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 similar to 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 similar to 0.15 times the halo virial radius (0.15 R (200)). The stellar mass versus total mass fractions drop with the increase in projected distance up to similar to 0.15 R (200), 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, M (200), for ICGs more massive than 10(10.5) M (circle dot), i.e., M (*,sat) proportional to M (200), whereas the relation between the stellar mass of ICGs + stellar halos and M (200) is close to M*,ICG+diffuse proportional to M2001/2 M (circle dot), the change in M (200) 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 M (200) similar to 10(12.7) M (circle dot), both M (*,sat) and the fraction of stellar mass in satellites versus total stellar mass, f (sat), tend to be marginally higher around blue ICGs. f (sat) increases with the increase in both M (*,ICG+diffuse) and M (200), and scales more linearly with M (200). We provide best-fitting relations to M (200) versus M (*,ICG+diffuse), M (*,sat) or M (*,ICG+diffuse) + M (*,sat), and to f (sat) versus M (200) or M (*,ICG+diffuse), for red and blue ICGs separately.