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Being WISE, I : validating stellar population models and M*/L ratios at 3.4 and 4.6 µm

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Abstract
Using data from the Wide-field Infrared Survey Explorer mission, we have measured near infra-red (NIR) photometry of a diverse sample of dust-free stellar systems (globular clusters, dwarf and giant early-type galaxies) which have metallicities that span the range -2.2 < [Fe/H] (dex) < 0.3. This dramatically increases the sample size and broadens the metallicity regime over which the 3.4 (W1) and 4.6 mu m (W2) photometry of stellar populations have been examined. We find that the W1-W2 colors of intermediate and old (>2Gyr) stellar populations are insensitive to the age of the stellar population, but that the W1 - W2 colors become bluer with increasing metallicity, a trend not well reproduced by most stellar population synthesis (SPS) models. In common with previous studies, we attribute this behavior to the increasing strength of the CO absorption feature located in the 4.6 mu m bandpass with metallicity. Having used our sample to validate the efficacy of some of the SPS models, we use these models to derive stellar mass-to-light ratios in the W1 and W2 bands. Utilizing observational data from the SAURON and ATLAS3D surveys, we demonstrate that these bands provide extremely simple, yet robust stellar mass tracers for dust free older stellar populations that are freed from many of the uncertainties common among optical estimators.
Keywords
EARLY-TYPE GALAXIES, SPECTRAL ENERGY-DISTRIBUTIONS, INFRARED-SURVEY-EXPLORER, FIELD DWARF ELLIPTICALS, M31, GLOBULAR-CLUSTERS, INITIAL MASS FUNCTION, S(4)G IRAC 3.6, SAURON, PROJECT, VIRGO CLUSTER, STAR-CLUSTERS, galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies:, fundamental parameters, globula clusters: general, infrared: galaxies

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Citation

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MLA
Norris, Mark A., et al. “Being WISE, I : Validating Stellar Population Models and M*/L Ratios at 3.4 and 4.6 Μm.” ASTROPHYSICAL JOURNAL, vol. 797, no. 1, 2014.
APA
Norris, M. A., van der Wel, S. M., Van de Ven, G., Schinnerer, E., Groves, B., & Querejeta, M. (2014). Being WISE, I : validating stellar population models and M*/L ratios at 3.4 and 4.6 µm. ASTROPHYSICAL JOURNAL, 797(1).
Chicago author-date
Norris, Mark A, Sharon Meidt van der Wel, Glenn Van de Ven, Eva Schinnerer, Brent Groves, and Miguel Querejeta. 2014. “Being WISE, I : Validating Stellar Population Models and M*/L Ratios at 3.4 and 4.6 Μm.” ASTROPHYSICAL JOURNAL 797 (1).
Chicago author-date (all authors)
Norris, Mark A, Sharon Meidt van der Wel, Glenn Van de Ven, Eva Schinnerer, Brent Groves, and Miguel Querejeta. 2014. “Being WISE, I : Validating Stellar Population Models and M*/L Ratios at 3.4 and 4.6 Μm.” ASTROPHYSICAL JOURNAL 797 (1).
Vancouver
1.
Norris MA, van der Wel SM, Van de Ven G, Schinnerer E, Groves B, Querejeta M. Being WISE, I : validating stellar population models and M*/L ratios at 3.4 and 4.6 µm. ASTROPHYSICAL JOURNAL. 2014;797(1).
IEEE
[1]
M. A. Norris, S. M. van der Wel, G. Van de Ven, E. Schinnerer, B. Groves, and M. Querejeta, “Being WISE, I : validating stellar population models and M*/L ratios at 3.4 and 4.6 µm,” ASTROPHYSICAL JOURNAL, vol. 797, no. 1, 2014.
@article{8622294,
  abstract     = {Using data from the Wide-field Infrared Survey Explorer mission, we have measured near infra-red (NIR) photometry of a diverse sample of dust-free stellar systems (globular clusters, dwarf and giant early-type galaxies) which have metallicities that span the range -2.2 < [Fe/H] (dex) < 0.3. This dramatically increases the sample size and broadens the metallicity regime over which the 3.4 (W1) and 4.6 mu m (W2) photometry of stellar populations have been examined. We find that the W1-W2 colors of intermediate and old (>2Gyr) stellar populations are insensitive to the age of the stellar population, but that the W1 - W2 colors become bluer with increasing metallicity, a trend not well reproduced by most stellar population synthesis (SPS) models. In common with previous studies, we attribute this behavior to the increasing strength of the CO absorption feature located in the 4.6 mu m bandpass with metallicity. Having used our sample to validate the efficacy of some of the SPS models, we use these models to derive stellar mass-to-light ratios in the W1 and W2 bands. Utilizing observational data from the SAURON and ATLAS3D surveys, we demonstrate that these bands provide extremely simple, yet robust stellar mass tracers for dust free older stellar populations that are freed from many of the uncertainties common among optical estimators.},
  articleno    = {55},
  author       = {Norris, Mark A and van der Wel, Sharon Meidt and Van de Ven, Glenn and Schinnerer, Eva and Groves, Brent and Querejeta, Miguel},
  issn         = {0004-637X},
  journal      = {ASTROPHYSICAL JOURNAL},
  keywords     = {EARLY-TYPE GALAXIES,SPECTRAL ENERGY-DISTRIBUTIONS,INFRARED-SURVEY-EXPLORER,FIELD DWARF ELLIPTICALS,M31,GLOBULAR-CLUSTERS,INITIAL MASS FUNCTION,S(4)G IRAC 3.6,SAURON,PROJECT,VIRGO CLUSTER,STAR-CLUSTERS,galaxies: elliptical and lenticular,cD,galaxies: evolution,galaxies:,fundamental parameters,globula clusters: general,infrared: galaxies},
  language     = {eng},
  number       = {1},
  pages        = {9},
  title        = {Being WISE, I : validating stellar population models and M*/L ratios at 3.4 and 4.6 µm},
  url          = {http://dx.doi.org/10.1088/0004-637X/797/1/55},
  volume       = {797},
  year         = {2014},
}

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