Details

Autor(en) / Beteiligte

• Wang, Wenting
• Li, Xiangchong
• Shi, Jingjing
• Han, Jiaxin
• Yasuda, Naoki
• Jing, Yipeng
• More, Surhud
• Takada, Masahiro
• Miyatake, Hironao
• Nishizawa, Atsushi J.

Titel

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

Ist Teil von

• The Astrophysical journal, 2021-09, Vol.919 (1), p.25

Ort / Verlag

Philadelphia: The American Astronomical Society

Erscheinungsjahr

2021

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• Abstract 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 R 200 ). The stellar mass versus total mass fractions drop with the increase in projected distance up 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 ⊙ , i.e., M *,sat ∝ M 200 , whereas the relation between the stellar mass of ICGs + stellar halos and M 200 is close to M * , ICG + diffuse ∝ M 200 1 / 2 . Below 10 10.5 M ⊙ , 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 ∼ 10 12.7 M ⊙ , 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.