The stellar-to-halo mass relation of GAMA galaxies from 100 square
  degrees of KiDS weak lensing data
  We study the stellar-to-halo mass relation of central galaxies in the range
9.7<log_10(M_*/h^-2 M_sun)<11.7 and z<0.4, obtained from a combined analysis of
the Kilo Degree Survey (KiDS) and the Galaxy And Mass Assembly (GAMA) survey.
We use ~100 deg^2 of KiDS data to study the lensing signal around galaxies for
which spectroscopic redshifts and stellar masses were determined by GAMA. We
show that lensing alone results in poor constraints on the stellar-to-halo mass
relation due to a degeneracy between the satellite fraction and the halo mass,
which is lifted when we simultaneously fit the stellar mass function. At
M_sun>5x10^10 h^-2 M_sun, the stellar mass increases with halo mass as
~M_h^0.25. The ratio of dark matter to stellar mass has a minimum at a halo
mass of 8x10^11 h^-1 M_sun with a value of M_h/M_*=56_-10^+16 [h]. We also use
the GAMA group catalogue to select centrals and satellites in groups with five
or more members, which trace regions in space where the local matter density is
higher than average, and determine for the first time the stellar-to-halo mass
relation in these denser environments. We find no significant differences
compared to the relation from the full sample, which suggests that the
stellar-to-halo mass relation does not vary strongly with local density.
Furthermore, we find that the stellar-to-halo mass relation of central galaxies
can also be obtained by modelling the lensing signal and stellar mass function
of satellite galaxies only, which shows that the assumptions to model the
satellite contribution in the halo model do not significantly bias the
stellar-to-halo mass relation. Finally, we show that the combination of weak
lensing with the stellar mass function can be used to test the purity of group
catalogues.
