Weak gravitational lensing is a powerful tool for understanding how galaxies populate dark matter halos. We use the publicly-available CFHTLenS galaxy catalog with shapes and photometric redshift information in order to measure the weak lensing signal of (CMASS) galaxies in the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey. By combining with the measurement of the projected auto-correlation function of CMASS galaxies over the entire BOSS DR11 area, we fit a halo model to the measurements assuming a ΛCDM cosmological model. I will present astrophysical constraints on the halo occupation distribution of CMASS galaxies, the structure of their dark matter halos, and the amount of stellar mass within these galaxies obtained from our analysis. Finally, I will also present cosmological constraints on the matter density parameter and amplitude of fluctuations using this new data. I will contrast these and our previous SDSS-I results with those obtained from the cosmic microwave background experiment Planck and discuss the interesting tensions between these results. I will conclude by highlighting the future prospects of such analyses with the Hyper Suprime-cam survey.