Reconstructing the stellar mass distributions of galaxies using S4G IRAC 3.6 and 4.5 μm images. II. The conversion from light to mass.
Physics and Astronomy
We present a new approach for estimating the 3.6μm stellar mass-to-light (M/L) ratio ϒ3.6 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 ϒ. 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 ϒ3.6, 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 3.6μm 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) 3.6μm fluxes, e.g., in WISE imaging, and establishes a reliable basis for exploring variations in the stellar IMF.
Original Publication Information
Meidt, Sharon E., et al. "Reconstructing the Stellar Mass Distributions of Galaxies Using S4G IRAC 3.6 and 4.5 μm Images. II. The Conversion from Light to Mass." 2014. The Astrophysical Journal 788(2): 12 pp.
Meidt, Sharon; Schinnerer, Eva; van de Ven, Glenn; Zaritsky, Dennis; Peletier, Reynier; Knapen, Johan H.; Sheth, Kartik; Regan, Michael; Querejeta, Miguel; Munoz-Mateos, Juan Carlos; Kim, Taehyun; Hinz, Joannah; Gil de Paz, Armando; Athanassoula, E.; Bosma, Albert; Buta, Ronald J.; Cisternas, Mauricio; Ho, Luis C.; Holwerda, Benne W.; Skibba, Ramin; Laurikainen, E.; Salo, H.; Gadotti, D. A.; Laine, Jarkko; Erroz-Ferrer, Santiago; Comeron, Sebastien; Menendez-Delmestre, K.; Seibert, M.; and Mizusawa, T., "Reconstructing the stellar mass distributions of galaxies using S4G IRAC 3.6 and 4.5 μm images. II. The conversion from light to mass." (2014). Faculty Scholarship. 201.
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