  We present predictions for the galaxy-galaxy lensing profile from the EAGLE
hydrodynamical cosmological simulation at redshift z=0.18, in the spatial range
0.02 < R/(Mpc/h) < 2, and for five logarithmically equi-spaced stellar mass
bins in the range 10.3 < $\log_{10}$(Mstar/ $M_{\odot}$) < 11.8. We compare
these excess surface density profiles to the observed signal from background
galaxies imaged by the Kilo Degree Survey around spectroscopically confirmed
foreground galaxies from the GAMA survey. Exploiting the GAMA galaxy group
catalogue, the profiles of central and satellite galaxies are computed
separately for groups with at least five members to minimise contamination.
EAGLE predictions are in broad agreement with the observed profiles for both
central and satellite galaxies, although the signal is underestimated at
R$\approx$0.5-2 Mpc/h for the highest stellar mass bins. When central and
satellite galaxies are considered simultaneously, agreement is found only when
the selection function of lens galaxies is taken into account in detail.
Specifically, in the case of GAMA galaxies, it is crucial to account for the
variation of the fraction of satellite galaxies in bins of stellar mass induced
by the flux-limited nature of the survey. We report the inferred
stellar-to-halo mass relation and we find good agreement with recent published
results. We note how the precision of the galaxy-galaxy lensing profiles in the
simulation holds the potential to constrain fine-grained aspects of the
galaxy-dark matter connection.
