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Date and Time of the Query: 2019-06-17 T10:14:15 PDT
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For refcode 2017ApJS..233...13Z:
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Copyright by American Astronomical Society. Reproduced by permission
2017ApJS..233...13Z The Impact of Star Formation Histories on Stellar Mass Estimation: Implications from the Local Group Dwarf Galaxies Zhang, Hong-Xin; Puzia, Thomas H.; Weisz, Daniel R. Abstract. Building on the relatively accurate star formation histories (SFHs) and metallicity evolution of 40 Local Group (LG) dwarf galaxies derived from resolved color-magnitude diagram modeling, we carried out a comprehensive study of the influence of SFHs, metallicity evolution, and dust extinction on the UV-to-near-IR color-mass-to-light ratio (color-{log}{{{{UPSILON}}}}_\star_(lambda)) distributions and M_*_ estimation of local universe galaxies. We find that (1) the LG galaxies follow color-{log}{{{{UPSILON}}}}_\star_(lambda) relations that fall in between the ones calibrated by previous studies; (2) optical color-{log}{{{{UPSILON}}}}_\star_(lambda) relations at higher [M/H] are generally broader and steeper; (3) the SFH "concentration" does not significantly affect the color-{log}{{{{UPSILON}}}}_\star_(lambda) relations; (4) light-weighted ages < {age}{>}_lambda_ and metallicities < [{{M}}/{{H}}]{>}_lambda_ together constrain {log}{{{{UPSILON}}}}_\star_(lambda) with uncertainties ranging from <~0.1 dex for the near-IR up to 0.2 dex for the optical passbands; (5) metallicity evolution induces significant uncertainties to the optical but not near-IR {{{{UPSILON}}}}_\star_(lambda) at a given < {age}{>}_lambda_ and < [{{M}}/{{H}}]{>}_lambda_; (6) the V band is the ideal luminance passband for estimating {{{{UPSILON}}}}_\star_(lambda) from single colors, because the combinations of {{{{UPSILON}}}}_\star_(V) and optical colors such as B - V and g - r exhibit the weakest systematic dependences on SFHs, metallicities, and dust extinction; and (7) without any prior assumption on SFHs, M_*_ is constrained with biases <~0.3 dex by the optical-to-near-IR SED fitting. Optical passbands alone constrain M_*_ with biases <~0.4 dex (or <~0.6 dex) when dust extinction is fixed (or variable) in SED fitting. SED fitting with monometallic SFH models tends to underestimate M_*_ of real galaxies. M_*_ tends to be overestimated (or underestimated) at the youngest (or oldest) < {age}{>}_{mass_}. Key words: galaxies: fundamental parameters, galaxies: general, galaxies: photometry, galaxies: stellar content, Local Group
Retrieve 40 NED objects in this reference.
Please click here for ADS abstract

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