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We use ~100 square deg of deep (>28.5 mag arcsec$^{-2}$ in i-band),high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam(HSC) survey to reveal the halo mass dependence of the surface mass densityprofiles and outer stellar envelopes of massive galaxies. The i-band imagesfrom the HSC survey reach ~4 magnitudes deeper than Sloan Digital Sky Surveyand enable us to directly trace stellar mass distributions to 100 kpc withoutrequiring stacking. We conclusively show that, at fixed stellar mass, thestellar profiles of massive galaxies depend on the masses of their dark matterhaloes. On average, massive central galaxies with $\log M_{\star, 100\\mathrm{kpc}}>11.6$ in more massive haloes at 0.3 < z < 0.5 have shallowerinner stellar mass density profiles (within ~10-20 kpc) and more prominentouter envelopes. These differences translate into a halo mass dependence of themass-size relation. Central galaxies in haloes with $\log M_{\rm{Halo}}>14.0$are ~20% larger in $R_{\mathrm{50}}$ at fixed stellar mass. Such dependence isalso reflected in the relationship between the stellar mass within 10 and 100kpc. Comparing to the mass--size relation, the $\log M_{\star, 100\\rm{kpc}}$-$\log M_{\star, 10\ \rm{kpc}}$ relation avoids the ambiguity in thedefinition of size, and can be straightforwardly compared with simulations. Ourresults demonstrate that, with deep images from HSC, we can quantify theconnection between halo mass and the outer stellar halo, which may provide newconstraints on the formation and assembly of massive central galaxies.

A Detection of the Environmental Dependence of the Sizes and Stellar Haloes of Massive Central Galaxies