We propose a new study using the Very Large Telescope Interferometer (VLTI) and gravitationally lensed broad absorption line (BAL) quasars to directly map the detailed structure of quasar outflows. Magnification increases the flux above VLTI detection limits and effectively stretches the apparent source, improving visibility and differential-phase signals at a specific baseline. By comparing differential interferometry and high-resolution spectroscopy across multiple lensed images, this method reveals outflow clumpiness, geometry, and kinematics. VLTI empirically anchors the outflow size, opening angle, inclination, and velocity fields. These measurements, combined with VLT spectroscopy, provide strong constraints on the mass outflow rates and kinetic luminosities of quasar winds, enabling improved calibration of AGN feedback models. While there are currently few suitable lensed BAL quasars, upcoming surveys like GAIA and LSST will provide enough statistically significant samples. This approach will transform our understanding of quasar-driven feedback, wind physics, and their role in the evolution of galaxies.