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Gullies are visible in this image of the northern rim of Holden Crater as seen by NASA's 2001 Mars Odyssey spacecraft. | Context imageGullies are visible in this VIS image of the northern rim of Holden Crater.Orbit Number: 43631 Latitude: -24.5308 Longitude: 326.128 Instrument: VIS Captured: 2011-10-15 19:38Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Orbiter Camera (MOC) took this image on August 20, 1997, when the Mars Global Surveyor (MGS) was 5.67 million kilometers (3.52 million miles) and 22 days from entering orbit. | The Mars Orbiter Camera (MOC) took this image on August 20, 1997, when the Mars Global Surveyor (MGS) was 5.67 million kilometers (3.52 million miles) and 22 days from entering orbit. At this distance, the MOC's resolution is about 21.2 km per picture element, and the 6800 km (4200 mile) diameter planet is about 327 pixels across. North is at the top of the image. The MGS spacecraft pointed the camera at the center of the planet (near the dark, morning sunrise line, or terminator) at 23.6° N, 82.1° W. At this distance from Mars, only bright and dark markings resulting from variations in the amount and thickness of dust and sand are visible. The large dark marking stretching from the right center northward is Acidalia Planitia, a region of rock and sand with less dust on it than the area immediately to the south, Chryse Planitia. Both Viking Lander 1 and Pathfinder landed in the latter, bright area. In this low resolution image, some of the dark features resemble the "canals" seen prominently in maps created by astronomers of the 19th and early 20th century. Mariner 9 and Viking images show that most of these dark lines are associated with sand deposits that are trapped in rough areas.Mars Global Surveyor was launched on November 7, 1996 and will enter Mars orbit on Thursday, September 11 around 6:30 PM PDT. The spacecraft will use atmospheric drag to reduce the size of its orbit. Mapping operations will begin in March 1998.The MOC on MGS is a spare camera originally developed for the ill-fated Mars Observer mission. Malin Space Science Systems and the California Institute of Technology were responsible for development of both cameras. MSSS operates the MOC from its facilities in San Diego, CA, under contract to the Jet Propulsion Laboratory. | |
This figure shows the location of CHIMRA on the turret of NASA's Curiosity rover, together with a cutaway view of the device. CHIMRA processes samples from the rover's scoop or drill and delivers them to science instruments. | This figure shows the location of CHIMRA on the turret of NASA's Curiosity rover, together with a cutaway view of the device. The CHIMRA, short for Collection and Handling for In-situ Martian Rock Analysis, processes samples from the rover's scoop or drill and delivers them to science instruments.The green highlighted surface shows the location of the 150-micrometer sieve through which samples are passed (a human hair is about 100 micrometers, or microns, thick on average). In addition, the pink line shows the path from the drill to the "portion box" used to deliver the sieved particles to the Sample Analysis at Mars (SAM) and Chemistry and Mineralogy (CheMin) instruments. JPL, a division of the California Institute of Technology, Pasadena, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the rover. More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
NASA's Mars Global Surveyor shows a scene in southern Galle Crater on Mars, otherwise known as Happy Face Crater. A series of dark sand dunes have been crisscrossed by dust devils. | 26 July 2004This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a scene in southern Galle Crater, otherwise known as Happy Face Crater. At the north end of the image (toward top, center) is a gully that formed on a slope. At the south end (bottom) is a series of dark sand dunes that have been crisscrossed by dust devils. The dust devils left behind tell-tale streaks. This image is located near 51.9°S, 31.6°W, and is illuminated by sunlight from the upper left. The image covers an area about 3 km (1.9 mi) wide. | |
This image captured by NASA's 2001 Mars Odyssey spacecraft shows martian terrain which could resemble Mickey Mouse's head. | Context imageDo you see what I see? Poor Mickey Mouse, only his head remains at the bottom of this VIS image.Orbit Number: 39927 Latitude: -6.9821 Longitude: 255.372 Instrument: VIS Captured: 2010-12-14 20:03 Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This cylindrical-projection mosaic was created from navigation camera images that NASA's Mars Exploration Rover Spirit acquired on sol 100 (April 14, 2004). It reveals Spirit's view after a century of sols on the martian surface. | This cylindrical-projection mosaic was created from navigation camera images that NASA's Mars Exploration Rover Spirit acquired on sol 100 (April 14, 2004). It reveals Spirit's view after a century of sols on the martian surface. | |
This NASA Mars Global Surveyor image shows ancient, dust-covered lava flows and remains of leveed lava channels located on a plain northwest of Jovis Tholus. Jovis is a relatively small volcano in the Tharsis region of Mars. | 4 May 2006This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows ancient, dust-covered lava flows and remains of leveed lava channels located on a plain northwest of Jovis Tholus. Jovis is a relatively small volcano in the Tharsis region of Mars.Location near: 22.4°N, 122.0°W Image width: ~3 km (~1.9 mi) Illumination from: lower left Season: Northern Winter | |
An elongated crater called 'Spirit of St. Louis,' with a rock spire in it, dominates a recent scene from the panoramic camera (Pancam) on NASA's Mars Exploration Rover Opportunity. | An elongated crater called "Spirit of St. Louis," with a rock spire in it, dominates a recent scene from the panoramic camera (Pancam) on NASA's Mars Exploration Rover Opportunity.Opportunity completed its 4,000 Martian day, or sol, of work on Mars on April 26, 2015. The rover has been exploring Mars since early 2004.This scene from late March 2015 shows a shallow crater called Spirit of St. Louis, about 110 feet (34 meters) long and about 80 feet (24 meters) wide, with a floor slightly darker than surrounding terrain. The rocky feature toward the far end of the crater is about 7 to 10 feet (2 to 3 meters) tall, rising higher than the crater's rim.The component images of this mosaic view were taken on March 29 and 30, 2015, during Sol 3973 and Sol 3974 of the mission. This version of the image is presented in approximate true color by combing exposures