The Stellar Mass in and around Isolated Central Galaxies: Connections to the Total Mass Distribution through Galaxy–Galaxy Lensing in the Hyper Suprime-Cam Survey.

Using photometrically selected galaxies from the Hyper Suprime-Cam (HSC) survey, we measure the stellar-mass density profiles for satellite galaxies around isolated central galaxies (ICGs) from SDSS/DR7 at z ∼ 0.1. By stacking HSC images, we also measure the projected stellar-mass density profiles for ICGs and their stellar halos. The total mass distributions are further measured from HSC weak-lensing signals. ICGs dominate within ∼0.15 times the halo virial radius (0.15 R200). The stellar mass versus total mass fractions drop with the increase in projected distance up to ∼0.15 R200, beyond which they are less than 1% while staying almost constant. The integrated stellar mass in satellites is proportional to the virial mass of the host halo, M200, for ICGs more massive than 1010.5M⊙, i.e., M*,sat ∝ M200, whereas the relation between the stellar mass of ICGs + stellar halos and M200 is close to. Below 1010.5M⊙, the change in M200 is much slower with the decrease in M*,ICG+diffuse. At fixed stellar mass, red ICGs are hosted by more massive dark matter halos and have more satellites. At M200 ∼ 1012.7M⊙, both M*,sat and the fraction of stellar mass in satellites versus total stellar mass, fsat, tend to be marginally higher around blue ICGs. fsat increases with the increase in both M*,ICG+diffuse and M200, and scales more linearly with M200. We provide best-fitting relations to M200 versus M*,ICG+diffuse, M*,sat or M*,ICG+diffuse + M*,sat, and to fsat versus M200 or M*,ICG+diffuse, for red and blue ICGs separately. [ABSTRACT FROM AUTHOR]