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Local Group (LG) galaxies have relatively accurate SFHs and metallicityevolution derived from resolved CMD modeling, and thus offer a uniqueopportunity to explore the efficacy of estimating stellar mass M$_{\star}$ ofreal galaxies based on integrated stellar luminosities. Building on the SFHsand metallicity evolution of 40 LG dwarf galaxies, we carried out acomprehensive study of the influence of SFHs, metallicity evolution, and dustextinction on the UV-to-NIR color-$M/L$(color-log$\Upsilon_{\star}$($\lambda$)) relations and M$_{\star}$ estimationof local universe galaxies. We find that: The LG galaxies followcolor-log$\Upsilon_{\star}$($\lambda$) relations that fall in between the onescalibrated by previous studies; Optical color-log$\Upsilon_{\star}$($\lambda$)relations at higher metallicities ([M/H]) are generally broader and steeper;The SFH "concentration" does not significantly affect thecolor-log$\Upsilon_{\star}$($\lambda$) relations; Light-weighted ages and [M/H]together constrain log$\Upsilon_{\star}$($\lambda$) with uncertainties rangingfrom $\lesssim$ 0.1 dex for the NIR up to 0.2 dex for the optical passbands;Metallicity evolution induces significant uncertainties to the optical but notNIR $\Upsilon_{\star}$($\lambda$) at given light-weighted ages and [M/H]; 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 theweakest systematic dependence on SFHs, [M/H] and dust extinction; Without anyprior assumption on SFHs, M$_{\star}$ is constrained with biases $\lesssim$ 0.3dex by the optical-to-NIR SED fitting. Optical passbands alone constrainM$_{\star}$ with biases $\lesssim$ 0.4 dex (or $\lesssim$ 0.6 dex) when dustextinction is fixed (or variable) in SED fitting. [abridged]

The Impact of Star Formation Histories on Stellar Mass Estimation: Implications from the Local Group Dwarf Galaxies