taken through three of the Pancam's color filters, centered on wavelengths of 753 nanometers (near-infrared), 535 nanometers (green) and 432 nanometers (violet).The view is centered toward the northeast. The rover's location and the Spirit of Saint Louis Crater are near the center of a map at http://mars.nasa.gov/mer/mission/tm-opportunity/images/MERB_Sol3998_1.jpg.The unusually shaped Spirit of St. Louis Crater lies on the outer portion of the western rim of Endeavour Crater. Endeavour spans about 14 miles (22 kilometers) in diameter, and Opportunity has been exploring its western rim for about one-third of the rover's mission, which has lasted more than 11 years. Endeavour's elevated western rim extends northward to the left from Spirit of St. Louis Crater in this scene. A glimpse to the far side of Endeavour is visible on either side of the rock spire.JPL manages the Mars Exploration Rover Project for NASA's Science Mission Directorate in Washington. For more information about Opportunity's mission, visit http://mars.nasa.gov/mer. | |
This image mosaic from NASA's Mars Exploration Rover Opportunity shows detailed structure of a small fin-like structure dubbed 'Roosevelt,' which sticks out from the outcrop pavement at the edge of 'Erebus Crater,' taken on Feb. 8, 2006. | This image mosaic from the microscopic imager aboard NASA's Mars Exploration Rover Opportunity shows detailed structure of a small fin-like structure dubbed "Roosevelt," which sticks out from the outcrop pavement at the edge of "Erebus Crater."Roosevelt lines a fracture in the local pavement and scientists hypothesize that it is a fracture fill, formed by water that percolated through the fracture. This would mean the feature is younger than surrounding rocks and, therefore, might provide evidence of water that was present some time after the formation of Meridiani Planum sedimentary rocks. The image shows fine laminations (layers about 1 millimeter or .04 inch thick) that run parallel to the axis of the fin. Some of the textures visible in the image likely indicate that minerals precipitated from the outcrop rocks, but sediment grains are also apparent. The three frames combined into this mosaic were taken during Opportunity's 727th Martian day, or sol (Feb. 8, 2006). In subsequent days, the rover completed textural and chemical inspection of Roosevelt to help the science team understand this structure's significance for Martian history. | |
NASA's Ingenuity helicopter does a slow spin test of its blades, on April 8, 2021. This image was captured by the Navigation Cameras on NASA's Perseverance Mars rover. | Click here for animationNASA's Ingenuity helicopter does a slow spin test of its blades on April 8, 2021, the 48th Martian day, or sol, of the mission. This image was captured by the Navigation Cameras on NASA's Perseverance Mars rover.A key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith (broken rock and dust).Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.The Mars 2020 Perseverance mission is part of NASA's Moon to Mars exploration approach, which includes Artemis missions to the Moon that will help prepare for human exploration of the Red Planet.JPL, which is managed for NASA by Caltech in Pasadena, California, built and manages operations of the Perseverance rover.For more about Perseverance: mars.nasa.gov/mars2020/ and nasa.gov/perseverance | |
This image of the rock 'Flat Top' was taken from one of NASA's Sojourner rover's front cameras on Sol 42. Sol 1 began on July 4, 1997. | This image of the rock "Flat Top" was taken from one of the Sojourner rover's front cameras on Sol 42. Pits on the edge of the rock and a fluted surface are clearly visible. The rocks in the left background comprise the Rock Garden.Mars Pathfinder is the second in NASA's Discovery program of low-cost spacecraft with highly focused science goals. The Jet Propulsion Laboratory, Pasadena, CA, developed and manages the Mars Pathfinder mission for NASA's Office of Space Science, Washington, D.C. JPL is a division of the California Institute of Technology (Caltech).
Photojournal note: Sojourner spent 83 days of a planned seven-day mission exploring the Martian terrain, acquiring images, and taking chemical, atmospheric and other measurements. The final data transmission received from Pathfinder was at 10:23 UTC on September 27, 1997. Although mission managers tried to restore full communications during the following five months, the successful mission was terminated on March 10, 1998. | |
This image taken on Jan. 6, 2005 by NASA's Mars Exploration Rover Opportunity highlights the seal on the rover's protective heat shield. Engineers evaluated the performance of the protective shell's seal during a 36-sol investigation. | This image from NASA's Mars Exploration Rover Opportunity highlights the seal on the rover's protective heat shield. Engineers evaluated the performance of the protective shell's seal during a 36-sol investigation.After viewing these images, engineers were pleased with how the seal performed.This is an approximately true-color rendering of the scene acquired around 1:07 p.m. local solar time on Opportunity's sol 339 (Jan. 6, 2005) in an image mosaic using panoramic camera filters at wavelengths of 750, 530, and 430 nanometers. | |
These channels and channel-like collapse features are located on the northeastern flank of Ascraeus Mons on Mars as seen by NASA's Mars Odyssey spacecraft. | Context image for PIA09046Ascraeus MonsThese channels and channel-like collapse features are located on the northeastern flank of Ascraeus Mons.Image information: VIS instrument. Latitude 14.5N, Longitude 257.3E. 18 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
View from Spirit's Overwintering Position (False Color) | NASA's Mars Exploration Rover Spirit has this view northward from the position at the north edge of the "Home Plate" plateau where the rover will spend its third Martian winter. Husband Hill is on the horizon. The dark area in the middle distance is "El Dorado" sand dune field.Spirit used its panoramic camera (Pancam) to capture this image during the rover's 1,448th Martian day, of sol (Jan. 29, 2008).This view combines separate images taken through the Pancam filters centered on wavelengths of 753 nanometers, 535 nanometers and 432 nanometers. It is presented in a false-color stretch to bring out subtle color differences in the scene. | |
