The quadrangle covers the region of 0° to 45° west longitude and 0° to 30° north latitude on Mars. This quadrangle contains parts of many regions: Chryse Planitia, Arabia Terra, Xanthe Terra, Margaritifer Terra, Meridiani Planum and Oxia Planum.

Mars Pathfinder landed in the Oxia Palus quadrangle at 19°08′N 33°13′W / 19.13°N 33.22°W / 19.13; -33.22, on July 4, 1997, at the intersection Tiu Valles and Ares Vallis.

Many craters within Oxia Palus are named after famous scientists. Besides Galilei and da Vinci, some of the people who discovered the atom and radiation are honored there: Curie, Becquerel, and Rutherford.

Mawrth Vallis was strongly considered as a landing site for NASA's Curiosity rover, the Mars Science Laboratory. It made it to at least the top two sites for NASA's EXoMars 2020 Rover mission. The exact location proposed for this landing is 22.16 N and 342.05 E.

The Mawrth Vallis region is well studied with more than 40 papers published in peer-reviewed publications. Near the Mawrth channel is a 200 meter high plateau with many exposed layers. Spectral studies have detected clay minerals that present as a sequence of layers. Clay minerals were probably deposited in the Early to Middle Noachian period. Later weathering exposed a variety of minerals such as kaolin, alunite, and jarosite. Later, volcanic material covered the region. This volcanic material would have protected any possible organic materials from radiation.

Another site in the Oxia Palus quadrangle has been picked for the EXoMars 2020 landing is at 18.14 N and 335.76 E. This site is of interest because of a long-duration aqueous system including a delta, possible biosignatures, and a variety of clays.

This quadrangle contains abundant evidence for past water in such forms as river valleys, lakes, springs, and chaos areas where water flowed out of the ground. A variety of clay minerals have been found in Oxia Palus. Clay is formed in water, and it is good for preserving microscopic evidence of ancient life. Recently, scientists have found strong evidence for a lake located in the Oxia Palus quadrangle that received drainage from Shalbatana Vallis. The study, carried out with HiRISE images, indicates that water formed a 30-mile-long canyon that opened up into a valley, deposited sediment, and created a delta. This delta and others around the basin imply the existence of a large, long-lived lake. Of special interest is evidence that the lake formed after the warm, wet period was thought to have ended. So, lakes may have been around much longer than previously thought. In October 2015, Oxia Planum, a plain located near 18°16′30″N 335°22′05″E / 18.275°N 335.368°E / 18.275; 335.368, was reported to be the preferred landing location for the ExoMars rover. An erosion-resistant layer on top of clay units may have preserved evidence of life.

The Mars Pathfinder found its landing site to contain a great deal of rocks. Analysis shows the area to have a greater density of rocks than 90% of Mars. Some of the rocks leaned against each other in a manner geologists term imbricated. It is believed strong flood waters in the past pushed the rocks around to face away from the flow. Some pebbles were rounded, perhaps from being tumbled in a stream. Some rocks have holes on their surfaces that seem to have been fluted by wind action. Small sand dunes are present. Parts of the ground are crusty, maybe due to cementing by a fluid containing minerals. In general the rocks show a dark gray color with patches of red dust or weathered appearance on their surfaces. Dust covers the lower 5–7 cm of some rocks, so they may have once been buried, but have now become exhumed. Three knobs, one large crater, and two small craters were visible on the horizon.

Results of Mars Pathfinder's Alpha Proton X-ray Spectrometer indicated that some rocks in the Oxia Palus quadrangle are like Earth's andesites. The discovery of andesites shows that some Martian rocks have been remelted and reprocessed. On Earth, Andesite forms when magma sits in pockets of rock while some of the iron and magnesium settle out. Consequently, the final rock contains less iron and magnesium and more silica. Volcanic rocks are usually classified by comparing the relative amount of alkalis (Na₂O and K₂O) with the amount of silica (SiO₂). Andesite is different from the rocks found in meteorites that have come from Mars.

