This image is a mosaic of Magellan data over the Lakshmi region of Venus.  The image is centered at about 66 degrees north latitude and 10 degrees east longitude.  The prominent circular feature in the image is the crater Cleopatra, located on the eastern slopes of Maxwell Montes, the highest mountain range on Venus.  Cleopatra is about 100 km (60 miles) across and 2.5 km (1.5 miles) deep.  In previous data sets, scientists were unable to determine whether Cleopatra was an impact crater or a volcanic caldera.  High-resolution Magellan data indicates that Cleopatra is a double-ring impact basin, similar to double-ring impact basins identified on the Moon, Mars and Mercury.  The inner and outer rings have a hummocky appearance typical of very large impact craters.  On the eastern edge of Cleopatra, a flow can be seen that has breached the wall of the crater and flowed downhill to surround the ridges to the east.  This flow may have been produced by melting of rocks due to the impact or by volcanism triggered by the impact.  Resolution of the Magellan data is about 120 meters (400 feet). This Magellan full-resolution mosaic shows an area in Ishtar Terra on Venus, centered at 65 degrees north latitude and 6 degrees east longitude.  The prominent circular feature is Cleopatra, an impact crater, 100 kilometers (62 miles) in diameter.  Cleopatra lies on the eastern slopes of Maxwell Montes, the tallest mountain range on Venus at almost 11 kilometers (6.8 miles) above the mean planetary radius.  The western slopes of Maxwell Montes are very steep while the eastern slopes descend gradually.  The radar-bright return throughout most: of the image is present on Venus at high altitudes.  This phenomenon is thought to indicate the presence of a radar reflective mineral such as pyrite which is stable at the pressure and temperature found at higher altitudes.  The ridges and troughs throughout the image formed from compression of the surface.  It was not determined whether Cleopatra was a volcanic or impact crater until high-resolution Magellan data was received.  The rough, surrounding ejecta is visible in Magellan images, distinguishing it as a large double-ring impact basin similar to those found on other planetary bodies.  Lava from impact melt or volcanism triggered by the impact breached the crater rim and filled the troughs in the upper right-hand corner of the image.