The first 3 days (24 orbits) of radar mapping from the Magellan spacecraft have revealed the presence of a wide diversity of geologic features on the surface of Venus. This full-resolution mosaic centered at 20 south latitude, 337.4 east longitude is located between Navka and Lavinia Planitia and covers a region 475 kilometers (285 miles) wide and 545 kilometers (330 miles) long. Analysis of this area from lower resolution Arecibo data show that this is part of an extensive region identified as bright plains. The Magellan data reveals the detailed geologic characteristics of different land forms in these plains. Located along the left central edge of the image is a cluster of volcanic domes which range from 1.5 kilometers to 7.5 kilometers in diameter and cover a region 150 kilometers by 100 kilometers (90 miles by 60 miles). The domes and their deposits are located at the convergence of radar-bright lineaments which are interpreted to be faults and troughs. In some places the domes overlie the faults. The faults and troughs extend into the lower part image where they terminate against dark plains deposits and are cross cut at right angles by additional faults. These relations indicate that multiple episodes of faulting and volcanism have occurred. An irregular shaped impact crater (11 kilometers by 8 kilometers - or 7 miles by 5 miles) located in the lower left corner of the image is interpreted to have formed by multiple impacts resulting from the breakup in the atmosphere of a larger impactor. An extremely radar-dark circular region located along the right central edge of the image is interpreted as a possible region of sedimentary deposits.