By the time that final results of the mission were described in a series of articles in the journal Science (December 5, 1997), it was believed that the rock Yogi contained a coating of dust, but was similar to the rock Barnacle Bill. Calculations suggest that the two rocks contain mostly the minerals orthopyroxene (magnesium-iron silicate), feldspars (aluminum silicates of potassium, sodium, and calcium), quartz (silicon dioxide), with smaller amounts of magnetite, ilmenite, iron sulfide, and calcium phosphate.

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  Map of Oxia Palus labeled with major features
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  View from Mars Pathfinder
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  The Sojourner Rover is taking its Alpha Proton X-ray Spectrometer measurement of the Yogi Rock (NASA). Note: Sojourner Rover was the rover part of the Mars Pathfinder. It rolled off of the lander. This picture was taken by the lander.

By taking multiple images of the sky at different distances from the sun, scientists were able to determine that size of the particles in the pink haze was about 1 micrometer in radius. The color of some soils was similar to that of an iron oxyhydroxide phase which would support a warmer and wetter climate in the past. Pathfinder carried a series of magnets to examine the magnetic component of the dust. Eventually, all but one of the magnets developed a coating of dust. Since the weakest magnet did not attract any soil, it was concluded that the airborne dust did not contain pure magnetite or one type of maghemite. The dust probably was an aggregate possible cemented with ferric oxide (Fe₂O₃).

Winds were usually less than 10 m/s. Dust devils were detected in the early afternoon. The sky had a pink color. There was evidence of clouds and maybe fog.

Many large, ancient river valleys are found in this area; along with collapsed features, called Chaos. The Chaotic features may have collapsed when water came out onto the surface. Martian rivers begin with a Chaos region. A chaotic region can be recognized by a rat's nest of mesas, buttes, and hills, chopped through with valleys which in places look almost patterned. Some parts of this chaotic area have not collapsed completely—they are still formed into large mesas, so they may still contain water ice. Chaotic terrain occurs in numerous locations on Mars, and always gives the strong impression that something abruptly disturbed the ground. More information and more examples of chaos can be found at Chaos terrain. Chaos regions formed long ago. By counting craters (more craters in any given area means an older surface) and by studying the valleys' relations with other geological features, scientists have concluded the channels formed 2.0 to 3.8 billion years ago.

One generally accepted view for the formation of large outflow channels is that they were formed by catastrophic floods of water released from giant groundwater reservoirs. Perhaps, the water started to come out of the ground due to faulting or volcanic activity. Sometimes hot magma just travels under the surface. If that is the case, the ground will be heated, but there may be no evidence of lava at the surface. After water escapes, the surface collapses. Moving across the surface, the water would have simultaneously frozen and evaporated. Chunks of ice that would have rapidly formed may have enhanced the erosive power of the flood. Furthermore, the water may have frozen over at the surface, but continuing to flow underneath, eroding the ground as it moved along. Rivers in cold climates on the Earth often become ice-covered, yet continue to flow.

Such catastrophic floods have occurred on Earth. One commonly cited example is the Channeled Scabland of Washington State; it was formed by the breakout of water from the Pleistocene Lake Missoula. This region resembles the Martian outflow channels.

Research, published in January 2010, suggests that Mars had lakes, each around 20 km wide, along parts of the equator, in the Oxia Palus quadrangle. Although earlier research showed that Mars had a warm and wet early history that has long since dried up, these lakes existed in the Hesperian Epoch, which was a much earlier period. Using detailed images from NASA's Mars Reconnaissance Orbiter, the researchers speculate that there may have been increased volcanic activity, meteorite impacts, or shifts in Mars' orbit during this period to warm Mars' atmosphere enough to melt the abundant ice present in the ground. Volcanoes would have released gases that thickened the atmosphere for a temporary period, trapping more sunlight and making it warm enough for liquid water to exist. In this new study, channels were discovered that connected lake basins near Ares Vallis. When one lake filled up, its waters overflowed the banks and carved the channels to a lower area where another lake formed. These lakes would be another place to look for evidence of present or past life.

