estimates for galaxies with low specific SFR, and that thestandard "recipes" for calculating FUV absorption overestimate the extinctioncompared to the SED-fitting results. Results also suggest that assuming a"standard" constant stellar mass-to-light ratio overestimates Mstar relative tothe SED fitting, and we provide new SED-based formulations for estimating Mstarfrom WISE W1 (3.4 micron) luminosities and colors. From a Principal ComponentAnalysis of Mstar, SFR, Mdust, and O/H, we reproduce previous scaling relationsamong Mstar, SFR, and O/H, and find that Mdust can be predicted to withinroughly 0.3 dex using only Mstar and SFR.

Comprehensive comparison of models for spectral energy distributions from 0.1 micron to 1 mm of nearby star-forming galaxies