RM2K5E55G–Martian landscape. This HiRISE image shows landforms on the surface of Mars. This observation was acquired to track dune gully and ripple changes in the winter season. Image taken from 254 km above the surface; terrain shown less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5EH–Martian landscape. This HiRISE image shows landforms on the surface of Mars. This is part of a steep scarp within the North Polar layered deposits. Scarps like this have the potential for active avalanches. Image taken from 319 km above the surface; terrain shown less than 10 km left to right. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5BB–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Monitoring changes among Russell Crater dunes and gullies This area is a favorite to look for changes over time. These gullies have been formed by the defrosting of carbon dioxide ice. NASA/JPL/University of Arizona (254 km above the surface, less than 5 km across) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2G7B1JY–Apollo 16 Command and Service Module Over the Moon. In this image, the Apollo 16 Command and Service Module (CSM) 'Casper' approaches the Lunar Module (LM). The two spacecraft were about to make their final rendezvous of the mission, on 23 April 1972. Astronauts John W. Young and Charles M. Duke Jr., aboard the LM, were returning to the CSM in lunar orbit after three successful days on the lunar surface. Astronaut Thomas K. Mattingly II was in the CSM. A unique optimised and enhanced version of an NASA image / credit NASA
RM2K5E4YH–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Dune Field Activity in Bonestell Crater. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6KH–Martian landscape. This HiRISE image shows landforms on the surface of Mars. These streaks indicate the prevailing direction of the Martian wind. (Note: north is to the right in this image). A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5TR–Martian landscape. This HiRISE image of the surface of Mars shows landforms that NASA scientists call 'Swiss cheese,' There seems to be an overlap of these features by thick lobes of carbon dioxide. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5N0–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Gullies in Southern Hemisphere Crater. Less than 1 km top to bottom and north is to the left.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6EB–Martian landscape. This HiRISE image shows seasonal fans on the surface of Mars. These fans are likely the result of sublimation that exposes darker subsurface material is that later blown about by the wind. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6N7–Martian landscape. This HiRISE image shows landforms on the surface of Mars. This observation captures exposed bedrock located within a very linear chain of impact craters. (North is to the right.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E574–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Elongated and Defrosting Dunes. Imaged 336 km above the surface; terrain show approximately 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4NC–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Tithonium Chasma is part of the massive Valles Marineris canyon system on Mars. It's about 810 kilometers in length. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E52F–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Exposure of layered deposits at the end of Bench in Terby Crater. (263 km above the surface, less than 5 km across) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E572–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Possible Gypsum-Rich Terrain in the Iani Chaos Region (269 km above the surface, less than 5 km across.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5EP–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Rocky ground and scarp. Imaged from 263 km above the surface; less than 5 km top to bottom; north is to the right. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4XA–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Debris Flow. There are a number of crevasse-like and arch-like features in this image with scientists looking for changes over repeat imaging. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5EB–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Exposed layers to the west of Gale Crater Imaged from 270 km above the surface; less than 5 km top to bottom; north is to the right. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E53J–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Gullies and dunes in a crater. Image taken from 251 km above the surface. Scene is 5 km top to bottom and North is to the left. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E55F–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Linear Dunes. Image taken from 322 km above the surface; terrain shown less than 1 km top to bottom; north is approximately to the left. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E591–Martian landscape. This HiRISE image shows landforms on the surface of Mars. This image is in Noachis Terra, an extensive southern landmass to the west of the Hellas impact basin. (258 km above the surface, less than 5 km across.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4PX–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Blocky Flow with Light-Toned Outcrops in the Noctis Region. This blocky flow has unusual light-toned and rounded material, along with light-toned outcrops. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E64W–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Both bright and dark fans can be seen on this patterned ground in the southern polar region of Mars. The patterns are the result of the contraction and expansion of subsurface ice. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E55C–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Seemingly etched into the surface. This terrain might be rich in hydrates.This image was taken from 317 km above the surface; terrain shown less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4NE–Martian landscape. This HiRISE image shows landforms on the surface of Mars. An Area East of Holden Crater Holden is located in the southern highlands of Mars, and is about 140 kilometers wide. (Less than 5 km top to bottom and north is to the right.