Aram Chaos is an ancient impact crater near the Martian equator, close to Ares Vallis. About 280 kilometers (170 mi) across, Aram lies in a region called Margaritifer Terra, where many water-carved channels show that floods poured out of the highlands onto the northern lowlands ages ago. The Thermal Emission Imaging System (THEMIS) on the Mars Odyssey orbiter found gray crystalline hematite on the floor of Aram. Hematite is an iron-oxide mineral that can precipitate when ground water circulates through iron-rich rocks, whether at normal temperatures or in hot springs. The floor of Aram contains huge blocks of collapsed, or chaotic, terrain that formed when water or ice was catastrophically removed. Elsewhere on Mars, the release of groundwater produced massive floods that eroded the large channels seen in Ares Vallis and similar outflow valleys. In Aram Chaos, however, the released water stayed mostly within the crater's ramparts, eroding only a small, shallow outlet channel in the eastern wall. Several minerals including hematite, sulfate minerals, and water-altered silicates in Aram suggests that a lake probably once existed within the crater. Because forming hematite requires liquid water, which could not long exist without a thick atmosphere, Mars must have had a much thicker atmosphere at some time in the past, when the hematite was formed.

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  Erosion in Aram Chaos, as seen by THEMIS
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  Blocks in Aram showing possible source of water, as seen by THEMIS

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  Hanging valleys in Aram Chaos, as seen by HiRISE under HiWish program
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  Wide view of Aram Chaos, as seen by HiRISE under the HiWish program. The black strip is where data was not gathered.
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  Aram Chaos with a light toned mound as seen by HiRISE under the HiWish program. The mound probably contains water bearing minerals.
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  Light toned mound as seen by HiRISE under the HiWish program. The mound probably contains water bearing minerals.

Oxia Palus is an interesting area with many craters showing layered sediments. Such sediments may have been deposited by water, wind, or volcanoes. The thickness of the layers is different in different craters. In Becquerel many layers are about 4 meters thick. In Crommelin crater the layers average 20 meters in thickness. At times, the top layer may be resistant to erosion and will form a feature called a mensa, the Latin word for table.

The pattern of layers within layers measured in Becquerel crater suggests that each layer was formed over a period of about 100,000 years. Moreover, every 10 layers can be grouped into larger bundles. So every 10-layer pattern took one million years to form (100,000 years/layer × 10 layers). The ten-layer pattern is repeated at least ten times, that is there are least ten bundles, each consisting of ten layers. It is believed that the layers relate to the cycle of changing tilt of Mars.

The tilt of the Earth's axis changes by only a little more than 2 degrees. In contrast, Mars's tilt varies by tens of degrees. Today, the tilt (or obliquity) of Mars is low, so the poles are the coldest places on the planet, while the equator is the warmest. This causes gases in the atmosphere, like water and carbon dioxide, to migrate poleward, where they turn into ice. When the obliquity is higher, the poles receive more sunlight, and those materials migrate away. When carbon dioxide moves from the poles, the atmospheric pressure increases, maybe causing a difference in the ability of winds to transport and deposit sand. With more water in the atmosphere, sand grains deposited on the surface may stick and cement together to form layers. This study was done using stereo topographic maps obtained by processing data from the high-resolution camera onboard NASA's Mars Reconnaissance Orbiter.

A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars.

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  Buttes, as seen by HiRISE under HiWish program. Buttes have layered rocks with a hard resistant cap rock on the top which protects the underlying rocks from erosion.
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  Becquerel layers, as seen by HiRISE. Click on image to see fault.
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  Mounds in craters showing layers are formed by the erosion of layers that were deposited after the impact.
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  Punsk Crater, as seen by HiRISE. Scale bar is 500 meters long. Click on image to see possible fine layers on floor. Image on right is an enlargement of south (bottom) wall of crater.
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  Hydraotes Chaos, as seen by HiRISE. Click on image to see channels and layers. Scale bar is 1000 meters long.
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  Grindavik Crater, as seen by HiRISE. Scale bar is 1000 meters long.
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  Layers in Monument Valley. These are accepted as being formed, at least in part, by water deposition. Since Mars contains similar layers, water remains as a major cause of layering on Mars.
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  Layered mesas, as seen by HiRISE under HiWish program. Location in Terra Meridiani.
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  Close-up of one of the mesas in previous photo showing layers. Mesa may be the remains of a lake in which sediments were deposited. Picture obtained with HiRISE, under HiWish program.
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  Wide view of layers, as seen by HiRISE under HiWish program
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  Close view of layers, as seen by HiRISE under HiWish program

