We use the shear catalog from the CFHT Stripe-82 Survey to measure the subhalo masses of satellite galaxies in redMaPPer clusters .
Assuming a Chabrier Initial Mass Function ( IMF ) and a truncated NFW model for the subhalo mass distribution , we find that the sub-halo mass to galaxy stellar mass ratio increases as a function of projected halo-centric radius r _ { p } , from M _ { sub } / M _ { star } = 4.43 ^ { +6.63 } _ { -2.23 } at r _ { p } \in [ 0.1 , 0.3 ] { h ^ { -1 } Mpc } to M _ { sub } / M _ { star } = 75.40 ^ { +19.73 } _ { -19.09 } at r _ { p } \in [ 0.6 , 0.9 ] { h ^ { -1 } Mpc } .
We also investigate the dependence of subhalo masses on stellar mass by splitting satellite galaxies into two stellar mass bins : 10 < \log ( M _ { star } / { h ^ { -1 } M _ { \odot } } ) < 10.5 and 11 < \log ( M _ { star } / { h ^ { -1 } M _ { \odot } } ) < 12 .
The best-fit subhalo mass of the more massive satellite galaxy bin is larger than that of the less massive satellites : \log ( M _ { sub } / { h ^ { -1 } M _ { \odot } } ) = 11.14 ^ { +0.66 } _ { -0.73 } ( M _ { sub } / M _ { star } = 19.5 ^ { +19.8 } _ { -17.9 } ) versus \log ( M _ { sub } / { h ^ { -1 } M _ { \odot } } ) = 12.38 ^ { +0.16 } _ { -0.16 } ( M _ { sub } / M _ { star } = 21.1 ^ { +7.4 } _ { -7.7 } ) .