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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 HyperSuprime-Cam (HSC) observations and from the Illustris, TNG100, and Ponossimulations. Weak lensing measurements from HSC enable measurements at fixedhalo mass and provide constraints on the strength and impact of feedback atdifferent halo mass scales. We compare the stellar mass function (SMF) and theStellar-to-Halo Mass Relation (SHMR) at various radii and show that the radiusat which the comparison is performed is important. In general, Illustris andTNG100 display steeper values of $\alpha$ where $M_{\star}\propto M_{\rmvir}^{\alpha}$. These differences are more pronounced for Illustris than forTNG100 and in the inner rather than outer regions of galaxies. Differences inthe inner regions may suggest that TNG100 is too efficient at quenching in-situstar formation at $M_{\rm vir}\simeq10^{13} M_{\odot}$ but not efficient enoughat $M_{\rm vir}\simeq10^{14} M_{\odot}$. The outer stellar masses are inexcellent agreement with our observations at $M_{\rm vir}\simeq10^{13}M_{\odot}$, but both Illustris and TNG100 display excess outer mass as $M_{\rmvir}\simeq10^{14} M_{\odot}$ (by ~0.25 and ~0.12 dex, respectively). We arguethat 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 massscale. The Ponos simulations do not implement AGN feedback and display anexcess mass of ~0.5 dex at $r<30$ kpc compared to HSC which is indicative ofover-cooling and excess star formation in the central regions. Jointcomparisons between weak lensing and galaxy stellar profiles are a direct testof whether simulations build and deposit galaxy mass in the correct dark matterhalos and thereby provide powerful constraints on the physics of feedback andgalaxy growth.

Stellar and Weak Lensing Profiles of Massive Galaxies in the Hyper-Suprime Cam Survey and in Hydrodynamic Simulations