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  Wide view of layered features, as seen by HiRISE under HiWish program
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  Close view of layered features, as seen by HiRISE under HiWish program

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  Wide view of layered features and ridges, as seen by HiRISE under HiWish program
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  Close view of layers, as seen by HiRISE under HiWish program
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  Close view of layers, as seen by HiRISE under HiWish program
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  Close view of layers, as seen by HiRISE under HiWish program
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  Close view of layers in a mound, as seen by HiRISE under HiWish program
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  Close view of layers, as seen by HiRISE under HiWish program
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  Small sets of layers in Aram Chaos, as seen by HiRISE under HiWish program
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  Layers and yardangs, as seen by HiRISE under HiWish program. Arrows point to some yardangs.

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  Wide view of layers, as seen by HiRISE. Black strip in middle is due to a malfunction.
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  Layers, as seen by HiRISE. Black strip in middle is due to a malfunction.
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  Layers, as seen by HiRISE. Black strip in middle is due to a malfunction. Colored strip is about 1 km across.
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  Close view of layers, as seen by HiRISE under HiWish program. Picture is about 1 km across.

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  Wide view of layers in a depression near Shalbatana Vallis, as seen by HiRISE under HiWish program
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  Close view of layers in a depression near Shalbatana Vallis, as seen by HiRISE under HiWish program
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  Close view of layers in a depression near Shalbatana Vallis, as seen by HiRISE under HiWish program

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  Wide view of layers, as seen by HiRISE under HiWish program
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  Close view of layers, as seen by HiRISE under HiWish program
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  Close view of layers, as seen by HiRISE under HiWish program. Box shows size of football field.
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  Close view of layers, as seen by HiRISE under HiWish program
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  Close view of layers, as seen by HiRISE under HiWish program. A fault is visible.
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  Close view of layers, as seen by HiRISE under HiWish program
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  Close view of layers, as seen by HiRISE under HiWish program
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  Layers, as seen by HiRISE under HiWish program
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  Wide view of various shapes created by erosion, as seen by HiRISE under HiWish program
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  Close color view of layered mesa and mound, as seen by HiRISE
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  Close view of edge of layered mesa, as seen by HiRISE
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  Close view of layered mesa with pyramid shapes, as seen by HiRISE under HiWish program
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  Wide view of layers in Danielson Crater, as seen by HiRISE under HiWish program
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  Close view of top of image of Danielson Crater, as seen by HiRISE (ESP_071634_1880)
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  Close view of top of image of Danielson. Arrows indicate parts that are enlarged.
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  Layers in Danielson Crater with enlargements of some spots (indicated with arrows)
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  Layers in Danielson Crater with enlargements of some spots (indicated with arrows)
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  Layers in Danielson Crater, as seen by HiRISE under HiWish program
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  Layers in Danielson Crater, as seen by HiRISE under HiWish program

Linear ridge networks are found in various places on Mars in and around craters. Ridges often appear as mostly straight segments that intersect in a lattice-like manner. They are hundreds of meters long, tens of meters high, and several meters wide. It is thought that impacts created fractures in the surface, these fractures later acted as channels for fluids. Fluids cemented the structures. With the passage of time, surrounding material was eroded away, thereby leaving hard ridges behind. Since the ridges occur in locations with clay, these formations could serve as a marker for clay which requires water for its formation. Water here could have supported past life in these locations. Clay may also preserve fossils or other traces of past life.