This observation from NASA's Mars Reconnaissance Orbiter shows it is late summer in the Southern hemisphere, so the Sun is low in the sky and subtle topography is accentuated in orbital images. | Map Projected Browse ImageClick on the image for larger versionThis observation from NASA's Mars Reconnaissance Orbiter show it is late summer in the Southern hemisphere, so the Sun is low in the sky and subtle topography is accentuated in orbital images.We see many shallow pits in the bright residual cap of carbon dioxide ice (also called "Swiss cheese terrain"). There is also a deeper, circular formation that penetrates through the ice and dust. This might be an impact crater or it could be a collapse pit.This is a stereo pair with ESP_049945_0930.The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 49.7 centimeters (19.6 inches) per pixel (with 2 x 2 binning); objects on the order of 149 centimeters (67.3 inches) across are resolved.] North is up.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
This anaglyph, acquired by NASA's Phoenix Lander on Jun. 26, 2008, shows a stereoscopic 3D view of the Martian surface near the lander. 3D glasses are necessary to view this image. | This anaglyph, acquired by NASA's Phoenix Lander's Surface Stereo Imager on Sol 31, the 31st Martian day of the mission (June 26, 2008), shows a stereoscopic 3D view of the Martian surface near the lander.The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.Photojournal Note: As planned, the Phoenix lander, which landed May 25, 2008 23:53 UTC, ended communications in November 2008, about six months after landing, when its solar panels ceased operating in the dark Martian winter. | |
This image from NASA's Mars Odyssey shows Mangala Valles, a complex channel more than 900km long (560 miles). | Context imageMangala Valles is a complex channel more than 900km long (560 miles). The channel system starts near Mangala Fossae, a large tectonic feature that intersects the volcanic plains of Daedalia Planum. Like other channels in the region, Mangala Valles flows northward, eventually emptying into southern Amazonis Planitia.Orbit Number: 79256 Latitude: -5.93824 Longitude: 209.388 Instrument: VIS Captured: 2019-10-27 06:08Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This is a portion of the first color image captured by the panoramic camera onboard NASA's Mars Exploration Rover Spirit. taken in 2004. | This is a portion of the first color image captured by the panoramic camera on the Mars Exploration Rover Spirit. | |
Layered Mesa in Coprates Chasma | Click on image for larger versionThis HiRISE image (PSP_002036_1655) shows a mesa within Coprates Chasma, a large trough in the Valles Marineris canyon system. Multiple layers, some only a few meters in thickness, are visible on the slopes descending from the edges of the flat-topped mesa. The layered rocks could have formed from volcanic, lacustrine, or aeolian sediments that were deposited in portions of the Valles Marineris trough. Variations in the brightness of the layers may represent compositional differences. In particular, the slopes contain a prominent layer of dark material that is seemingly composed of materials more resistant to erosion than the overlying brighter layers. Dunes and ripples can also visible on the top of the mesa. Observation Toolbox Acquisition date: 1 January 2007Local Mars time: 3:40 PMDegrees latitude (centered): -14.4°Degrees longitude (East): 304.2°Range to target site: 258.8 km (161.7 miles)Original image scale range: from 25.9 cm/pixel (with 1 x 1 binning) to 51.8 cm/pixel (with 2 x 2 binning)Map-projected scale: 25 cm/pixel and north is upMap-projection: EQUIRECTANGULAREmission angle: 2.3°Phase angle: 61.4°Solar incidence angle: 59°, with the Sun about 31° above the horizonSolar longitude: 160.0°, Northern SummerNASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. | |
Gullies and Dunes in a Crater in Newton Basin | Click on image for larger versionThis HiRISE image (PSP_003464_1380) is a spectacular image showing gullies associated with distinct layers located at multiple elevations along one crater wall as well as multiple generations of dunes that are eroding or covering a more coherent rock structure. The gullies in this crater appear to originate at the layers that cover a large extent of the slope. On the left side of the image, gullies can be seen emanating from layers in two distinct sets, each at a different elevation. Gullies are often, but not always, form near layers. Many of the gullies seen here have sinuous, or wavy, channels. The bends are called meanders, and on Earth, meanders form in streams that have sustained and/or repeated flow. Not all of the gullies seen in this image extend the same distance downslope. This could result from differences in water supply, sediment supply, slope angle, and time of formation, among other factors.Dunes are also visible in this image; they indicate the prevailing wind direction. What is particularly interesting about this dune field is that there is exposed rock in the middle of it. This rock is either being exposed as the wind moves the dunes away from it or it is being covered. The dunes appear to outline the shape of the rock, which suggests that the rock has been uncovered long enough for dunes to form around it. As the dunes shift over time, they will probably expose more of the underlying rock. The subimage (~1 km across) shows several generations of dunes interacting with the protruding rock.Observation Toolbox Acquisition date: 4 April 2007Local Mars time: 3:40 PMDegrees latitude (centered): -41.5°Degrees longitude (East): 202.1°Range to target site: 254.3 km (158.9 miles)Original image scale range: 50.9 cm/pixel (with 2 x 2 binning) so objects ~153 cm across are resolvedMap-projected scale: 50 cm/pixel and north is upMap-projection: EQUIRECTANGULAREmission angle: 2.2°Phase angle: 54.8°Solar incidence angle: 53°, with the Sun about 37° above the horizonSolar longitude: 224.5°, Northern AutumnNASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. | |
This image from NASA's Mars Odyssey shows two segments of the channel system called Granicus Valles. | Context imageThis VIS image shows two segments of the channel system called Granicus Valles. Granicus Valles is a complex channel system located west of Elysium Mons. The system is approximately 750km (466 miles) long. It is likely that both water and lava played a part in creation of this feature.Orbit Number: 85635 Latitude: 24.8871 Longitude: 137.814 Instrument: VIS Captured: 2021-04-04 12:00Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's 2001 Mars Odyssey shows a lava flow that topped the rim of an impact crater and flowed down to the floor of the crater. | Context imageThis VIS image in the Tharsis region shows a lava flow that topped the rim of an impact crater and flowed down to the floor of the crater.Orbit Number: 36520 Latitude: 17.7889 Longitude: 238.986 Instrument: VIS Captured: 2010-03-09 09:43Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows a portion of Cyane Sulci. Located to the northeast of Olympus Mons, Cyane Sulci is a complexly fractured region of material inundated on its margins by volcanic flows. | Context imageToday's VIS image shows a portion of Cyane Sulci. Located to the northeast of Olympus Mons, Cyane Sulci is a complexly fractured region of material inundated on its margins by volcanic flows.Orbit Number: 93905 Latitude: 23.0568 Longitude: 233.41 Instrument: VIS Captured: 2023-02-14 10:45Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
