Geologic maps have been produced for each of the seven Venera/Vega landing sites on Venus. The dominant terrain identified at all the sites is plains. The sites contain minor amounts of complex ridge terrain (CRT), complex terrain (CT), and an older plains (Po) that are all embayed by younger plains (Py). Some of the sites (Venera 9 and Vega 1 and 2) are made up of vast regional plains units while the other sites (Venera 8, 10, 13, and 14) contain more localized plains. The Venera 8 and 13 sites have unusual volcanic features associated with them and a nontholeiitic composition was measured by the landers at these sites. At the other five sites where a tholeiitic composition was measured, lava flows with morphologies that suggest an apparent low viscosity have been identified. This indicates a good correspondence between the geochemistry measured by the landers and the Magellan imagery. A good correlation also exists between the TV panoramas taken by four of the landers and the Magellan imagery. At the Venera 9, 10, 14 and Vega 1, 2 sites, the most likely material sampled are plains composed of tholeiitic lavas. A steep-sided dome, lamprophyre-like lavas, or ash beds are the most likely material sampled by the Venera 8 lander. The Venera 13 lander may have sampled lava flows from a corona-like feature or from a steep-sided dome in the southeast of the landing circle. Radiophysical properties of the landing sites show a good correspondence with the local geology, with most variations in backscatter, emissivity, and rms slopes reflecting differences in surface roughness. The Venera/Vega sites are good examples of typical venusian plains, indicating that geochemical measurements and TV observations provide representative characteristics of this most abundant terrain type on Venus. ¿ American Geophysical Union 1992