Simulations of stellar convection are typically performed in parameter spaces orders of magnitude away from astrophysical regimes. To be astrophysically relevant, we need to be able to extrapolate simulated results into these regimes. Convection in stars is almost universally modelled using Mixing Length Theory which is “diffusion-free”: it exhibits no dependence on microphysical viscosity or conductivity. However, in typical simulations of Rayleigh-Bénard convection the heat transport is often throttled by thermal boundary layers and as such is not diffusion-free. Here, we examine simulations of convection designed to minimise the impact of these boundary layers through the use of internal heating and cooling profiles, as pioneered by Kazemi et al. 2020. We extend that work to rotating convection, and present results using both no-slip and more astrophysical free-slip boundary conditions. We find that in rotating no-slip cases the heat transport is diffusion-free. Surprisingly, we do not find the same thing in the more physical free-slip case, where we find a steeper-than-expected scaling.