As NASA's Phoenix Mars Lander excavates trenches, it also builds piles with most of the material scooped from the holes. The piles, like this one called 'Caterpillar,' provide researchers some information about the soil. 3D glasses are necessary. | As NASA's Phoenix Mars Lander excavates trenches, it also builds piles with most of the material scooped from the holes. The piles, like this one called "Caterpillar," provide researchers some information about the soil.On Aug. 24, 2008, during the late afternoon of the 88th Martian day after landing, Phoenix's Surface Stereo Imager took separate exposures through its left eye and right eye that have been combined into this stereo view. The image appears three dimensional when seen through red-blue glasses.This conical pile of soil is about 10 centimeters (4 inches) tall. The sources of material that the robotic arm has dropped onto the Caterpillar pile have included the "Dodo" and ""Upper Cupboard" trenches and, more recently, the deeper "Stone Soup" trench.Observations of the pile provide information, such as the slope of the cone and the textures of the soil, that helps scientists understand properties of material excavated from the trenches.For the Stone Soup trench in particular, which is about 18 centimeters (7 inches) deep, the bottom of the trench is in shadow and more difficult to observe than other trenches that Phoenix has dug. The Phoenix team obtained spectral clues about the composition of material from the bottom of Stone Soup by photographing Caterpillar through 15 different filters of the Surface Stereo Imager when the pile was covered in freshly excavated material from the trench.The spectral observation did not produce any sign of water-ice, just typical soil for the site. However, the bigger clumps do show a platy texture that could be consistent with elevated concentration of salts in the soil from deep in Stone Soup. The team chose that location as the source for a soil sample to be analyzed in the lander's wet chemistry laboratory, which can identify soluble salts in the soil.The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.Photojournal Note: As planned, the Phoenix lander, which landed May 25, 2008 23:53 UTC, ended communications in November 2008, about six months after landing, when its solar panels ceased operating in the dark Martian winter. | |
This view taken from orbit shows a cluster of small, steep-sided knobs called 'Murray Buttes,' in tribute to Bruce Murray (1931-2013), an influential advocate for planetary exploration. | This view taken from orbit shows a cluster of small, steep-sided knobs called "Murray Buttes," on the planned route for NASA's Mars rover Curiosity to reach the slopes of Mount Sharp. The scene covers a patch of ground about 0.8 mile (1.3 kilometers) across. North is up. The largest buttes in the group are about the size of a football field and the height of a goal post. Darker ground at upper right and lower left is part of sand dunes along the northern edge of Mount Sharp, within Gale Crater. Murray Buttes is located at a gap in that band of dunes, making passage through this area an attractive access route to the mountain slopes just south of this scene.Curiosity's science team chose the informal name Murray Buttes in tribute to Bruce Murray (1931-2013), an influential advocate for planetary exploration who was a member of the science teams for NASA's earliest missions to Mars and later served as director of NASA's Jet Propulsion Laboratory.The image is a portion of an observation made by the High Resolution Imaging Science Experiment (HiRISE) camera aboard NASA's Mars Reconnaissance Orbiter. A scale bar of 100 meters (328 feet) is provided at lower left. | |
NASA's Mars Global Surveyor shows layered material in west Arabia Terra crater on Mars. | Hundreds of layers of similar thickness, texture, and pattern have been exposed by erosion in a 64 kilometer-wide (40 mile-wide) impact crater in western Arabia Terra at 8°N, 7°W. In other words, these layers provide a record of repeated, episodic changes that took place at some time far in the martian past, when this particular impact crater was the site of sediment deposition. Layers toward the center of the crater are nearly horizontal, but those closer to or draping over the crater walls are tilted (geologist use the term dipping) toward the basin center. These relationships suggest that the sediments that created these layers were deposited from above--perhaps by settling out of the martian atmosphere, or perhaps by settling out of water that might have occupied this crater as a lake.The context view (above) was taken by the Viking 1 orbiter in 1978; in it, north is up and sunlight illuminates the scene from the right. The three Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) narrow angle (high resolution) views (PIA02840, PIA02841, PIA02842) sample layer outcrops that were previously not known to exist in this crater. Each MOC image is illuminated from the left. Dark material in PIA02841 and PIA02840 (this release) is windblown sand; in PIA02840 (this release), this sand enhances the appearance of the layers.Note: In the context image above, the boxes marked A, B, and C refer to PIA02842, PIA02841, and PIA02840 (this release) respectively. | |
North Polar Layers, Mars | This view shows the basal layers of Mars' north polar layered deposits. The floor of Chasma Boreale is at the bottom of the image. This is a sub-image of a larger view imaged by the High Resolution Imaging Science Experiment (HiRISE) on NASA's Mars Reconnaissance Orbiter on Oct. 1, 2006. The resolution is 64 centimeters (25 inches) per pixel, and the scene is 568 meters (621 yards) wide. | |
NASA's Perseverance rover captured this portrait of its recently completed sample depot using its Mastcam-Z camera on Jan. 31, 2023. Containing 10 samples, the depot is a crucial milestone in the NASA-ESA Mars Sample Return campaign. | Figure AFigure BFigure CClick on images for larger versions
