Mars Geological Imaging

False color images showcasing Martian landscapes such as Candor Chasma and large impact craters, highlighting erosion and geological formations.

. Firsoff Crater - False Color. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of the floor of Firsoff Crater. Located in southern Arabia Terra, Firsoff Crater, and the neighboring Crommelin Crater, have large layered deposits on the crater floor. The circular feature at the bottom of the image is a smaller crater within Firsoff Crater. The layering of the interior deposit can be seen in the northern side of this smaller crater. Wind action has modified the large deposit. In this color combination dark blue typically indicates basaltic sand. Firsoff Crater is 90 km (56 miles) in diameter. The THEMIS VIS camera is capable of capturing color images of the Martian surface using five different color filters. In this mode of operation, the spatial reso

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of Candor Chasma. Candor Chasma is one of the largest canyons that make up Valles Marineris. It is approximately 810 km long (503 miles) and has is divided into two regions - eastern and western Candor. Candor is located south of Ophir Chasma and north of Melas Chasma. The border with Melas Chasma contains many large landslide deposits. The floor of Candor Chasma includes a variety of landforms, including layered deposits (seen in this image), dunes, landslide deposits and steep sided cliffs and mesas. Many forms of erosion have shaped Candor Chasma. There is evidence of wind and water erosion, as well as significant gravity driven mass wasting (landslides). Orbit Number 71132 Latitude -6.71232 Longit

This observation from NASA's Mars Reconnaissance Orbiter shows part of the floor of a large impact crater in the southern highlands, north of the giant Hellas impact basin.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of Candor Labes.

Meridiani

This observation from NASA's Mars Reconnaissance Orbiter (MRO) shows part of the floor of a large impact crater in the southern highlands, north of the giant Hellas impact basin.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of Iani Chaos.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of the floor of Gale Crater.

. Firsoff Crater - False Color. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of the floor of Firsoff Crater. Located in southern Arabia Terra, Firsoff Crater, and the neighboring Crommelin Crater, have large layered deposits on the crater floor. The circular feature at the bottom of the image is a smaller crater within Firsoff Crater. The layering of the interior deposit can be seen in the northern side of this smaller crater. Wind action has modified the large deposit. In this color combination dark blue typically indicates basaltic sand. Firsoff Crater is 90 km (56 miles) in diameter. The THEMIS VIS camera is capable of capturing color images of the Martian surface using five different color filters. In this mode of operation, the spatial reso

This image shows part of the Nili Fossae region

This image from NASA's Mars Reconnaissance Orbiter shows Gorgonum Basin, one of several large basins within the Terra Sirenum region of Mars. Each basin has light-toned mounds, many of which contain clays. Scientists think that Terra Sirenum once had a large lake during an epoch called the Late Noachian/Early Hesperian, and each basin filled with sediments. The water within the lake may have altered these sediments to form the clays we now observe from orbit. Ma'adim Vallis, which drains into Gusev Crater where the Spirit rover landed, drained the water from this ancient lake. Why the basin floors exhibit mounds similar to chaos regions on Mars is unknown, but could be the result of collapse and subsequent erosion within the basins.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows a section of Tempe Fossae located in Tempe Terra.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of an unnamed crater in Terra Cimmeria.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of Iani Chaos.

This colorful image, acquired on May 21, 2018 by NASA's Mars Reconnaissance Orbiter, shows clays within the Eridania basin region. Many scientists using orbital data have proposed that a large lake may have once existed here during the Late Noachian through Early Hesperian time periods, and then much of the water drained out to the north via Ma'adim Vallis. Understanding where and what kind of clay exists within this region using CRISM data can help scientists learn more about how long the postulated lake existed and the water chemistry within the lake. More information is available at

This image covers a 26-kilometer-wide impact crater northeast of the Hellas impact basin as observed by NASA's Mars Reconnaissance Orbiter.

This false color image shows a tributary channel that empties into the main Ares Vallis channel. This tributary channel is located east of Ares Vallis. Located in Margaritifer Terra, Ares Vallis is part of a large system of channels that arise from Vallis Marineris and empty into Chryse Planitia. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Orbit Number 63809 Latitude 4.17241 Longitude 343.459 Instrument VIS Captured 2016-05-02 20 09

This image shows (part of) a 6-kilometer crater located on the northern slope of Bond Crater. Pole-facing gullies have eroded the northern slope of this small crater, located just west of where Uzboi Valles emanates from Bond and continues in a northerly direction. However, Hale Crater to the south has numerous gullies on its slopes and even on its central peak region. Researchers have analyzed both Bond and Hale Craters to try to determine why Bond has no gullies on its slopes, except for a small 7-km crater on the floor in its central area. (Reiss et al., 2009, PSS). The gullies in this observation have eroded into bedrock layers forming tributaries in the upper slope region and distributary channels further downslope on the debris fans. Research attributes these features to fluvial processes. (Gulick et al., 2018, Geol. Soc. London.)

