The masses of satellites in GAMA galaxy groups from 100 square degrees
  of KiDS weak lensing data
  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
($M > 10^{13}h^{-1}{\rm M}_\odot$) 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 $\log M_{\rm sub} /(h^{-1}{\rm
M}_\odot) \approx 11.7 - 12.2$ consistent across group-centric distance within
the errorbars. Given their typical stellar masses, $\log M_{\rm
\star,sat}/(h^{-2}{\rm M}_\odot) \sim 10.5$, such total masses imply stellar
mass fractions of $M_{\rm \star,sat} /M_{\rm sub} \approx 0.04 h^{-1}$ . The
average subhalo hosting these satellite galaxies has a mass $M_{\rm sub} \sim
0.015M_{\rm host}$ independent of host halo mass, in broad agreement with the
expectations of structure formation in a $\Lambda$CDM universe.