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  Possible dikes and layered structures, as seen by HiRISE under HiWish program. These may be part of linear ridge networks that are produced with impact craters.
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  Possible fault along a butte, as seen by HiRISE under HiWish program. These may be part of linear ridge networks that are produced with impact craters.

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  Layers and ridge networks, as seen by HiRISE under HiWish program
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  Layers in a mound and ridge networks, as seen by HiRISE under HiWish program
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  Ridge networks of various sizes, as seen by HiRISE under HiWish program
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  Ridge networks, as seen by HiRISE under HiWish program

Many areas of Mars show wrinkles on the surface, called wrinkle ridges. They are elongated and are often found on smooth area of Mars. Because they are wide, gentle topographic highs, they are sometimes hard to see. Although first thought to be caused by lava flows, they are now generally thought to be more likely caused by compressional tectonic forces that cause folding and faulting. A wrinkle ridge is visible in the image to the right of Ares Vallis.

A picture below right, taken of layers in Becquerel Crater, shows a straight line that represents a fault. Faults are breaks in rocks where movement has taken place. The movement may be only inches or much more. Faults can be very significant, as the break in the rock is a focus for erosion and, more importantly, can allow fluids containing dissolved minerals to rise, then be deposited. Some of the major ore deposits on Earth are formed by this process.

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  Faults in Danielson Crater, as seen by HiRISE under HiWish program
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  Faults and layers in Danielson Crater, as seen by HiRISE under HiWish program
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  Faults in Crommelin Crater, as seen by HiRISE under HiWish program
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  Fault in Crommelin Crater, as seen by HiRISE under HiWish program

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  Faults in layers, as seen by HiRise under HiWish program Faults in layers, as seen by HiRise under HiWish program Image is about 1 km across.
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  Faults in layers, as seen by HiRise under HiWish program Image is about 1 km across.
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  Faults in layers, as seen by HiRise under HiWish program Image is about 1 km across.
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  Faults in layers, as seen by HiRise under HiWish program Image is about 1 km across.
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  Faults in layers, as seen by HiRise under HiWish program Image is about 1 km across.

A study of images taken with the High Resolution Imaging Science Experiment (HiRISE) on the Mars Reconnaissance Orbiter strongly suggests that hot springs once existed in Vernal Crater, in the Oxia Palus quadrangle. These springs may have provided a long-time location for life. Furthermore, mineral deposits associated with these springs may have preserved traces of Martian life. In Vernal Crater on a dark part of the floor, two light-toned, elliptical structures closely resemble hot springs on the Earth. They have inner and outer halos, with roughly circular depressions. A large number of hills are lined up close to the springs. These are thought to have formed by the movement of fluids along the boundaries of dipping beds. A picture below shows these springs. One of the depressions is visible. The discovery of opaline silica by the Mars Rovers, on the surface also suggests the presence of hot springs. Opaline silica is often deposited in hot springs. Scientists proposed this area should be visited by the Mars Science Laboratory.

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  Vernal Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter)
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  Springs in Vernal Crater, as seen by HIRISE

The crater Mojave, in the Xanthe Terra region, has alluvial fans that look remarkably similar to landforms in the Mojave Desert in the American southwest. As on Earth, the largest rocks are near the mouths of the fans. Because channels start at the tops of ridges, it is believed they were formed by heavy downpours. Researchers have suggested that the rain may have been initiated by impacts.

Mojave is approximately 2,604 meters (1.618 miles) deep. Its depth relative to its diameter and its ray system are indications it is very young. Crater counts of its ejecta blanket give an age of about 3 million years. It is considered the most recent crater of its size on Mars, and has been identified as the probable source of the shergottite meteorites collected on Earth.