Main image - full resolution download, (1.03 GB)
Figure A image - full resolution download, (1.03 GB)
Figure B image - full resolution download, (1.18 GB)
Figure C image - full resolution download, (1.17 GB)NASA's Perseverance Mars rover captured this portrait of its recently completed sample depot using its Mastcam-Z camera on Jan. 31, 2023, the 693rd Martian day, or sol, of the mission. This panorama is made up of 368 individual images that were stitched together after being sent back to Earth. The color in the scene has been adjusted to show the Martian surface as it would look to the human eye.Each sample tube is approximately 7 inches (18 centimeters) long and .8 inches (2 centimeters) in diameter.The "Amalik" sample closest to the rover was approximately 10 feet (3 meters) away from the camera at the time the image was taken. The "Atsah" and "Skyland" samples were approximately 66 feet (20 meters) away. "Bearwallow," "Coulettes," "Montdenier," "Crosswind Lake," and "Roubion" were approximately 115 to 164 feet (35 to 50 meters) away. "Mageik" and "Malay" were approximately 197 feet (60 meters) away.This is a natural-color view of the scene, showing the surface as it would appear to a human observer. Figure A is the same natural-color version annotated with the names of each of the samples in the depot.Figure B is an enhanced-color version of the scene; the color bands of the image have been processed to improve visual contrast and accentuate color differences. Figure C is the same enhanced-color version annotated with the names of each of the samples in the depot.Throughout its science campaigns, the rover has been taking a pair of samples from rocks the mission team deems scientifically significant. One sample from each pair taken so far now sits in the depot – along with one atmospheric sample and one "witness" tube – for a total of 10 tubes that were carefully arranged on the surface in a zigzag pattern.The depot is a crucial milestone in the NASA-ESA (European Space Agency) Mars Sample Return campaign, which aims to bring Mars samples to Earth for closer study. The Perseverance rover will be the primary means to hand off the collected samples to a future robotic lander as part of the campaign. The lander would, in turn, use a robotic arm to place the samples in a containment capsule aboard a small rocket that would blast off to Mars orbit, where another spacecraft would capture the sample container and return it safely to Earth. Hosting a duplicate set, the depot will serve as a backup if Perseverance can't deliver its samples.Perseverance built the depot at "Three Forks," a location within Mars' Jezero Crater. Billions of years ago, this crater was filled by a lake and delta. Sediment that built up in the delta formed a steep mound that Perseverance will be driving up in the months ahead to arrive at the top of the delta.Arizona State University leads the operations of the Mastcam-Z instrument, working in collaboration with Malin Space Science Systems in San Diego, on the design, fabrication, testing, and operation of the cameras, and in collaboration with the Neils Bohr Institute of the University of Copenhagen on the design, fabrication, and testing of the calibration targets.A key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith (broken rock and dust).Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.The Mars 2020 Perseverance mission is part of NASA's Moon to Mars exploration approach, which includes Artemis missions to the Moon that will help prepare for human exploration of the Red Planet.NASA's Jet Propulsion Laboratory, which is managed for NASA by Caltech in Pasadena, California, built and manages operations of the Perseverance rover. Arizona State University leads the operations of the Mastcam-Z instrument, working in collaboration with Malin Space Science Systems in San Diego, on the design, fabrication, testing, and operation of the cameras, and in collaboration with the Neils Bohr Institute of the University of Copenhagen on the design, fabrication, and testing of the calibration targets.For more about Perseverance: mars.nasa.gov/mars2020/For more about the Mars Sample Return campaign: mars.nasa.gov/msr | |
NASA's Mars Reconnaissance Orbiter observed sand dunes in the north polar regions of Mars showing light coatings of pale orange dust blown partially across the dark basaltic sand. Around the edges of the dunes, patches of seasonal dry ice remain. | Map Projected Browse ImageClick on image for larger versionNASA's Mars Reconnaissance Orbiter (MRO) observed sand dunes in the north polar regions of Mars showing light coatings of pale orange dust blown partially across the dark basaltic sand. Around the edges of the dunes, patches of seasonal dry ice remain.These patches will be gone soon as they sublimate (turn from ice to gas) in the summer sun. Some blocks of ice are visible at the foot of an alcove formed by a sand avalanche down the slipface of the dune.The map is projected above at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 32.0 centimeters (12.6 inches) per pixel (with 1 x 1 binning); objects on the order of 96 centimeters (37.8 inches) across are resolved.] North is up.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
NASA's Mars Global Surveyor shows an intermountain valley floor in the Libya Montes region of Mars. The Libya Montes were formed by the giant impact that created the ancient Isidis basin. | (A)(B)(C)This Mars Global Surveyor Mars Orbiter Camera narrow angle image (top) shows an intermountain valley floor in the Libya Montes region of Mars. Its regional setting is seen in the wide angle color mosaic (Figure A). The Libya Montes were formed by the giant impact that created the ancient Isidis basin. The Libya Mountains and valleys -- like the one shown here -- were subsequently modified and eroded by other processes, including wind, impact cratering, and flow of liquid water to make the small valley that runs across the middle of the scene. Until the mission was canceled, the Libya Montes region was among the top two candidates for the Mars Surveyor 2001 Lander. This image, illuminated by sunlight from the left, covers an area 3 kilometers (1.9 miles) wide and 19 kilometers (11.8 miles) long. The scene is located near 1.5°N, 278.4°W and was acquired on June 27, 1999. The high resolution color view (top) was created by combining the colors derived from Mars Orbiter Camera Wide Angle views of the region obtained in May 1999 (Figures A and B) with the high resolution view obtained in June 1999 (Figure C). | |
