We simultaneously present constraints on the stellar-to-halo mass relation for central and satellite galaxies through a weak lensing analysis of spectroscopically classified galaxies . Using overlapping data from the 4th data release of the Kilo-Degree Survey ( KiDS ) , and the Galaxy And Mass Assembly survey ( GAMA ) , we find that satellite galaxies are hosted by halo masses that are 0.53 \pm 0.39 dex ( 68 % confidence , 3 \sigma detection ) smaller than those of central galaxies of the same stellar mass ( for a stellar mass of \log ( M _ { \star } / M _ { \odot } ) = 10.6 ) . This is consistent with galaxy formation models , whereby infalling satellite galaxies are preferentially stripped of their dark matter . We find consistent results with similar uncertainties when comparing constraints from a standard azimuthally averaged galaxy-galaxy lensing analysis and a two-dimensional likelihood analysis of the full shear field . As the latter approach is somewhat biased due to the lens incompleteness , and does not provide any improvement in precision when applied to actual data , we conclude that stacked tangential shear measurements are best-suited for studies of the galaxy-halo connection .