Photoelectric observations of Venus were made between 1963 and 1965 from the Harvard College Observatory's Boyden Station in South Africa. Interference filters with half widths between 50 and 200 Å were used to isolate ten narrow bands between 3150 Å and 1.06 μ; observations were also made in the standard UBV bands. Phase curves are presented and compared with previous observations. The spectral reflectivity is found to be strongly dependent on both wavelength and phase angle. Spherical (Bond) albedos are determined as a function of wavelength. The radiometric albedo of Venus is estimated to be A*=0.77±0.07, where the principal source of uncertainty is the visual magnitude of the sun. Abstract Photoelectric observations of Venus were made between 1963 and 1965 from the Harvard College Observatory's Boyden Station in South Africa. Interference filters with half widths between 50 and 200 Å were used to isolate ten narrow bands between 3150 Å and 1.06 μ; observations were also made in the standard UBV bands. Phase curves are presented and compared with previous observations. The spectral reflectivity is found to be strongly dependent on both wavelength and phase angle. Spherical (Bond) albedos are determined as a function of wavelength. The radiometric albedo of Venus is estimated to be A*=0.77±0.07, where the principal source of uncertainty is the visual magnitude of the sun.