Reconstructing the stellar mass distributions of galaxies using S^4G irac 3.6 and 4.5 μm images. II. The conversion from light to mass

dc.contributor.authorGil de Paz, Armando, otros
dc.description© 2014. The American Astronomical Society. All rights reserved. Artículo firmado por 29 autores. Thanks to Mariya Lyubenova for fruitful discussion and the entire S4G team. E.A., A.B., J.K., G.vdV., M.Q., S.M., and E.S. acknowledge financial support of the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/ under REA grant agreement number PITN-GA-2011-289313. K.S., J.-C.M.-M., and T.K. acknowledge support from the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.
dc.description.abstractWe present a new approach for estimating the 3.6 μm stellar mass-to-light (M/L) ratio Υ_3.6 in terms of the [3.6]-[4.5] colors of old stellar populations. Our approach avoids several of the largest sources of uncertainty in existing techniques using population synthesis models. By focusing on mid-IR wavelengths, we gain a virtually dust extinction-free tracer of the old stars, avoiding the need to adopt a dust model to correctly interpret optical or optical/near-IR colors normally leveraged to assign the mass-to-light ratio Upsilon. By calibrating a new relation between near-IR and mid-IR colors of giant stars observed in GLIMPSE we also avoid the discrepancies in model predictions for the [3.6]-[4.5] colors of old stellar populations due to uncertainties in the molecular line opacities assumed in template spectra. We find that the [3.6]-[4.5] color, which is driven primarily by metallicity, provides a tight constraint on Upsilon3.6, which varies intrinsically less than at optical wavelengths. The uncertainty on Υ3.6 of ~0.07 dex due to unconstrained age variations marks a significant improvement on existing techniques for estimating the stellar M/L with shorter wavelength data. A single Υ3.6 = 0.6 (assuming a Chabrier initial mass function (IMF)), independent of [3.6]-[4.5] color, is also feasible because it can be applied simultaneously to old, metal-rich and young, metal-poor populations, and still with comparable (or better) accuracy (~0.1 dex) than alternatives. We expect our Υ3.6 to be optimal for mapping the stellar mass distributions in S4G galaxies, for which we have developed an independent component analysis technique to first isolate the old stellar light at 3.6 μm from nonstellar emission (e.g., hot dust and the 3.3 polycyclic aromatic hydrocarbon feature). Our estimate can also be used to determine the fractional contribution of nonstellar emission to global (rest-frame) 3.6 μm fluxes, e.g., in WISE imaging, and establishes a reliable basis for exploring variations in the stellar IMF.
dc.description.departmentDepto. de Física de la Tierra y Astrofísica
dc.description.facultyFac. de Ciencias Físicas
dc.description.sponsorshipDAGAL network of the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme
dc.description.sponsorshipNational Radio Astronomy Observatory (NRAO)
dc.description.sponsorshipUnión Europea (UE)
dc.description.sponsorship7th Framework Programme 7FP (UE)
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dc.journal.titleAstrophysical journal
dc.publisherAmerican Astronomical Society
dc.rights.accessRightsopen access
dc.subject.keywordStar-formation history
dc.subject.keywordColor gradients
dc.subject.keywordSpiral galaxies
dc.subject.keywordPopulation synthesis
dc.subject.keywordDust extinction
dc.subject.keywordSpitzer survey
dc.subject.keywordDisc galaxies
dc.subject.ucmAstronomía (Física)
dc.titleReconstructing the stellar mass distributions of galaxies using S^4G irac 3.6 and 4.5 μm images. II. The conversion from light to mass
dc.typejournal article
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