Inside Mission Control at NASA's Jet Propulsion Laboratory, Mars 2020 Perseverance team members eagerly watched and waited before the rover safely landed on the Martian surface. | Inside Mission Control at NASA's Jet Propulsion Laboratory in Southern California, Mars 2020 Perseverance team members eagerly watched and waited while the spacecraft performed a complex series of steps before the rover safely landed on the Martian surface.A key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith (broken rock and dust).Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.The Mars 2020 mission is part of a larger program that includes missions to the Moon as a way to prepare for human exploration of the Red Planet.JPL, which is managed for NASA by Caltech in Pasadena, California, built and manages operations of the Perseverance rover.For more about Perseverance, go to: mars.nasa.gov/mars2020/ or nasa.gov/perseverance. | |
This image shows the remains of an ancient delta in Mars' Jezero Crater, which NASA's Perseverance Mars rover will explore for signs of fossilized microbial life. | This image shows the remains of an ancient delta in Mars' Jezero Crater, which NASA's Perseverance Mars rover will explore for signs of fossilized microbial life. The image was taken by the High Resolution Stereo Camera aboard the ESA (European Space Agency) Mars Express orbiter. The European Space Operations Centre in Darmstadt, Germany, operates the ESA mission. The High Resolution Stereo Camera was developed by a group with leadership at the Freie Universitat Berlin. | |
This false-color image from NASA's Mars Odyssey spacecraft shows a channel at the end of the Marwrth Valles, taken during Mars' northern spring season. | 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 blue intensity image. These three images are then combined to produce a full color, single image. Because the THEMIS color filters don't span the full range of colors seen by the human eye, a color THEMIS image does not represent true color. Also, because each single-filter image is contrast enhanced before inclusion in the three-color image, the apparent color variation of the scene is exaggerated. Nevertheless, the color variation that does appear is representative of some change in color, however subtle, in the actual scene. Note that the long edges of THEMIS color images typically contain color artifacts that do not represent surface variation.This false color image is from further downstream in Mawrth Valles than yesterday's image. The channel here is at the end of the vallis. This image was collected during the Northern Spring season. Image information: VIS instrument. Latitude 26.7, Longitude 340.2 East (19.8 West). 37 meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Global Surveyor shows | MGS MOC Release No. MOC2-557, 27 November 2003This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows sand dunes and large ripples in a crater in the Hellespontus region of Mars. The winds that formed these dunes generally blew from the left/lower-left (west/southwest). Unlike the majority of dunes on Earth, sand dunes on Mars are mostly made up of dark, rather than light, grains. This scene is located near 50.3°S, 327.5°W. The image covers an area 3 km (1.9 mi) wide, and is illuminated by sunlight from the upper left. | |
The floor of the crater at the top of this image from NASA's 2001 Mars Odyssey spacecraft is completely covered by a large sand sheet with surface dune forms. Now that is it near the end of northern spring all the frost has disappeared from the sand. | Context imageThe floor of the crater at the top of this VIS image is completely covered by a large sand sheet with surface dune forms. Now that is it near the end of northern spring all the frost has disappeared from the sand.Orbit Number: 45541 Latitude: 73.8601 Longitude: 318.667 Instrument: VIS Captured: 2012-03-21 02:04Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of Olympia Undae where the surface beneath the dunes is visible. | Context imageThis VIS image shows part of Olympia Undae where the surface beneath the dunes is visible.Orbit Number: 47083 Latitude: 79.9317 Longitude: 136.222 Instrument: VIS Captured: 2012-07-26 00:01Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows many of the channel segments of Granicus Valles. Granicus Valles is a complex channel system located west of Elysium Mons. | Context imageThis VIS image shows many of the channel segments of Granicus Valles. Granicus Valles is a complex channel system located west of Elysium Mons. The system is approximately 750km (466 miles) long. It is likely that both water and lava played a part in creation of the feature.Orbit Number: 85523 Latitude: 29.3053 Longitude: 128.19 Instrument: VIS Captured: 2021-03-26 06:42Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Global Surveyor shows dark north polar dunes overlying other materials in the north polar region of Mars. | 21 March 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows dark north polar dunes overlying other materials in the north polar region.Location near: 79.1°N, 228.8°W Image width: ~3 km (~1.9 mi) Illumination from: lower left Season: Northern Summer | |
NASA's Mars Global Surveyor shows changes in dark streak patterns caused by wind movement of dust on Mars. | MGS MOC Release No. MOC2-358, 12 May 2003Mars is a dynamic planet. This pair of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) pictures, taken 2 Mars years apart, show changes in dark streak patterns caused by wind movement of dust. The top picture was taken in July 1999, the bottom one in March 2003. The pair of images are in Tharsis near 9.5°S, 128.5°W. Sunlight illuminates both from the upper left. | |
North polar troughs are the typical location to see evidence of strong polar surface winds. This image captured by NASA's 2001 Mars Odyssey shows 'streamers' of clouds created by catabatic winds. | Context imageNorth polar troughs are the typical location to see evidence of strong polar surface winds. This VIS image shows 'streamers' of clouds created by catabatic winds. Catabatic winds are created by cold air sinking at the pole and then speeding along the surface towards the edge of the polar cap. When the wind enters troughs the wind regime changes from laminar flow to choatic and clouds of ice particles or dust are visible.Orbit Number: 37100 Latitude: 82.9725 Longitude: 97.2613 Instrument: VIS Captured: 2010-04-26 03:29Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Exploration Rover Opportunity shows in superb detail a portion of the puzzling rock outcropping the rover investigated. | This high-resolution image captured by the Mars Exploration Rover Opportunity's panoramic camera shows in superb detail a portion of the puzzling rock outcropping that scientists are eagerly planning to investigate. Presently, Opportunity is on its lander facing northeast; the outcropping lies to the northwest. These layered rocks measure only 10 centimeters (4 inches) tall and are thought to be either volcanic ash deposits or sediments carried by water or wind. The small rock in the center is about the size of a golf ball. | |
