Galaxy-galaxy lensing measures the distortion of images of background galaxies caused by the gravitational deflection of light by foreground galaxies. We use this deflection to constrain the mass profiles of the dark matter halos of the lens galaxies. We find that for early-type galaxies the deflection is stronger and can be detected to larger distances from the centers than for late-type galaxies indicating that the halos of these galaxies are more massive and more extended. We model the lenses as singular isothermal spheres and use a Tully-Fisher/Faber-Jackson relation. We find that the velocity dispersion decreases when going outwards from the center. At distances r=30-300 kpc the velocity dispersion of an L* galaxy is 168 km/s (146-187 km/s, 1-sigma) averaged over all galaxy types. For early-type galaxies (SED<=45) we find 194 km/s (169-215 km/s, 1-sigma).

Fig.1: Galaxy-galaxy lensing signal measured for lens galaxies of different SED-types (early-type galaxy have small SED-type). The fits do not use the binned distribution shown but a much finer distribution. Used are only two fields (A901, S11). For the measurement only galaxies with redshift estimate were taken. Lens galaxies have R=18-22 and z=0.2-0.7, source galaxies have R=18-24 and z=0.8-1.5