Continuing Through Iani Chaos

This false color image shows part of Juventae Chasma. Located north of Valles Marineris, Juventae Chasma stretches for 180 kilometers (110 miles) east-west and 250 km (155 mi) north-south. Most of its floor lies 5,000 meters (16,000 feet) or more below the surrounding surface. Juventae Chasma is the source region for the outflow channel Maja Valles. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Orbit Number 65981 Latitude -2.2663 Longitude 298.189 Instrument VIS Captured 2016-10-28 18 05

This false color image shows part of Mangala Fossa - the linear depression in the bottom half of the image. The bright blue tones in this image are thought to be surface frost. It is winter time and early in the morning when this image was taken. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Orbit Number 63514 Latitude -15.1457 Longitude 219.23 Instrument VIS Captured 2016-04-08 12 54

In this Context Camera image in Terra Cimmeria, we see a 30-kilometer diameter crater, filled-in with materials that created bedrock, and through subsequent erosion, wind-driven particles. There is a ring of exposed light-toned bedrock at the base of the crater wall. This distinctive ring suggests high winds climbing up the crater wall slope may be responsible for the erosion and the extent of bedrock exposure we see. A close-up on the southeastern part of these deposits shows a mound of bedrock with beautiful color contrasts. The variation in color represents diverse minerals in the rock. There is also a small degraded crater (about 300-meter diameter) to the left of the exposed bedrock. Fine-grained materials trapped inside the crater appear as wind-driven ripples or small dune-forms. More information is available at

This VIS image is located in an unnamed crater in Arabia Terra. Dark blue tones in false color indicate basaltic sands. These sands have created the dunes seen in this image. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Orbit Number 62274 Latitude 10.6037 Longitude 358.441 Instrument VIS Captured 2015-12-28 09 57

Crater Wall on Mars Seen by Mars Reconnaissance Orbiter

CUEVA DE PEDRO FERNANDEZ: GRABADOS DE LINEAS PARALELAS EN LA PARED DERECHA DE LA GALERIA 34 (PANEL 3) ESTREMERA, COMUNIDAD DE MADRID, ESPAÑA.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of the plains and craters in Terra Sirenum. Orbit Number 59228 Latitude -37.9211 Longitude 224.753 Instrument VIS Captured 2015-04-21 13 06

Carbonate-Olivine Relationship in Nile Fossae, Mars

Candor Chasma

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of Iani Chaos.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part Syrtis Major Planum.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of Arabia Terra.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of Juventae Chasma. Orbit Number 43345 Latitude -4.63793 Longitude 296.778 Instrument VIS Captured 2011-09-22 06 32 http //photojournal.jpl.nasa.gov/catalog/PIA20987

The THEMIS VIS camera contains 5 filters. Data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows mesas and channels on the margin of Terra Sabaea.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of Aureum Chaos.

NASA's Mars Reconnaissance Orbiter reveals that gullies, or ravines, are landforms commonly found in the mid-latitudes on Mars, particularly in the Southern highlands.

This image was acquired on May 30, 2018 by NASA's Mars Reconnaissance Orbiter. This image shows inverted channels within a fan whose origin could be either fluvial (produced by the action of a stream) or alluvial (created by sedimentary deposits). If the fan is alluvial, then it formed on dry land. If the fan is fluvial, then it could have formed in water, like a delta. Similar fans with inverted channels are found in Eberswalde and Jezero craters, both of which are interpreted as deltas and are considered candidate locations of future rover landing sites. More information is available at

Mawrth Valles

Syrtis Major

The mid-latitudes of Mars are draped with deposits of water ice and dust on the order of tens of meters thick. The deposits are preserved to varying degrees, depending on latitude and the degree of dust cover that insulates and protects the ice from subliming away. These mantling deposits are thought to have been mobilized from the polar caps and redeposited from the atmosphere millions of years ago during periods when Mars' axial tilt was higher than it is today. The floor of this crater appears filled with such deposits, as evidenced by surface textures such as pits, hollows, grooves, and other small filled craters. The material has undergone viscous flow, resulting in many curved ridges. Much of the original ice may have been lost to sublimation, but it is likely that a significant amount of ice remains.

This image from NASA's Mars Reconnaissance Orbiter shows exposures of deposits along the plateau just to the south of Coprates Chasma.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of Sirenum Fossae.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of Melas Chasma.