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  Alluvial Fans in Mojave, as seen by HiRISE. The crater rim is on the right. A branched network of channels runs down towards the left.
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  Another view of Mojave from HiRISE (north is at bottom)

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  MOLA map showing Firsoff Crater and other nearby craters. Colors indicate elevations.
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  Layers in Firsoff Crater, as seen by HiRISE
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  Close-up of layers in Firsoff Crater, as seen by HiRISE Note: this is an enlargement of the previous image of Firsoff Crater.
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  Top part of previous images, as seen by HiRISE. Note: dark parts are basalt sand.
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  Fault across layers in a mesa in Firsoff Crater, as seen by HiRISE under HiWish program
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  Close-up of layers in Firsoff Crater, as seen by HiRISE under HiWish program
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  Wide view of layered surface in Firsoff Crater, as seen by HiRISE under HiWish program
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  Layers in Firsoff crater with a box showing the size of a football field. Picture taken by HiRISE under HiWish program.
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  Layers and faults in Firsoff Crater, as seen by HiRISE under HiWish program. Arrows show one large fault, but there are other smaller ones in the picture.
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  Layered mound, as seen by HiRISE under HiWish program. The white box represents the size of a football field for scale.

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  Layered mesas, as seen by HiRISE
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  Layered mesa, as seen by HiRISE
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  Layered mesa, as seen by HiRISE. Box is the size of a football field.
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  Layered mounds
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  Eroded layers, as seen by HiRISE. Picture is about 1 km across.
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  Crommelin (Martian crater), as seen by CTX camera (on MRO)
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  Crommelin crater showing layers and dust devil tracks, as seen by CTX camera. Note: this is an enlargement of a previous image of Crommelin crater.
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  Crommelin crater showing layers arranged in the shape of ovals, as seen by CTX camera. Note: this is an enlargement of a previous image of Crommelin crater.
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  Crommelin crater showing layers in buttes and inside a small crater, as seen by CTX camera. Note: this is an enlargement of a previous image of Crommelin crater.
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  Crommelin crater, showing layers, as seen by HiRISE
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  Butte in Crommelin (Martian crater), as seen by HiRISE
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  Layers in Crommelin Crater, as seen by HiRISE
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  Layers in Crommelin Crater, as seen by HiRISE. Arrow indicates fault.
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  Crommelin Crater Layered Deposit, as seen by HiRISE. The color blue in the photo is a false color.

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  Wide view of layers in Crommelin crater, as seen by HiRISE . Parts of thi photo are enlarged in following images.
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  Close view of layered mound in Crommelin crater, as seen by HiRISE. Box indicates the size of a football field for scale.
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  Close view of layers in Crommelin crater, as seen by HiRISE
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  Close view of layers in Crommelin crater, as seen by HiRISE
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  Close view of layers in Crommelin crater, as seen by HiRISE. Arrow points to a fault.
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  Close view of layers in Crommelin crater, as seen by HiRISE
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  Close view of layers in Crommelin crater, as seen by HiRISE. Arrow points to a fault.

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  West side of Danielson Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Danielson has a great deal of regular layering.
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  Some of the layers of Danielson Crater is just visible in this CTX image. Dunes are also visible.
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  Many layers are visible in this HiRISE image of Danielson Crater. Dark dust serves to highlight some of the layers.
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  Wide-view of layers in Danielson Crater, as seen by HiRISE under HiWish program. Box shows location of next image. Dark parts of image are dark, basalt sand sitting on level places.
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  Enlargement of previous image of Danielson Crater showing a fault and layers. Image taken with HiRISE, under HiWish program.
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  Wide view of part of Danielson Crater, as seen by HiRISE under HiWish program
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  Enlargement of previous image of Danielson Crater, as seen by HiRISE under HiWish program. The box represents the size of a football field.
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  Close up of layers in Danielson Crater, as seen by HiRISE under HiWish program—boulders are visible, as well as dark sand
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  Layers in Danielson Crater with dust devil tracks at the top of the picture, as seen by HiRISE under HiWish program

