COLOR–MASS-TO-LIGHT-RATIO RELATIONS FOR DISK GALAXIES
By S. McGaugh, J. Schombert. 2014
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We combine Spitzer 3.6 μm observations of a sample of disk galaxies spanning over 10 mag in luminosity with optical luminosities and colors to test population synthesis prescriptions for computing stellar mass. Many commonly employed models fail to provide self-consistent results: the stellar mass estimated from the luminosity in one band can differ grossly from that of another band for the same galaxy. Independent models agree closely in the optical (V band), but diverge at longer wavelengths. This effect is particularly pronounced in recent models with substantial contributions from TP-AGB stars. We provide revised color–mass-to-light ratio relations that yield self-consistent stellar masses when applied to real galaxies. The B − V color is a good indicator of the mass-to-light ratio. Some additional information is provided by V − I, but neither it nor J − Ks are particularly useful for constraining the mass-to-light ratio on their own. In the near-infrared, the mass-to-light ratio depends weakly on color, with typical values of 0.6 M☉/L☉ in the Ks band and 0.47 M☉/L☉ at 3.6 μm.
Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics
View Paper: https://www.semanticscholar.org/paper/a27e22511d20768a27509c9bc31fc867c8e7c342
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Citations in the corpus
- Masses and scaling relations for nuclear star clusters, and their co-existence with central black holes (2016, unknown): “…one colour is available, we calculate the error weighted mean of the different M/L-values to obtainMNSC, which helps to minimize systematic uncer- 3 Full version of the table is available in the electronic version of the journal c© 2014 RAS, MNRAS 000, 1–22 tainties (cf McGaugh & Schombert 2014).”
- Fitting the radial acceleration relation to individual SPARC galaxies (2018, background): “ESO Fellow Assuming that the stellar mass-to-light ratio Υ? does not vary strongly at [3.6] (McGaugh & Schombert 2014, 2015; Meidt et al. 2014; Schombert & McGaugh 2014), it is found that the RAR has an observed rms scatter of only 0.13 dex (McGaugh et al. 2016; Lelli et al. 2017a).”
- SPARC: MASS MODELS FOR 175 DISK GALAXIES WITH SPITZER PHOTOMETRY AND ACCURATE ROTATION CURVES (2016, methodology): “If we adopt the customary 12 definition of maximum disk as Vbar/Vobs = 0.85 (Sackett 1997), then the mean maximum-disk value of Υ? is ∼0.5 M /L , which is similar to the predictions of SPS models with standard IMFs (e.g., McGaugh & Schombert 2014; Meidt et al. 2014; Schombert & McGaugh 2014a).”
- THE SMALL SCATTER OF THE BARYONIC TULLY–FISHER RELATION (2015, methodology): “We assume δΥ∗ = 0.11 dex, as suggested by stellar population models (Meidt et al. 2014; McGaugh & Schombert 2014).”
- A z = 0 Multiwavelength Galaxy Synthesis. I. A WISE and GALEX Atlas of Local Galaxies (2019, background): “Schombert & McGaugh (2014) and McGaugh & Schombert (2014) argue for Υ3.”
- GALEX–SDSS–WISE LEGACY CATALOG (GSWLC): STAR FORMATION RATES, STELLAR MASSES, AND DUST ATTENUATIONS OF 700,000 LOW-REDSHIFT GALAXIES (2016, background): “While these arguments are correct, they do not take into account large modeling discrepancies in the near-IR mass-tolight ratios (McGaugh & Schombert 2014), arising due to the uncertainties in our understanding of the post-main sequence phases of stellar evolution, the phases which dominate the…”
- One Law to Rule Them All: The Radial Acceleration Relation of Galaxies (2016, background): “These values are in good agreement with different SPS models (McGaugh & Schombert 2014; Meidt et al. 2014; Norris et al. 2016).”