This image shows some bright layered deposits exposed within a linear trough along the floor of the Ladon Basin as seen by NASA's Mars Reconnaissance Orbiter.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of Gale Crater.

April 5, 2007 - Mesas in the Nilosyrtis Mensae region of Mars appear in enhanced color in this image taken from the camera aboard the Mars Reconnaissance Orbiter.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of the floor of Candor Chasma.

NASA's Curiosity Mars rover and tracks from its driving are visible in this view from orbit, acquired on April 11, 2014, by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows the southeastern floor and rim of Virrat Crater (top of image), and the northern rim of Wukari Crater (bottom of image). These craters are located in Claritas Fossae. Orbit Number 67710 Latitude -31.2255 Longitude 257.255 Instrument VIS Captured 2017-03-20 04 07

This is a portion of an inverted fluvial channel in the region of Aeolis/Zephyria Plana, at the Martian equator as seen by NASA's Mars Reconnaissance Orbiter.

South Polar Residual Ice Cap

This observation from NASA's Mars Reconnaissance Orbiter (MRO) shows the very steep side of a plateau, part of the northern limit of the Kasei Valles system, which is one of the largest outflow channel systems on Mars.

Oxia Planum is broad clay-bearing surface between Mawrth and Ares Vallis that has been proposed as a future landing site on Mars. This image is from NASA's Mars Reconnaissance Orbiter.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the plains of Arabia Terra.

This observation from NASA's Mars Reconnaissance Orbiter shows samples of bedrock lithologies which give us a measure of the post-flood erosion and modification history for the floor of Kasei Valles.

This image covers channels cutting through the ancient rim of Savich Crater, a 188 kilometer-wide depression near the northeastern edge of the much larger Hellas impact basin. The channels were likely eroded by water flowing into Savich Crater long ago. Our image reveals layers of varying brightness and texture exposed along the channels. Individual boulders are visible within the brighter layers (appearing blue-white in this enhanced color view), while redder layers lack distinct boulders. The meter-scale boulders could have been transported by floodwaters, or perhaps could be an even more ancient rock unit broken apart by impacts that these channels subsequently exposed.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of Asimov Crater.

A conspicuous fretted channel, Reull Valles, Mars which dissects wall deposits of the large Hellas impact basin, trends southeast towards the basin floor as seen by NASA's Viking Orbiter 2.

The THEMIS camera contains 5 filters. Data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows some of the highlands between the multiple graben of Nili Fossae.

This image shows blocks of bright, layered rock embedded in darker material that are thought to have been deposited by a giant flood that occurred when Uzboi Valles breached the rim of Holden Crater.

A significant event has occurred in Inca City. The layer of seasonal ice has started to develop long cracks as evidenced by NASA's Mars Reconnaissance Orbiter.

Mamers Valles by Mars Odyssey

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of Solis Planum.

. Ariadnes Colles - False Color. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of Ariadnes Colles. The term colles means hills or knobs. In this false color combination the hills stand out against the darker surrounding plains. This difference is due to the amount of dust covering the hills versus the plains. The THEMIS VIS camera is capable of capturing color images of the Martian surface using five different color filters. In this mode of operation, the spatial resolution and coverage of the image must be reduced to accommodate the additional data volume produced from using multiple filters. To make a color image, three of the five filter images (each in grayscale) are selected. Each is contrast enhanced and then converted to a red, green, or b

Gullies eroded into the steep inner slope of an impact crater at this location appear perfectly pristine near Gasa Crater, in this image captured by NASA's Mars Reconnaissance Orbiter (MRO).

West Candor Chasm, Approximately Natural Color

This closeup from NASA's Mars Reconnaissance Orbiter covers a region in the Eridania Basin that shows interesting inverted ridges.

This image of Moreux Crater shows the highest elevations of the central peak, as well as the nearby sand dunes. In this false color image sand dunes are blue . Smaller patches of blue are located on the central peak materials and indicate where surface winds have moved fine materials on/off the peak deposits. The pitted and curvilinear morphology of the central peak deposits have been interpreted to have formed by glacial activity. Moreux Crater is located in northern Arabia Terra and has a diameter of 138 kilometers. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected dat

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows an unnamed crater in Terra Sabaea.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows an unnamed crater located on the floor of Newton Crater.

This terrain, as seen by NASA's Mars Reconnaissance Orbiter, looks like lumpy sediment on top of patterned ground. The lumpy sediment is likely just loosely consolidated because it is covered with spidery channels.

