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 / ( h ^ { -1 } Mpc ) < 2 , and for five logarithmically equi-spaced stellar mass bins in the range 10.3 < \mathrm { log _ { 10 } } ( M _ { star } / { 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 h ^ { -1 } Mpc 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 .