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tokens: ( M *) or the cumulative number density of massive galaxies () over 0.4 z 1.0 (even after accounting for the Eddington bias using the forward-modeling method). In this section, we further investigate the evolution of the SMFs derived using specific sets of M * measurements. We first consider how the SMF changes based on different assumptions for the SFH. In Figure 8 , we show galaxy SMFs derived using stellar masses from different SFHs, including the effects of bursts. It is clear that the effects of SFH, at least among the set of stellar mass estimates used here, on the SMF are minor. In Figure 11 , we illustrate this by comparing the SMFs based on FSPS models with bursts () with those with no bursts (). While there is a slight (≲0.1 dex) increase in characteristic mass derived from SFHs that allow bursts, this falls within the range of uncertainties, and we do not consider it significant. In both cases where we measure the SMF from stellar masses with SFHs that allow and disallow bursts, we find that the characteristic mass shows little evolution from z = 0.4 to 1.5. In Figure 12 , we show the cumulative comoving number density of massive galaxies () derived using stellar masses with different SFHs. In both cases, we normalize the results to the measurement at z = 0.4. Over 0.4 z 1.0, the normalized comoving number density of massive galaxies is approximately constant regardless of SFH. Similarly, the number densities drop by ≲0.3 dex from z = 1.0 to z = 1.5 relative to that at z = 0.4 if we use stellar masses from SFHs that allow bursts. We conclude that the systematic uncertainties arising from the choice of SFH contribute 0.1 dex to the error budget in the growth of the characteristic stellar mass of massive galaxies, which we determined from the combined assumption-average mass function. 6.3. Dependence on SPS Models In Figure 9 we evaluate how three choices for the stellar population models underlying iSEDfit M * estimates impact the derived SMFs and constraints on the growth of massive galaxies. In all cases, we compare only models with smoothly varying SFHs (e.g., no bursts). We show again the FSPS SMF in the left panel. We compare these to the SMFs based on Bruzual Charlot ( 2003 ) masses (, middle panel) and Maraston ( 2005 ) masses (, right panel). The different SPS models lead to different trends in terms of the redshift of the evolution of both the characteristic mass ( M *) of the SMF and comoving number density of galaxies with stellar mass >10 11 M ⊙ . There are competing claims as to the ability of the treatment of TP-AGB stars in the Maraston ( 2005 ) models to reproduce the colors of galaxies and star clusters. Kriek et al. ( 2010 ) found that the Maraston ( 2005 ) models could not simultaneously reproduce the rest-frame optical and near-IR portions of galaxy SEDs. Similarly, Conroy Gunn ( 2010a ) showed that the Maraston ( 2005 ) models produce redder colors at intermediate ages inconsistent with the colors of star