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  Wide view of layers in Danielson Crater, as seen by HiRISE under HiWish program
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  Wide view of layers in Danielson Crater, as seen by HiRISE under HiWish program. Center color band of the HiRISE image is visible.
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  Layers in Danielson Crater, as seen by HiRISE under HiWish program. Scale is shown.
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  Layers and dark dust in Danielson Crater, as seen by HiRISE under HiWish program
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  Layers and dark dust in Danielson Crater, as seen by HiRISE under HiWish program
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  Layers, crater, and mounds on floor of Danielson Crater, as seen by HiRISE under HiWish program
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  Close view of crater on floor of Danielson Crater, as seen by HiRISE under HiWish program
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  Layered mound on floor of Danielson Crater, as seen by HiRISE under HiWish program
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  Close, color view of layers and dark dust on floor of Danielson Crater, as seen by HiRISE under HiWish program
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  Close, color view of layers and dark dust on floor of Danielson Crater, as seen by HiRISE under HiWish program. Boulders are visible in the image.
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  Close, color view of layers and dark dust on floor of Danielson Crater, as seen by HiRISE under HiWish program. Faults are indicated with arrows.
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  Close view of layers on floor of Danielson Crater, as seen by HiRISE under HiWish program. Some faults are visible in image.
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  Close, color view of layers and dark dust on floor of Danielson Crater, as seen by HiRISE under HiWish program. Some small faults are visible in image.

A pedestal crater is a crater with its ejecta sitting above the surrounding terrain and thereby forming a raised platform (like a pedestal). They form when an impact crater ejects material which forms an erosion-resistant layer, thus causing the immediate area to erode more slowly than the rest of the region. Some pedestals have been accurately measured to be hundreds of meters above the surrounding area. This means that hundreds of meters of material were eroded away. The result is that both the crater and its ejecta blanket stand above the surroundings. Pedestal craters were first observed during the Mariner missions.

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  Pedestal Crater and ridge in Oxia Palus quadrangle, as seen by HiRISE. Click on image to see detail of the edge of the pedestal crater. The flat-topped ridge near the top of the image was once a river that became inverted. The pedestal crater superposes the ridge, so it is younger.
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  Pedestal craters form when the ejecta from impacts protect the underlying material from erosion. As a result of this process, craters appear perched above their surroundings.
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  Drawing shows a later idea of how some pedestal craters form. In this way of thinking, an impacting projectile goes into an ice-rich layer—but no further. Heat and wind from the impact hardens the surface against erosion. This hardening can be accomplished by the melting of ice which produces a salt/mineral solution thereby cementing the surface.

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  Wide CTX image of layers under the ejecta surface of a pedestal crater
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  Layers under top layer of pedestal crater, as seen by HiRISE under HiWish program
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  Close view of layers under ejecta surface of pedestal crater, as seen by HiRISE under HiWish program
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  Close view of layers under ejecta surface of pedestal crater, as seen by HiRISE under HiWish program

Impact craters generally have rims with ejecta around them; in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak. The peak is caused by a rebound of the crater floor following the impact. Sometimes craters display layers. Since the collision that produces a crater is like a powerful explosion, rocks from deep underground are tossed onto the surface. Hence, craters can show what lies deep under the surface.

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  Trouvelot Crater floor, as seen by HiRISE
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  Central peak of Radau Crater, as seen by HiRISE
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  Kipini Crater south rim, as seen by HiRISE. Scale bar is 500 meters long.
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  Sagan Crater Central Peak Ring, as seen by HiRISE. Scale bar is 500 meters long.
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  Curie Crater, as seen by HiRISE
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  Close-up of layers in central mound of Curie Crater, as seen by HiRISE. Layers may have formed in a lake.
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  Tayray Crater, as seen by HiRISE
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  Light toned rocks surrounded by dark material along wall of a crater, as seen by HiRISE under HiWish program. Click on image for a better view.
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  Western side of Rutherford Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Light-toned deposits are visible.
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  Dunes on floor of Rutherford Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image.
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  Da Vinci (Martian crater), as seen by CTX camera (on Mars Reconnaissance Orbiter)
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  Masursky Crater Floor, as seen by HiRISE
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  Marth Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).
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  Marth Crater showing dunes, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image of Marth Crater.
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  Ejecta margin of unnamed crater, as seen by HiRISE under HiWish program
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  Eroded craters, as seen by HiRISE. One crater is half eroded away. Another crater has eroded to form a tall, thin rim, and its ejecta has been eroded away. This image is part of an image that was named HiRISE picture of the day.
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  One crater here has a depression on its floor. This may be due to the impacting body going down to a softer material.

