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Galaxy and mass assembly (GAMA): The consistency of GAMA and WISE derived mass-to-light ratios

Research output: Contribution to journalArticle

Original languageEnglish
Article numberstx2379
Pages (from-to)776-783
Number of pages8
JournalMonthly Notices of the Royal Astronomical Society
Volume473
Issue number1
Early online date13 Sep 2017
DOIs
DateAccepted/In press - 11 Sep 2017
DateE-pub ahead of print - 13 Sep 2017
DatePublished (current) - Jan 2018

Abstract

Recent work has suggested that mid-IR wavelengths are optimal for estimating the mass-to-light ratios of stellar populations and hence the stellar masses of galaxies. We compare stellar masses deduced from spectral energy distribution (SED) models, fitted to multi-wavelength optical-NIR photometry, to luminosities derived from {\it WISE} photometry in the W1 and W2 bands at 3.6 and 4.5μm for non-star forming galaxies. The SED derived masses for a carefully selected sample of low redshift (z≤0.15) passive galaxies agree with the prediction from stellar population synthesis models that M∗/LW1≃0.6 for all such galaxies, independent of other stellar population parameters. The small scatter between masses predicted from the optical SED and from the {\it WISE} measurements implies that random errors (as opposed to systematic ones such as the use of different IMFs) are smaller than previous, deliberately conservative, estimates for the SED fits. This test is subtly different from simultaneously fitting at a wide range of optical and mid-IR wavelengths, which may just generate a compromise fit: we are directly checking that the best fit model to the optical data generates an SED whose M∗/LW1 is also consistent with separate mid-IR data. We confirm that for passive low redshift galaxies a fixed M∗/LW1=0.65 can generate masses at least as accurate as those obtained from more complex methods. Going beyond the mean value, in agreement with expectations from the models, we see a modest change in M∗/LW1 with SED fitted stellar population age but an insignificant one with metallicity.

    Research areas

  • galaxies: fundamental parameters, galaxies: photometry, galaxies: stellar content, galaxies: evolution, infrared: galaxies

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  • Full-text PDF (accepted author manuscript)

    Rights statement: This is the author accepted manuscript (AAM). The final published version (version of record) is available online via Oxford University Press at https://academic.oup.com/mnras/article/473/1/776/4157818 . Please refer to any applicable terms of use of the publisher.

    Accepted author manuscript, 296 KB, PDF-document

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