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Stellar population synthesis models can now reproduce the photometry of oldstellar systems (age $>$ 2 Gyr) in the near-infrared (NIR) bands at 3.4 and4.6$\mu$m (WISE W1 $\&$ W2 or IRAC 1 $\&$ 2). In this paper we derive stellarmass-to-light ratios for these and optical bands, and confirm that the NIR M/Lshows dramatically reduced sensitivity to both age and metallicity compared tooptical bands, and further, that this behavior leads to significantly morerobust stellar masses for quiescent galaxies with [Fe/H] > -0.5 regardless ofstar formation history (SFH). We then use realistic early-type galaxy SFHs andmetallicity distributions from the EAGLE simulations of galaxy formation toinvestigate two methods to determine the appropriate M/L for a galaxy: 1) Weshow that the uncertainties introduced by an unknown SFH can be largely removedusing a spectroscopically inferred luminosity-weighted age and metallicity forthe population to select the appropriate single stellar population (SSP)equivalent M/L. Using this method, the maximum systematic error due to SFH onthe M/L of an early-type galaxy is $<$ 4$\%$ at 3.4 $\mu$m and typicaluncertainties due to errors in the age and metallicity create scatter of$\lesssim$13$\%$. The equivalent values for optical bands are more than 2-3times greater, even before considering uncertainties associated with internaldust extinction. 2) We demonstrate that if the EAGLE SFHs and metallicitiesaccurately reproduce the true properties of early-type galaxies, the use of aniterative approach to select a mass dependent M/L can provide even moreaccurate stellar masses for early-type galaxies, with typical uncertainties $<$9$\%$.

Being WISE II: Reducing the Influence of Star Formation History on the Mass-to-Light Ratio of Quiescent Galaxies