The masses of satellites in GAMA galaxy groups from 100 square degrees of KiDS weak lensing data

Abstract

We use the first 100 sq. deg. of overlap between the Kilo-Degree Survey (KiDS) and the Galaxy And Mass Assembly (GAMA) survey to determine the galaxy halo mass of ~10,000 spectroscopically-confirmed satellite galaxies in massive ($M>10^{13}{h}^{-1}{\mathrm{M}}_{\odot }$) galaxy groups. Separating the sample as a function of projected distance to the group centre, we jointly model the satellites and their host groups with Navarro-Frenk-White (NFW) density profiles, fully accounting for the data covariance. The probed satellite galaxies in these groups have total masses $\log M_{\mathrm{sub}}/(h^{-1}{\mathrm{M}}_{\odot })\approx 11.7-12.2$ consistent across group-centric distance within the errorbars. Given their typical stellar masses, $\log M_{\star ,\mathrm{sat}}/(h^{-2}{\mathrm{M}}_{\odot })\sim 10.5$, such total masses imply stellar mass fractions of $M_{\star ,\mathrm{sat}}/M_{\mathrm{sub}}\approx 0.04h^{-1}$ . The average subhalo hosting these satellite galaxies has a mass $M_{\mathrm{sub}}\sim 0.015M_{\mathrm{host}}$ independent of host halo mass, in broad agreement with the expectations of structure formation in a $\Lambda$CDM universe.

Accepted for publication in MNRAS. 14 pages; 9 figures, 2 tables. New subsection discussing sensitivity to contamination added during the refereeing process

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