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Within a galaxy the stellar mass-to-light ratio $\Upsilon_*$ is not constant.Spatially resolved kinematics of nearby early-type galaxies suggest thatallowing for a variable initial mass function (IMF) returns significantlylarger $\Upsilon_*$ gradients than if the IMF is held fixed. If $\Upsilon_*$ isgreater in the central regions, then ignoring the IMF-driven gradient canoverestimate $M_*^{\rm dyn}$ by as much as a factor of two for the most massivegalaxies, though stellar population estimates $M_*^{\rm SP}$ are also affected.Large $\Upsilon_*$-gradients have four main consequences: First, $M_*^{\rmdyn}$ cannot be estimated independently of stellar population synthesis models.Second, if there is a lower limit to $\Upsilon_*$ and gradients are unknown,then requiring $M_*^{\rm dyn}=M_*^{\rm SP}$ constrains them. Third, ifgradients are stronger in more massive galaxies, then $M_*^{\rm dyn}$ and$M_*^{\rm SP}$ can be brought into agreement, not by shifting $M_*^{\rm SP}$upwards by invoking constant bottom-heavy IMFs, as advocated by a number ofrecent studies, but by revising $M_*^{\rm dyn}$ estimates in the literaturedownwards. Fourth, accounting for $\Upsilon_*$ gradients changes the high-massslope of the stellar mass function $\phi(M_*^{\rm dyn})$, and reduces theassociated stellar mass density. These conclusions potentially impact estimatesof the need for feedback and adiabatic contraction, so our results highlightthe importance of measuring $\Upsilon_*$ gradients in larger samples.

$M_*/L$ gradients driven by IMF variation: Large impact on dynamical stellar mass estimates