Abstract
Local Group (LG) galaxies have relatively accurate SFHs and metallicity
evolution derived from resolved CMD modeling, and thus offer a unique
opportunity to explore the efficacy of estimating stellar mass M$_\star$ of
real galaxies based on integrated stellar luminosities. Building on the SFHs
and metallicity evolution of 40 LG dwarf galaxies, we carried out a
comprehensive study of the influence of SFHs, metallicity evolution and dust
extinction on the UV-to-NIR color-$M/L$
(color-log$\Upsilon_\star$($łambda$)) relations and M$_\star$ estimation
of local universe galaxies. We find that: The LG galaxies follow
color-log$\Upsilon_\star$($łambda$) relations that fall in between the ones
calibrated by previous studies; Optical color-log$\Upsilon_\star$($łambda$)
relations at higher metallicities (M/H) are generally broader and steeper;
The SFH "concentration" does not significantly affect the
color-log$\Upsilon_\star$($łambda$) relations; Light-weighted ages and M/H
together constrain log$\Upsilon_\star$($łambda$) with uncertainties ranging
from $łesssim$ 0.1 dex for the NIR up to 0.2 dex for the optical passbands;
Metallicity evolution induces significant uncertainties to the optical but not
NIR $\Upsilon_\star$($łambda$) at given light-weighted ages and M/H; The
$V$ band is the ideal luminance passband for estimating
$\Upsilon_\star$($łambda$) from single colors, because the combinations of
$\Upsilon_\star$($V$) and optical colors such as $B-V$ and $g-r$ exhibit the
weakest systematic dependence on SFHs, M/H and dust extinction; Without any
prior assumption on SFHs, M$_\star$ is constrained with biases $łesssim$ 0.3
dex by the optical-to-NIR SED fitting. Optical passbands alone constrain
M$_\star$ with biases $łesssim$ 0.4 dex (or $łesssim$ 0.6 dex) when dust
extinction is fixed (or variable) in SED fitting. abridged
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