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Reconstructing the stellar mass distributions of galaxies using S⁴G IRAC 3.6 and 4.5 µm images, II : the conversion from light to mass

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Abstract
We present a new approach for estimating the 3.6 mu m stellar mass-to-light (M/L) ratio Rho 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.. 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.3.6, which varies intrinsically less than at optical wavelengths. The uncertainty on.3.6 of similar to 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.3.6 = 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 (similar to 0.1 dex) than alternatives. We expect our.3.6 to be optimal formapping the stellarmass distributions in S(4)G galaxies, for which we have developed an independent component analysis technique to first isolate the old stellar light at 3.6 mu m 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 mu m fluxes, e.g., in WISE imaging, and establishes a reliable basis for exploring variations in the stellar IMF.
Keywords
STAR-FORMATION HISTORY, COLOR GRADIENTS, SPIRAL GALAXIES, POPULATION, SYNTHESIS, MAGELLANIC-CLOUD, DUST EXTINCTION, SPACE-TELESCOPE, SPITZER, SURVEY, DISC GALAXIES, PHOTOMETRY, galaxies: stellar content, galaxies: structure, infrared: galaxies, supergiants

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Citation

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MLA
van der Wel, Sharon Meidt, 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.” ASTROPHYSICAL JOURNAL, vol. 788, no. 2, 2014.
APA
van der Wel, S. M., Schinnerer, E., van de Ven, G., Zaritsky, D., Peletier, R., Knapen, J. H., … Mizusawa, T. (2014). Reconstructing the stellar mass distributions of galaxies using S4G IRAC 3.6 and 4.5 µm images, II : the conversion from light to mass. ASTROPHYSICAL JOURNAL, 788(2).
Chicago author-date
Wel, Sharon Meidt van der, Eva Schinnerer, Glenn van de Ven, Dennis Zaritsky, Reynier Peletier, Johan H Knapen, Kartik Sheth, et al. 2014. “Reconstructing the Stellar Mass Distributions of Galaxies Using S4G IRAC 3.6 and 4.5 Μm Images, II : The Conversion from Light to Mass.” ASTROPHYSICAL JOURNAL 788 (2).
Chicago author-date (all authors)
van der Wel, Sharon Meidt, Eva Schinnerer, Glenn van de Ven, Dennis Zaritsky, Reynier Peletier, Johan H Knapen, Kartik Sheth, Michael Regan, Miguel Querejeta, Juan-Carlos Munoz-Mateos, Taehyun Kim, Joannah L Hinz, Armando Gil de Paz, E Athanassoula, Albert Bosma, Ronald J Buta, Mauricio Cisternas, Luis C Ho, Benne Holwerda, Ramin Skibba, E Laurikainen, H Salo, DA Gadotti, Jarkko Laine, S Erroz-Ferrer, Ebastien Comeron, K Menendez-Delmestre, M Seibert, and T Mizusawa. 2014. “Reconstructing the Stellar Mass Distributions of Galaxies Using S4G IRAC 3.6 and 4.5 Μm Images, II : The Conversion from Light to Mass.” ASTROPHYSICAL JOURNAL 788 (2).
Vancouver
1.
van der Wel SM, Schinnerer E, van de Ven G, Zaritsky D, Peletier R, Knapen JH, 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. ASTROPHYSICAL JOURNAL. 2014;788(2).
IEEE
[1]
S. M. van der Wel 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,” ASTROPHYSICAL JOURNAL, vol. 788, no. 2, 2014.
@article{8622306,
  abstract     = {We present a new approach for estimating the 3.6 mu m stellar mass-to-light (M/L) ratio Rho 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.. 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.3.6, which varies intrinsically less than at optical wavelengths. The uncertainty on.3.6 of similar to 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.3.6 = 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 (similar to 0.1 dex) than alternatives. We expect our.3.6 to be optimal formapping the stellarmass distributions in S(4)G galaxies, for which we have developed an independent component analysis technique to first isolate the old stellar light at 3.6 mu m 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 mu m fluxes, e.g., in WISE imaging, and establishes a reliable basis for exploring variations in the stellar IMF.},
  articleno    = {144},
  author       = {van der Wel, Sharon Meidt and Schinnerer, Eva and van de Ven, Glenn and Zaritsky, Dennis and Peletier, Reynier and Knapen, Johan H and Sheth, Kartik and Regan, Michael and Querejeta, Miguel and Munoz-Mateos, Juan-Carlos and Kim, Taehyun and Hinz, Joannah L and de Paz, Armando Gil and Athanassoula, E and Bosma, Albert and Buta, Ronald J and Cisternas, Mauricio and Ho, Luis C and Holwerda, Benne and Skibba, Ramin and Laurikainen, E and Salo, H and Gadotti, DA and Laine, Jarkko and Erroz-Ferrer, S and Comeron, Ebastien and Menendez-Delmestre, K and Seibert, M and Mizusawa, T},
  issn         = {0004-637X},
  journal      = {ASTROPHYSICAL JOURNAL},
  keywords     = {STAR-FORMATION HISTORY,COLOR GRADIENTS,SPIRAL GALAXIES,POPULATION,SYNTHESIS,MAGELLANIC-CLOUD,DUST EXTINCTION,SPACE-TELESCOPE,SPITZER,SURVEY,DISC GALAXIES,PHOTOMETRY,galaxies: stellar content,galaxies: structure,infrared: galaxies,supergiants},
  language     = {eng},
  number       = {2},
  pages        = {12},
  title        = {Reconstructing the stellar mass distributions of galaxies using S⁴G IRAC 3.6 and 4.5 µm images, II : the conversion from light to mass},
  url          = {http://dx.doi.org/10.1088/0004-637X/788/2/144},
  volume       = {788},
  year         = {2014},
}

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