While primarily designed for radar studies of the Venus surface, the high effective isotropic radiated power (EIRP) from the Magellan spacecraft makes it an ideal transmitter for use in radio occultation measurements of the refractivity and absorptivity of the Venus atmosphere. Such experiments have been conducted involving transmissions at (2.3 \mathrm{GHz}) and (8.4 \mathrm{GHz}(13) (\mathrm{cm}) and (3.6 \mathrm{~cm}), respectively), during spacecraft ingress. Since the stability of the spacecraft transmitter is critical for accurately determining the Doppler shift and amplitude attenuation created as the ray penetrates the atmosphere, the spacecraft transmitter was locked to a (2.1 \mathrm{GHz}) uplink from a 70 -meter DSN station which also received the signals. Because of the high directivity of the spacecraft antenna, and the significant ray bending in the deep Venus atmosphere, a spacecraft tracking maneuver was designed to keep the spacecraft antenna pointed in the direction of the refracted ray path back to Earth. This tracking maneuver, plus the high EIRP of the Magellan transmitter has yielded (3.6 \mathrm{~cm}) refractivity and absorptivity profiles down to the (35 \mathrm{~km}) altitude and (13 \mathrm{~cm}) profiles down to the altitude of critical refraction (approximately (33 \mathrm{~km}) ). The statistical uncertainties in the derived profiles are significantly lower than those previously obtained, resulting in extremely accurate profiles of (\mathrm{H}{2} \mathrm{SO}{4}) (g)