During 1999, this region became one of the top two that were being considered for the canceled Mars Surveyor 2001 Lander. The Isidis basin is very ancient. Thus, the Libya Montes that form the southern Isidis basin rim contain some of the oldest rocks available at the Martian surface, and a landing in this region might potentially provide information about conditions on early Mars.
After they formed by the Isidis impact, the Libya Montes were subsequently modified by a large variety of processes, including fluvial activity, wind erosion and impact cratering. In particular, precipitation induced surface runoff and groundwater seepage resulted in the formation of fluvial landforms, i.e., dense valley networks, broad and elongated valleys, delta deposits, alluvial fans, open-basin paleolakes and coastlines. Crater size - frequency distribution measurements ("crater counting") revealed that the majority of valleys were formed early in Martian history (more than 3.7 billion years ago, Late Noachian). However, recent studies show that the formation of valleys continued throughout the Middle Ages of Mars (Hesperian period) and stopped 3.1 billion years ago in the Late Hesperian.
Libya Montes "face"
Libya Montes has a face-like formation that appears even when viewed at different angles and with different sun angles. It can be found in the Mars Global Surveyor, MOC narrow-angle image M02-03051, located here (MSSS) or here (by USGS) (Crop). Also in HiRISE image ESP 018368 1830 (non-map projected) and ESP 018223 1830—a stereo pair that allows 3D terrain data to be generated. Like the more famous Face on Mars, it is an example of pareidolia.
| MOC Image M02-03051 (1999)
facial pareidola is about half-way down
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