This image from NASA's Mars Odyssey spacecraft shows small, bright, linear dunes located on lava flows from Arsia Mons. | Context image for PIA09293Bright DunesThese small, bright, linear dunes are located on lava flows from Arsia Mons.Image information: VIS instrument. Latitude -17.8N, Longitude 247.1E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
The wheels of NASA's Mars Exploration Rover Opportunity dug deep into the soft, sandy material of a wind-shaped ripple in Mars' Meridiani Planum region on April 26, 2005. Getting the rover out of the dunes took more than five weeks. | The wheels of NASA's Mars Exploration Rover Opportunity dug more than 10 centimeters (4 inches) deep into the soft, sandy material of a wind-shaped ripple in Mars' Meridiani Planum region during the rover's 446th martian day, or sol (April 26, 2005). Getting the rover out of the ripple, dubbed "Purgatory Dune," required more than five weeks of planning, testing, and carefully monitored driving. Opportunity used its navigation camera to capture this look back at the ripple during sol 491 (June 11, 2005), a week after the rover drove safely onto firmer ground. The ripple that became a sand trap is about one-third meter (one foot) tall and 2.5 meters (8 feet) wide. | |
NASA's Mars Exploration Rover Opportunity tried to get as detailed a look as possible at a target region near eastern foot of 'Burns Cliff.' The intervening layered terrain was too difficult for driving the rover closer. | Researchers used a special imaging technique with the panoramic camera on NASA's Mars Exploration Rover Opportunity to get as detailed a look as possible at a target region near eastern foot of "Burns Cliff." The intervening terrain was too difficult for driving the rover closer. The target is the boundary between two sections of layered rock. The layers in lower section (left) run at a marked angle to the layers in next higher section (right). This view is the product of a technique called super resolution. It was generated from data acquired on sol 288 of Opportunity's mission (Nov. 14, 2004) from a position along the southeast wall of "Endurance Crater." Resolution slightly higher than normal for the panoramic camera was synthesized for this view by combining 17 separate images of this scene, each one "dithered" or pointed slightly differently from the previous one. Computer manipulation of the individual images was then used to generate a new synthetic view of the scene in a process known mathematically as iterative deconvolution, but referred to informally as super resolution. Similar methods have been used to enhance the resolution of images from the Mars Pathfinder mission and the Hubble Space Telescope. | |
NASA's Mars Global Surveyor shows patterns created by defrosting processes on the martian south polar seasonal ice cap. Dark cracks form a polygon pattern, and wind blows material to form varied bright and dark streaks. | MGS MOC Release No. MOC2-487, 18 September 2003This June 2003 Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) picture shows patterns created by defrosting processes on the south polar seasonal ice cap. Seasonal cap refers to the part of the polar cap that comes and goes with the seasons, as opposed to the residual cap, which lasts throughout the summer. The area shown here, in summer, will have no frost. This picture was taken during southern spring. As the seasonal frost begins to sublime away, dark cracks form a polygon pattern, and wind blows material to form varied bright and dark streaks. What is unknown is whether the dark streaks consist of sand and silt from beneath the seasonal frost, or whether they, too, consist of frost that has been transformed into coarse-grained particles that can be mobilized by wind. Alternatively, the streaks represent erosion and removal of frost, rather than deposition of granular material. The bright streaks are most likely made of frost--whether they are water ice or carbon dioxide ice remains to be determined. The bulk of the frosted surface shown here is carbon dioxide ice. The image is located near 87.3°S, 192.4°W. The picture covers an area 3 km (1.9 mi) wide and is illuminated by sunlight from the upper left. | |
This illustration shows a concept for multiple robots that would team up to ferry to Earth samples collected from the Mars surface by NASA's Mars Perseverance rover. | This illustration shows a concept for multiple robots that would team up to ferry to Earth samples collected from the Mars surface by NASA's Mars Perseverance rover.NASA and ESA (European Space Agency) are developing concepts for the Mars Sample Return program designed to retrieve the samples of Martian rocks and soil being collected and stored in sealed tubes by Perseverance. In the future, the samples would be returned to Earth for detailed laboratory analysis.The current concept envisions delivering a Mars lander near Jezero Crater, where Perseverance (far left) is caching, or collecting, samples. A NASA-provided Sample Retrieval Lander (far right) would carry a NASA rocket (the Mars Ascent Vehicle), and a second lander, pictured in the background, would carry ESA's Sample Fetch Rover (center), which is a little smaller than a golf cart. The fetch rover would gather the cached samples left on the surface by Perseverance and transport them to the Sample Retrieval Lander, where they would then be transferred onto the Mars Ascent Vehicle. Perseverance could also deliver additional samples directly to the lander. The Mars Ascent Vehicle would launch a container with the samples inside into orbit. Waiting in Mars orbit would be an ESA-provided Earth Return Obiter, which would rendezvous with and capture the orbiting sample container using a NASA-provided Capture, Containment, and Return System. This system would capture and orient the container, then prepare it for return to Earth inside the Earth Entry System.For more information, visit: mars.nasa.gov/msr. | |
