  We perform a consistent comparison of the mass and mass profiles of massive
($M_\star > 10^{11.4}M_{\odot}$) central galaxies at z~0.4 from deep Hyper
Suprime-Cam (HSC) observations and from the Illustris, TNG100, and Ponos
simulations. Weak lensing measurements from HSC enable measurements at fixed
halo mass and provide constraints on the strength and impact of feedback at
different halo mass scales. We compare the stellar mass function (SMF) and the
Stellar-to-Halo Mass Relation (SHMR) at various radii and show that the radius
at which the comparison is performed is important. In general, Illustris and
TNG100 display steeper values of $\alpha$ where $M_{\star}\propto M_{\rm
vir}^{\alpha}$. These differences are more pronounced for Illustris than for
TNG100 and in the inner rather than outer regions of galaxies. Differences in
the inner regions may suggest that TNG100 is too efficient at quenching in-situ
star formation at $M_{\rm vir}\simeq10^{13} M_{\odot}$ but not efficient enough
at $M_{\rm vir}\simeq10^{14} M_{\odot}$. The outer stellar masses are in
excellent agreement with our observations at $M_{\rm vir}\simeq10^{13}
M_{\odot}$, but both Illustris and TNG100 display excess outer mass as $M_{\rm
vir}\simeq10^{14} M_{\odot}$ (by ~0.25 and ~0.12 dex, respectively). We argue
that reducing stellar growth at early times in $M_\star \sim 10^{9-10}
M_{\odot}$ galaxies would help to prevent excess ex-situ growth at this mass
scale. The Ponos simulations do not implement AGN feedback and display an
excess mass of ~0.5 dex at $r<30$ kpc compared to HSC which is indicative of
over-cooling and excess star formation in the central regions. Joint
comparisons between weak lensing and galaxy stellar profiles are a direct test
of whether simulations build and deposit galaxy mass in the correct dark matter
halos and thereby provide powerful constraints on the physics of feedback and
galaxy growth.