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4EK–Martian landscape. This HiRISE image shows landforms on the surface of Mars. This enormous massif crosses the northern border fault in Coprates Chasma. The massif also has light toned material near its top and wallrock-like material near the bottom. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4YG–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Distinct Gullies. Images shows terrain less than 5 km (3 mi) across; imaged from analtitude of 248 km (154 miles) above the surface of Mars. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E64C–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Outcrops in Terrain East of Olympus Mons This image has perhaps one of the better justifications we've seen lately: 'Interesting rock outcrop. I want a closer look.' A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5EN–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Looking for Viscous Flow What kind of flow? Most likely ancient glacial processes. Imaged from 254 km above the surface; terrain shown less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E524–Martian landscape. This HiRISE image shows landforms on the surface of Mars. A layered deposit in a crater in the Arabia Region. NASA/JPL/University of Arizona (299 km above the surface, less than 5 km across) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E59H–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Possible Carbonate-Rich Terrain in the Northeast Syrtis Region Basin NASA/JPL/University of Arizona (279 km above the surface, less than 5 km across.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E636–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Megadunes. These dunes in Hyperborei Cavi are known as 'barchan' for their shape, which typically follows the direction of the wind. In addition, these barchan dunes indicate unidirectional flow and high sand supply. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E53R–Martian landscape. This HiRISE image shows landforms on the surface of Mars. At the Boundary of Noachian Epoch Olivine-Rich Terrain The Noachian period is roughly 4 billion years ago. Imaged from 284 km above the surface; less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E541–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Etched Terrain in Meridiani Planum. Meridiani Planum is also where the Challenger Memorial Station is located (not pictured here). Imaged from 272 km above the surface; less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5CN–Martian landscape. This HiRISE image shows landforms on the surface of Mars. A raised sinuous ridge. What process might have created this? Fluvial, glacial or perhaps volcanic? Image taken f251 km above the surface; terrain shown less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizonarom
RM2K5E4J3–Martian landscape. This HiRISE image shows landforms on the surface of Mars. A ridge near Olympus Mons. This particular ridge is located southeast of the Olympus Mons aureole, and our purpose is to take a look at the interaction between the wrinkle ridge and ancient lava flows. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5B9–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Sample of the terrain in the Southern Mid-Latitudes This area may contain ice table-related morphologies. Image taken from 251 km above the surface; terrain shown less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6TH–Martian landscape. This HiRISE image shows evidence for inverted channels and possible meanders similar to those seen in Eberswalde Crater. There are also clays in the nearby region and possibly in this location. Image is less than 5 km (3 mi) across and is 259 km (161 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E589–Martian landscape. This HiRISE image shows landforms on the surface of Mars. This (mostly) solitary crater has lots of dune ripples inside it, and is located in an area of possible olivine-rich terrain. NASA/JPL/University of Arizona (267 km above the surface, less than 5 km across.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E558–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Bedrock exposures on a crater floor in northwest Terra Cimmeria. Image taken from 264 km above the surface; terrain imaged here less than 5km top to bottom; north is to the right. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E69H–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Slopes on light-toned layered deposits. These slopes might be good candidates to study what are called 'recurring slope lineae,' which are dark flows. We don't know if these are briny or sandy flows. (Less than 5 km across.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4HT–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Here, a small crater has been cut in half by erosion and is exposed in cross section. These types of 'cut craters' provide a unique opportunity to view the subsurface geometry of impacts and also to assess erosional and landslide processes. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6N6–Martian landscape. This HiRISE image shows landforms on the surface of Mars. A perennial favourite on the list of potential landing sites, Mawrth Vallis is known for the presence of clays in addition to the beautiful topography. The valley is a channel likely formed by massive flooding in the ancient past. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E56R–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Dune Changes in Syrtis Major.This image will help document any changes of Syrtis Major dunes over time. NASA/JPL/University of Arizona (283 km above the surface, less than 5 km across) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E528–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Layered Rocks in Western Arabia Terra This region may have aqueously-altered bedrock although most of surface is now dust-covered. Image taken from 295 km above the surface. Scene is less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E512–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Dunes on the floor of Katoomba Crater, Mars. Image shows terrain 5 km (3 mi) across, taken from an altitude of 247.7 km (154.0 miles) above the surface, and north is approximately down. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4GG–Martian landscape. This HiRISE image shows pitted surface in Tartarus Montes, Mars.The objective of this observation is to determine the nature of a highly pitted surface. The wall of one pit is shared with a neighbouring pit. The heat from lava may have caused ground ice to turn to steam and form the pits. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5PN–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Scientists took this image as a follow-up to previous images to detect any recent landslide activity. This cliff is also known as a 'basal scarp' and is part of the north polar layered deposits. Image shows terrain 10-13km lengthwise. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5H1–Martian landscape. This HiRISE image shows landforms on the surface of Mars. This is a youthful-appearing fault scarp south of Arsia Mons, also imaged by the Context Camera onboard MRO. Our resolution can help us determine if the scarp is indeed (geologically) fresh, or perhaps just buried by wind-driven sediment. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E594–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Intercrater Terrain in Ophir Planum The Ophir Planum plateau separates two separate canyon systems in the Valles Marineris complex. Image taken from 260 km above the surface. Scene is 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E62X–Martian landscape. This HiRISE image shows landforms on the surface of Mars. The Mars Orbiter Camera and a single HiRISE image show some very interesting light-toned rocks and narrow ridges here. One of the reasons for this observation was to look for jointing and layering. Image shows terrain less than 5 km (3 mi) across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5ET–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Light Toned Possible Clays in Margaritifer Terra. Mapping data done by the CRISM instrument indicates that there is the presence of clay layer here. Image taken from 265 km above the surface; terrain shown less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E63G–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Multiple Branches of the Cerberus Fossae The Cerberus Fossae are a series of semi-parallel fissures on Mars formed by faults which pulled the crust apart in the Cerberus region. This image also shows some aligned pits with two fissures directly south of their location. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6H3–Martian landscape. This HiRISE image shows landforms on the surface of Mars. A Channel in Mamers Valles with Possible Clays. Mamers Valles is a long, winding canyon in the north of Mars, extending 1000 kilometers, and cuts through the cratered uplands of the Arabia Terra, to the edge of the vast northern lowlands. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E52A–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Possible Hydrated Minerals between Scylla Scopulus and Charybdis Scopulus. Scylla Scopulus is an escarpment that is located opposite to Charybdis Scopulus and runs opposite to each other. Image taken255 km above the surface; terrain shown is less than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5XR–Martian landscape. This HiRISE image shows layered bedrock northwest of Hellas Region, Mars.This image can help to complete a mosaic of the area as other adjacent images also show revealing exposures of the bedrock.This Image is less than 5 km (3 mi) across and is 255 km (158 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5KB–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Ganges Mensa, Mars. Ganges Mensa is a mesa and an interior layered deposit in Ganges Chasma, one of the peripheral valleys of Valles Marineris on Mars. The mesa rises up to 4 kilometers from the floor of Ganges Chasma. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5BR–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Knobs in West Candor Chasma. Are these possible spring mounds or liquefaction structures (meaning they resist erosion in a wet environment)? Image taken from 264 km above the surface; terrain shown less than 5 km across) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5BP–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Gullies and fissures What is the nature of these particular channels and deposits in this crater? Its eroded rim tells us that it's extremely old, and has been filled in over time with sediment. Image taken from 279 km above the surface; the terrain shown is 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4K3–Martian landscape. This HiRISE image shows landforms on the surface of Mars. A valley network along the Wallrock in Melas Chasma. There are geologically young and well-preserved valley networks and layering along this southern wall of Melas Chasma in Valles Marineris. At HiRISE resolution, it will be useful to see how these networks and layering correspond to topography. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4EM–Martian landscape. This HiRISE image shows landforms on the surface of Mars. A landslide in Claritas Fossae. This is an uncommon example of a possible landslide in Claritas Fossae. The bedrock seems to be light-toned materials, perhaps sedimentary. If this is a landslide, then stability analysis will provide insight into the strength of the light-toned material. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E523–Martian landscape. This HiRISE image shows erosional surface features in Arabia Terra, Mars. The area shows a set of trapezoid and triangular surface features that appear to differ from the surrounding area. The features may be eroded impact craters, but their proximity and alignment to each other rather suggests another geological explanation. (North is to the right.