THE CLIMATE HISTORY OF MARS AS RECORDED BY THE GEOLOGIC RECORD
If valley networks do not represent the climatic conditions that occurred through the Noachian, then modified impact craters do. Modified impact craters occurred at all crater diameters; however, the degree of modification is independent of size. This indicates that modification processes were continuously (if not episodically) operating as new craters were forming on early Mars, as demonstrated by results of landscape evolution simulations presented by Barnhardt et al. [2008]. Unlike valley networks, which are restricted to a band near the equatorial region of Mars, modified impact craters also occur at higher latitudes suggesting that the erosional processes—and thus the associated climatic conditions—were global. This suggests that potentially early conditions were controlled by a primordial steam atmosphere that slowly collapsed and precipitated into the Martian regolith, eventually resulting in lakes and even an ocean. Unlike the Earth where most of the rock record from earlier conditions has been lost to erosion and plate tectonics, the spatial and temporal variations of the ancient climate as represented by the geology are preserved on Mars. The implications are not only for understanding the history of water on Mars, but the origin of life on Earth as well as habitable zones and extrasolar planets.