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

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dc.contributor.authorHunt, L. K.
dc.contributor.authorDe Looze, I
dc.contributor.authorBoquien, M.
dc.contributor.authorNikutta, R.
dc.contributor.authorRossi, A.
dc.contributor.authorBianchil, S.
dc.contributor.authorDale, D. A.
dc.contributor.authorGranato, G. L.
dc.contributor.authorKennicutt, R. C.
dc.contributor.authorSilva, L.
dc.contributor.authorCiesla, L.
dc.contributor.authorRelano, M.
dc.contributor.authorViaene, S.
dc.contributor.authorBrandl, B.
dc.contributor.authorCalzetti, D.
dc.contributor.authorCroxall, K., V
dc.contributor.authorDraine, B. T.
dc.contributor.authorGalametz, M.
dc.contributor.authorGordon, K. D.
dc.contributor.authorGroves, B. A.
dc.contributor.authorHelou, G.
dc.contributor.authorHerrera-Camus, R.
dc.contributor.authorHinz, J. L.
dc.contributor.authorKoda, J.
dc.contributor.authorSalim, S.
dc.contributor.authorSandstrom, K. M.
dc.contributor.authorSmith, J. D.
dc.contributor.authorWilson, C. D.
dc.contributor.authorZibetti, S.
dc.date.accessioned2025-01-23T21:19:36Z
dc.date.available2025-01-23T21:19:36Z
dc.date.issued2019
dc.description.abstractWe have fit the far-ultraviolet (FUV) to sub-millimeter (850 mu m) spectral energy distributions (SEDs) of the 61 galaxies from the Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel (KINGFISH). The fitting has been performed using three models: the Code for Investigating GALaxy Evolution (CIGALE), the GRAphite-SILicate approach (GRASIL), and the Multiwavelength Analysis of Galaxy PHYSical properties (MAGPHYS). We have analyzed the results of the three codes in terms of the SED shapes, and by comparing the derived quantities with simple "recipes" for stellar mass (M-star), star-formation rate (SFR), dust mass (M-dust), and monochromatic luminosities. Although the algorithms rely on different assumptions for star-formation history, dust attenuation and dust reprocessing, they all well approximate the observed SEDs and are in generally good agreement for the associated quantities. However, the three codes show very different behavior in the mid-infrared regime: in the 5-10 mu m region dominated by PAH emission, and also between 25 and 70 mu m where there are no observational constraints for the KINGFISH sample. We find that different algorithms give discordant SFR estimates for galaxies with low specific SFR, and that the standard recipes for calculating FUV absorption overestimate the extinction compared to the SED-fitting results. Results also suggest that assuming a "standard" constant stellar mass-to-light ratio overestimates Mstar relative to the SED fitting, and we provide new SED-based formulations for estimating Mstar from WISE W1 (3.4 mu m) luminosities and colors. From a principal component analysis of M-star, SFR, M-dust, and O/H, we reproduce previous scaling relations among Mstar, SFR, and O/H, and find that Mdust can be predicted to within similar to 0.3 dex using only M-star and SFR.
dc.fuente.origenWOS
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/101186
dc.identifier.wosidWOS:000454936300004
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectgalaxies: fundamental parameters
dc.subjectgalaxies: star formation
dc.subjectgalaxies: ISM
dc.subjectgalaxies: spiral
dc.subjectinfrared: galaxies
dc.subjectultraviolet: galaxies
dc.titleComprehensive comparison of models for spectral energy distributions from 0.1 μm to 1mm of nearby star-forming galaxies
dc.typeartículo
dc.volumen621
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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