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E582–Martian landscape. This HiRISE image shows landforms on the surface of Mars. CRISM Detection of Olivine in Syrtis Major CRISM is a visible-infrared spectrometer instrument onboard the Mars Reconnaissance Orbiter. Olivine is a magnesium iron silicate. NASA/JPL/University of Arizona (281 km above the surface, less than 5 km across.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5BX–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Acidalia region slope monitoring. Some of the best documented recurring slope lineae have occurred here, so we continue to observe for possible changes and compare them to earlier images. Image taken 301 km above the surface; terrain shown less tham 5 km top to bottom; north is to the left. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6G6–Martian landscape. This HiRISE image shows landforms on the surface of Mars. The Floor of Flaugergues Crater The rocky ground here also features some inverted materials. This often indicates that the material is more resistant to erosion than the surrounding terrain. Question is: how was it deposited here? Flaugergues is about 245 kilometers in diameter and was named after Honore Flaugergues, a French astronomer (1755-1835). A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6X9–Martian landscape. This HiRISE image shows landforms on the floor of East Candor Chasma. These folding and deformational structures within the layered deposits in east Candor Chasma will be terrific for a structural analysis with a digital terrain model. Image is less than 5 km (3 mi) across and is 266 km (165 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6P0–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Here, an impact crater on the northeast rim of Hellas basin, with excellent exposures of bedrock layers. Here we can see a portion of the steep inner slope where some of the bedrock has broken into angular pieces and slide partway down the slope. Image shows terrain less than 5 km (3 mi) across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E522–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Aluminum Hydroxide on a Crater Floor in the Sirenum Region The aluminum hydroxide (also known as the mineral gibbsite) is visible with the CRISM instrument (a spectrometer.) Taken from 259 km above the surface; terrain shown less than 5 km top to bottom; north is to the right. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5F9–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Chaos Terrain. Chaos terrain on Mars is distinctive; nothing on Earth compares to it. Chaos terrain generally consists of irregular groups of large blocks, some tens of kilometers across and a hundred or more meters high. The tilted and flat topped blocks form depressions hundreds of metres deep. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E50T–Martian landscape. This HiRISE image shows landforms on the surface of Mars.Dust Devils of Mars- swirls on sand dunes created by dust devils that expose the darker subsurface. The scene is located in the centre of an ancient impact crater to the west of the Isidis basin in the Northern Hemisphere of Mars. Terrain shown is less than 5 km (3 mi) across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E53H–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Aram Chaos, located at the eastern end of the large canyon Valles Marineris and close to Ares Vallis. Various geological processes have reduced it to a circular area of chaotic terrain. Imaged from 274 km above the surface; terrain shown less than 5 km top to bottom; north is to the right. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6TX–Martian landscape. This HiRISE image shows landforms in the area between Crommelin and Firsoff craters, we see heavily cratered terrain with deposits that record Martian geologic history and stratigraphy.With HiRISE resolution, we might be able to decipher what materials are in the ridges of the inverted channels in this region and what the flows are: lava or sediment?Image is less than 5 km (3 mi) across and is 272 km (169 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4GH–Martian landscape. This HiRISE image a pit on Arsia MonsWe acquired this image to determine if any underlying void (an open fracture, for example) and associated faults can be observed. Pits may reflect geologically-recent tectonic or volcanic activity. Any associated caves could be targets for future robotic exploration. Image is less than 5 km (3 mi) across and is 251 km (156 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5XC–Martian landscape. This HiRISE image shows landforms on the surface of Mars. The objective of this observation was to examine layered features near a group of mounds in the northern mid-latitudes of Mars. We can also see that the impact craters here have long been filled-in with sediment. This image shows terrain less than 5 km (3 mi) across and was taken from 298 km (185 mi) above the surface of Mars.A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4W6–Martian landscape. This HiRISE image of Mars shows dark spots that are the result of sublimation, when ice under the surface gets heated and turns directly into a gas. This exposes darker material that looks like dark spots. Over time, even these will fade, but newer spots will appear. The ice here is made of carbon dioxide. Image is less than 5 km (3 mi) across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E60J–Martian landscape. This HiRISE image shows landforms on the surface of Mars.This impact crater in the Nilosyrtis region of Mars contains numerous layers exposed along its floor. These layers formed long after the impact event and are likely deposits of dust and ice. Also present are dunes of dark sand that probably blew in from the surrounding terrain. Image shows terrain less than 5km [3 mi] across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4XD–Martian landscape. This HiRISE image shows landforms on the surface of Mars.Debris flows. The purpose of this observation was to get more coverage of the debris flows on the walls of Eos Chasma, which is in the southern part of the Valles Marineris canyon system. Image shows terrain less than 5 km (3 mi) across, taken from an altitude of 264 km (164 mi) above the surface of Mars. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4RE–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Channels in Phlegra Montes. Also visible in a Context Camera image, pictures like this can help us understand the fluvial and climate history of ancient Mars. Image shows terrain less than 5 km (3 mi) across; taken 296 km (184 mi) above the surface of Mars. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E625–Martian landscape. This HiRISE image shows landforms on the surface of Mars.Light-Toned Deposits in Noctis Labyrinthus. CRISM observations of this region of the Noctis Labyrinthus formation have shown indications of iron-bearing sulfates and phyllosilicate (clay) minerals. (CRISM is another instrument on the Mars Reconnaissance Orbiter.) Image is less than 5 km (3 mi) across and is 253 km (157 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E55E–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Possible Clay-Rich Terrain on the Edge of Rutherford Crater This crater, located within Arabia Terra, is 107 km in diameter, and is named after British physicist Ernest Rutherford in 1973. Image taken from 283 km above the surface; terrain shown ess than 5 km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4YN–Martian landscape. This HiRISE image shows landforms on the surface of Mars.Diverse exposures of bedrock associated with massifs outside Hellas Planitia. This observation was made to help determine the origins of the diverse materials exposed in a number of massifs associated with the Hellas impact basin. This image shows terrain less than 1 km (under a mile) from top to bottom. North is to the right. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4K4–Martian landscape. This HiRISE image shows a terraced fan in the east Candor Chasma, Mars. This is an interesting area, located adjacent to the massive Valles Marineris canyon system. There is possible soft sediment deformation of lake-related sediment, which can help with geologic mapping. Image is less than 5 km (3 mi) across and is 264 km (164 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2TJC9FE–Bisected Crater, Mars. This impact crater is cut by a fracture that is part of the Cerberus Fossae. The exposure of stratigraphy in the crater walls coupled with the exposure of stratigraphy in the fracture may shed light on the nature of near-surface stratigraphic units at this location. The fracture also cuts young lavas. It is not clear whether the crater or the lavas are older. Image shows terrain less than 5km. A unique optimised version of NASA HIRISE imagery. Credit: NASA/JPL/UArizonaMartian landscape.
RM2K5E6RN–Martian landscape. This image was taken to observe bedrock exposures in a crater wall in the Acidalia region of Mars. Other nearby pictures showed bedrock that is at least 1,000 meters thick, with hints of columnar jointing. Our goal is to analyse in detail the layering and joint patterns that would help determine the nature of the bedrock. Image is less than 5 km (3 mi) across and is 303 km (188 mi) above the surface. An unique optimised version of an original NASA image. Credit: NASA
RM2K5E5PB–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Libya Montes are a highland terrain on Mars that were formed by the giant impact that created the Isidis basin to the north. This area contains some of the oldest rocks on the Martian surface. The terrain was subsequently transformed by a number of different processes, including fluvial activity, wind erosion and other impact cratering. Image shows terrain less than 5km across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4X9–Martian landscape. This HiRISE image shows a central peak surrounded by a ring-like graben feature and relatively flat terrain. Does the graben show evidence of what geologists call 'differential compaction?' Compaction refers to sediment that is originally porous and is covered up by other sediment (called 'loading') that reduces that porousness. Differential compaction is when there is variation in the thickness of a given area that creates uneven surface and has different degrees of porosity A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4W3–Martian landscape. This HiRISE image shows landforms on the surface of Mars. This image shows part of a depression with terraced margins, located to the northwest of Nicholson Crater. This crater is about 100 kilometers wide, and sits almost directly on the Martian equator. It is named after Seth Barnes Nicholson, an American astronomer. NASA/JPL/University of Arizona (273 km above the surface, less than 5 km top to bottom and north is to the right.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E573–Martian landscape. This HiRISE image shows landforms on the surface of Mars. Floor of a Degraded Crater in Terra Cimmeria Terra Cimmeria is one part of the heavily cratered, southern highland region of the planet. The Spirit rover landed near the area. The word 'Cimmerium' comes from an ancient Thracian seafaring people. (256 km above the surface, less than 5 km top to bottom and north is to the right.