Vallis (plural valles) is the Latin word for valley. It is used in planetary geology for the naming of landform features on other planets.

Vallis was used for old river valleys that were discovered on Mars, when probes were first sent to Mars. The Viking Orbiters caused a revolution in our ideas about water on Mars; huge river valleys were found in many areas. Spacecraft cameras showed that floods of water broke through dams, carved deep valleys, eroded grooves into bedrock, and traveled thousands of kilometers.

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  Shalbatana Vallis, as seen by HiRISE. The scale bar is 500 meters long.
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  Shalbatana Vallis Floor, as seen by HiRISE. Scale bar is 1000 meters long.
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  Close-up of Simud Valles, as seen by HiRISE
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  Ares Vallis, as seen by Viking. The channel is 25 km wide and about 1 km deep.
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  Channels in Ares Vallis Region, as seen by HiRISE
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  Ares Valles, as seen by HiRISE
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  Tiu Valles Ridges, as seen by HiRISE. Ridges were probably formed by running water. Scale bar is 1 km long.
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  Teardrop-shaped islands caused by flood waters from Maja Valles, as seen by Viking Orbiter. Image is located in Oxia Palus quadrangle. The islands are formed in the ejecta of Lod Crater, Bok Crater, and Gold Crater.
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  Valley, as seen by HiRISE under HiWish program

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  Hanging valleys in Aram Chaos, as seen by HiRISE under HiWish program

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  Erosion has created huge pits with steep walls. Picture from Mars Odyssey THEMIS.
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  Eos Chasma with a Mensa, a flat topped prominence with cliff-like edges, as seen by THEMIS. In many places rock layers are visible.
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  Hydaspis Chaos, as seen by HiRISE
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  Chaos along Shalbatana Vallis as seen by HiRISE under HiWish program
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  Cyclic Bedding in Arabia Terra, as seen by HiRISE
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  Cliffs and canyons in Arabia, as seen by HiRISE
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  Cap rock breaking up into large blocks, as seen by HiRISE under HiWish program
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  Rock breaking up into large blocks, as seen by HiRISE under HiWish program
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  FPyramid shapes in Oxia Palus quadrangle

A large part of the popular movie The Martian takes place in the Oxia Palus quadrangle.

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  Much of the astronaut's journey takes place in Oxia Palus quadrangle.

0°N 180°W / 0°N 180°W / 0; -180

0°N 0°W / 0°N -0°E / 0; -0

90°N 0°W / 90°N -0°E / 90; -0

MC-01

Mare Boreum

MC-02

Diacria

MC-03

Arcadia

MC-04

Mare Acidalium

MC-05

Ismenius Lacus

MC-06

Casius

MC-07

Cebrenia

MC-08

Amazonis

MC-09

Tharsis

MC-10

Lunae Palus

MC-11

Oxia Palus

MC-12

Arabia

MC-13

Syrtis Major

MC-14

Amenthes

MC-15

Elysium

MC-16

Memnonia

MC-17

Phoenicis

MC-18

Coprates

MC-19

Margaritifer

MC-20

Sabaeus

MC-21

Iapygia

MC-22

Tyrrhenum

MC-23

Aeolis

MC-24

Phaethontis

MC-25

Thaumasia

MC-26

Argyre

MC-27

Noachis

MC-28

Hellas

MC-29

Eridania

MC-30

Mare Australe

Clickable image of the 30 cartographic quadrangles of Mars, defined by the USGS. Quadrangle numbers (beginning with MC for "Mars Chart") and names link to the corresponding articles. North is at the top; 0°N 180°W / 0°N 180°W / 0; -180 is at the far left on the equator. The map images were taken by the Mars Global Surveyor.

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