This image shows a cratered area to the southeast of the ExoMars 2020 Rosalind Franklin rover landing site at Oxia Palus. Selecting and characterizing landing sites is a balance between having science targets and avoiding potential obstacles, and HiRISE is used for both purposes. Craters like this one excavate material from within the crust, including both sedimentary and igneous rocks, and scatter this material far from the crater itself. This is one of the ways that so-called float rocks (rocks that are not connected to their original outcrop) can occur across a landing site they are often ejecta from distant impacts. Here, an ejecta blanket is visible in the rays of material surrounding this 2-kilometer diameter crater. The ExoMars rover has a suite of cameras and a close-up imager (called CLUPI) that will be used to study these float rocks. Studying such samples has been an important way of learning about the deep crust of Mars on previous missions, notably the Spirit and Opportuni

Ophir Chasma

This image is an oblique view from NASA's Mars Reconnaissance Orbiter of the sloping edge of the stack of icy layers over the South Pole has some interesting morphologies. The slope appears to be eroding from a combination of landslides, block falls, and sublimation. The bright icy exposure in the larger landslide scar (upper right) suggests that this was a relatively recent event. Small-scale textures over the scene are due to both blowing wind and the thermal expansion and contraction of shallow ice.

Mars digital-image mosaic merged with color of the MC-24 quadrangle, Phaethontis region of Mars. This image is from NASA's Viking Orbiter 1.

This pile of old rocks is an island surrounded by younger lava flows from Syrtis Major. This image was captured by NASA's Mars Reconnaissance Orbiter.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of Gusev Crater.

This image from NASA's MESSENGER spacecraft provides a perspective view of the center portion of Carnegie Rupes, a large tectonic landform, which cuts through Duccio crater.

Sand and Rock on a Crater Floor Seen by Mars Reconnaissance Orbiter

The THEMIS VIS camera contains 5 filters. The data from different filters can create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of the floor of Schaeberle Crater, including small dunes.

East Candor Chasma

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows a large dune covered sand sheet on the floor of this unnamed crater in Noachis Terra. Large scale dunes and dune fields cover the floor of many craters in this region west of Hellas Planitia including Rabe, Proctor, and Matara craters and numerous other unnamed craters. In this false color combination blue indicates basaltic sands. Orbit Number 67250 Latitude -49.0136 Longitude 34.0967 Instrument VIS Captured 2017-02-10 07 02

Elysium

An oblique, color image of central Valles Marineris, Mars showing relief of Ophir and Candor Chasmata; view toward north. The photograph is a composite of Viking high-resolution images in black and white and low-resolution images in color.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows the floor of Peridier Crater. Small dunes are visible in the image. Dark blue tones indicate basaltic sands. Peridier Crater is 94 km (58 miles) in diameter. Orbit Number 71276 Latitude 25.1422 Longitude 83.61 Instrument VIS Captured 2018-01-08 00 25

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of Gale Crater.

View of Mars, August 1976. Artist: Unknown

NASA's Mars Reconnaissance Orbiter used its HiRISE camera to obtain this view of an area with unusual texture on the southern floor of Gale Crater. An enigmatic deposit appears to have flowed into the small crater from the south.

This image taken by NASA's Mars Reconnaissance Orbiter shows Samara Valles, one of the longest ancient valley systems on Mars; its surface is mantled with dust as evidenced by the system of dunes that line the valley floor.

Arabia Terra is one of the more dusty regions on Mars, where ever-falling red dust covers the surface allowing only minor variations in color and tone as seen by NASA's Mars Reconnaissance Orbiter.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of Juventae Chasma.

NASA's Curiosity Mars rover can be seen at the 'Pahrump Hills' area of Gale Crater in this view from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.

Inverted Dendritic Stream Channels in Antoniadi Crater Seen by Mars Reconnaissance Orbiter

Sublime Sublimation, Not Subliminal

Terrain in Mawrth Vallis Region Seen by Mars Reconnaissance Orbiter

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of the plains of Terra Sirenum.

This picture from NASA's Viking Orbiter 2 shows areas of central Valles Marineris, Mars, including Candor Chasm (lower left), Ophir Chasm (lower right), and Hebes Chasm (upper right).

This image from NASA's Mars Reconnaissance Orbiter shows chlorides that have a bright appearance and are covered by other dark materials.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of the interior deposit in Firsoff Crater.

Rhea's Pop-up Crater

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of Margaritifer Terra. The linear depressions were created by extensional tectonic stresses. The nature of the white toned material is unknown at this time. Orbit Number 71991 Latitude -18.9301 Longitude 332.049 Instrument VIS Captured 2018-03-07 21 50

Over 500 new impact events have been detected from before-and-after images from NASA's Mars Reconnaissance Orbiter. This image shows new craters that expose shallow ice are of special interest.

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