  The clustering of galaxies and the matter distribution around them can be
described using the halo model complemented with a realistic description of the
way galaxies populate dark matter haloes. This has been used successfully to
describe statistical properties of samples of galaxies at z<0.2. Without
adjusting any model parameters, we compare the predicted weak lensing signal
induced by Luminous Red Galaxies to measurements from SDSS DR7 on much larger
scales (up to ~90 h_{70}^{-1} Mpc) and at higher redshift (z~0.4). We find
excellent agreement, suggesting that the model captures the main properties of
the galaxy-dark matter connection. To extend the comparison to lenses at even
higher redshifts we complement the SDSS data with shape measurements from the
deeper RCS2, resulting in precise lensing measurements for lenses up to z~0.6.
These measurements are also well described using the same model. Considering
solely these weak lensing measurements, we robustly assess that, up to z~0.6,
the number of central galaxies as a function of halo mass is well described by
a log-normal distribution with scatter $\sigma_{\log L_{\rm c}}=0.146\pm0.011$,
in agreement with previous independent studies at lower redshift. Our results
demonstrate the value of complementing the information about the properties of
the (lens) galaxies provided by SDSS with deeper, high-quality imaging data.