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4HX–Martian landscape. This HiRISE image shows landforms on the surface of Mars. A Small Crater with Possible Olivine Deposits. This is the southern edge of a very eroded and almost filled-in impact crater. Olivine is an olive-green, gray-green, or brown mineral occurring widely in basalt, peridotite, and other basic igneous rocks. (261 km above the surface, less than 5 km top to bottom and north is to the right.) A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5KA–Martian landscape. This HiRISE image shows flows from the CentralPeak of Moreux Crater with large ridges extending down off of the central mountains.What made those flows? It doesn't look like lava, and the central mountains are not volcanoesÑthey were thrust up by the impact event. Instead, it may be that these were flows of ice, or glaciers. There are lots of boulders on the surface, and glaciers tend to carry lots of rocks. Image is less than 5 km (3 mi) across A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E5KD–Martian landscape. This HiRISE image shows landforms on the surface of Mars.Faults in Granicus. This stunning shows off the results of faults in Granicus and Tinjar Valles.. Granicus Valles are a network of valleys, probably outflow channels, that are 750km in length and located west of Elysium Mons. Both water and lava may have played a role in its formation. This image shows terrain less than 5 km (3 mi) across A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6H1–Martian landscape. This HiRISE image shows landforms on the surface of Mars.Mesa in Southwest Nili Fossae. Images from other spacecraft missions show that this mesa is mix of diverse lithology, probably stemming from the early Noachian epoch on Mars, about 3.7 to 4 billion years ago. (The absolute age of the Noachian age remains uncertain.) Image shows terrain less than 5 km (3 mi) across A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4GF–Martian landscape. This HiRISE image shows a possible chloride deposit in Bosporos Planum.On Earth, chlorides form from aqueous processes, so similar processes are expected to be responsible for the formation of chloride deposits on Mars. The finding of these deposits is significant in that it provides further evidence for the presence of surface or subsurface water in the ancient Martian past.Image is less than 5 km (3 mi) across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4CE–Martian landscape. This HiRISE image shows landforms on the surface of Mars.A Floor-Fractured Crater in Elysium Planitia. Scientists believe this fracturing might be related to invasive lava, as it resembles tilted-facet terrain elsewhere on Mars. With another observation to help create an anaglyph, we can take a look at the outside terrain and see how the elevations compare. Image shows terrain less than 5 km (3 mi). A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6PF–Martian landscape.Near the centre of this image, there is a large angular fragment that appears to have light and dark-toned bands.Nili Fossae was once considered a potential landing spot for the Mars Science Laboratory, and has one of the largest, most diverse exposures of clay minerals. Clay minerals contain water in their mineral structure and may preserve organic materials. Image is less than 5 km (3 mi) across and is 279 km (174 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6PG–Martian landscape. This HiRISE image shows a fresh, 2-kilometer diameter crater on the floor of the much larger Pasteur Crater. Within the crater, that still has a fairly sharp rim, is a dark patch of sand interestingly located in one area only instead of being spread out. Has some of it blown in from the surrounding terrain?Image is less than 5 km (3 mi) across and is 284 km (176 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6RP–Martian landscape. This HiRISE image shows channels from Hale Crater, up to c.250m (820ft) across, though most are much smaller. The channels appear to emanate directly from Hale Crater's ejecta, and were likely formed by the impact event. The heat of the impact could have melted large amounts of subsurface ice, and generated surface runoff capable of carving the channels. Channels associated with impact craters were once thought to be quite rare.Image is less than 5km (3 mi) across. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E4R0–Martian landscape. This HiRISE image shows a mixture of bright & dark terrain along the plains west of Ganges Chasma, Mars. The concentration of these bright patches adjacent to an old impact crater suggests that the bright patches could be ejecta from when the crater formed. This would be an interesting discovery because it would mean that a different unit underlies the surface we now see. Or, this darker debris has been removed by the wind, exposing underlying brighter substrate. Image shows terrain less than 5km across A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E6N8–Martian landscape. This HiRISE image shows valleys north of Huygens Crater, Mars.This observation covers an area of northeastern rim of Huygens with valleys visible in Context Camera, Viking, and THEMIS data, but no HiRISE coverage to enable high resolution analysis. A small valley appears to be inverted/transition into a ridge as it extends out onto the crater floor. Image is less than 5 km across and is 284 km (177 mi) above the surface. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E67K–Martian landscape. This HiRISE image shows part of the Athabasca Valles flood lava plain, the youngest large lava flow on the surface of Mars. At this location, there are two rafted pieces of lava crust with strange infrared properties. Compared to the rest of the lava flow, these two raised areas are cold at night and warm in the day. This property of the surface, where the temperature changes quickly, is called 'low thermal inertia.' Rocks tend to have relatively high thermal inertia, so this is unexpected. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
RM2K5E60G–Martian landscape. This HiRISE image shows layers, dunes and cliffs in Hydrae Chasma, a deep, circular depression approximately 50 km across, situated between Juventae Chasma to the north and the large canyon system Valles Marineris to the south. The chasma has steep walls flanked by numerous landslides and a massive scarp along its southern boundary where the surface has collapsed into this depression. Image shows terrain less than 1 km (under a mile) top to bottom. A unique optimised version of NASA imagery. Credit: NASA/JPL/UArizona
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