This image of the South Séítah region of Jezero Crater was taken by NASA's Ingenuity Mars Helicopter during its 11th flight on August 4, 2021. | Figure 1This image shows the "South Séítah" region of Jezero Crater, captured by NASA's Ingenuity Mars Helicopter during its 11th flight on August 4, 2021. At the bottom center of the image is Ingenuity's shadow. Above it, toward the top of the frame – just beyond the dune field and right of center – is the Perseverance rover (the bright white dot). Figure 1 zooms into the scene, revealing Perseverance's location. The Ingenuity Mars Helicopter was built by JPL, which also manages the technology demonstration project for NASA Headquarters. It is supported by NASA's Science, Aeronautics Research, and Space Technology mission directorates. NASA's Ames Research Center in California's Silicon Valley, and NASA's Langley Research Center in Hampton, Virginia, provided significant flight performance analysis and technical assistance during Ingenuity's development. AeroVironment Inc., Qualcomm, and SolAero also provided design assistance and major vehicle components. Lockheed Martin Space designed and manufactured the Mars Helicopter Delivery System. | |
This image from NASA's Mars Odyssey spacecraft shows what looks like Mickey Mouse's hat on martian terrain. | Context imageDo you see what I see? There is a mickey mouse hat sitting on the top right side of this daytime infrared image.Orbit Number: 33506 Latitude: -21.6082 Longitude: 85.9368 Instrument: IR Captured: 2009-07-04 04:10 Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image shows NASA's Mars Exploration Rover Spirit's view from its location inside the shallow depression dubbed 'Laguna Hollow.' Tracks in the soil show that Spirit drove forward a bit, wiggled its wheels, then turned and backed up. | This image shows the Mars Exploration Rover Spirit's view from its new location inside the shallow depression dubbed "Laguna Hollow." To get a better look at the soil making up the hollow, Spirit drove forward a bit, wiggled its wheels, then turned and backed up. The result - a scrape on the floor and a clod of dirt stuck on one of Spirit's wheels - told scientists that the soil is sticky and reminiscent of that observed at the airbag drag mark nicknamed "Magic Carpet." Spirit will further investigate this disturbed patch of soil with its robotic arm beginning today (Feb. 19, 2004). It will also dig a trench at "Laguna Hollow" with one of its wheels. This fish-eye image was taken by the rover's hazard-avoidance camera. | |
NASA's Mars Global Surveyor shows a chilly Lomonosov Crater in the northern hemisphere of Mars on April 20, 2000. The rims of the crater appear white because they are covered with wintertime frost. | It is still winter in the northern hemisphere of Mars. On April 20, 2000, the Mars Orbiter Camera (MOC) onboard Mars Global Surveyor (MGS) captured this view of a chilly Lomonosov Crater. The rims of the crater appear white because they are covered with wintertime frost. A dark patch just right of center on the crater floor is a sand dune field. Both low-lying ground fogs(fuzzy, patchy areas around the lower perimeter of the crater) and higher cloud layers (fuzzy white arcs seen within the crater and towards the upper right) obscure much of the surface. The sun, only 12° above the horizon, bathes the scene in a reddish-brown hue. Lomonosov Crater is about 150 km (93 mi) across and located on the martian northern plains at 64.8° N, 8.8° W. The crater is named for the 18th Century Russian chemist, Mikhail V. Lomonosov (1741-1765). Spring will arrive in the martian northern hemisphere around June 1, 2000, and summer will come in December 2000. Sunlight illuminates this scene from the lower left. | |
This image from NASA's Mars Odyssey spacecraft shows Arsia Mons, the southernmost of the Tharsis volcanoes. For comparison, the largest volcano on Earth is Mauna Loa. | Arsia Mons is the southernmost of the Tharsis volcanoes. It is 270 miles in diameter, almost 12 miles high, and the summit caldera is 72 miles wide. For comparison, the largest volcano on Earth is Mauna Loa. From its base on the sea floor, Mauna Loa measures only 6.3 miles high and 75 miles in diameter. The image here is a mosaic of several daytime IR images. The indentations on the SW and NE sides align with the Pavonis Mons and Ascreaus Mons to the NE. This may indicate a large fracture/vent system was responsible for the eruptions that formed all three volcanoes.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image shows a portion of Auqakuh Vallis on Mars as seen by NASA's 2001 Mars Odyssey spacecraft. | Context image for PIA08465Auqakuh VallisThis image shows a portion of Auqakuh Vallis.Image information: VIS instrument. Latitude 31.0N, Longitude 60.6E. 19 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows sand dunes located in the mountains at the margin of the Argyre Basin. | Context image for PIA10276Argyre DunesThese sand dunes are located in the mountains at the margin of the Argyre Basin.Image information: VIS instrument. Latitude -47.9N, Longitude 304.8E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows a crater just out of frame to the left in this image located on the floor of Schiaparelli Crater. Within the lows of the ejecta blanket of the small crater are old, linear dunes. | Context image for PIA10309Old DunesThe crater just out of frame to the left in this image is located on the floor of Schiaparelli Crater. Within the lows of the ejecta blanket of the small crater are old, linear dunes. These dunes do not appear to be active at this time.Image information: VIS instrument. Latitude -2.9N, Longitude 14.5E. 18 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This infrared image captured by NASA's 2001 Mars Odyssey spacecraft shows dunes in an unnamed crater in Noachis Terra. | Context imageThis infrared image shows dunes in an unnamed crater in Noachis Terra.Latitude: -49.5174 Longitude: 33.942 Instrument: IR Captured: 2015-01-27 07:56Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
Multiple channels in this image from NASA's 2001 Mars Odyssey dissect this region on the margin of Terra Sabaea on Mars. | Context imageMultiple channels dissect this region on the margin of Terra Sabaea.Orbit Number: 46748 Latitude: 32.9252 Longitude: 58.7282 Instrument: VIS Captured: 2012-06-28 10:40Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
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 Pyrrhae Chaos. | Context imageThe 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 Pyrrhae Chaos.Orbit Number: 58875 Latitude: -10.0832 Longitude: 332.017 Instrument: VIS Captured: 2015-03-23 11:20Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Phoenix Mars Lander inserted the four needles of its thermal and conductivity probe into Martian soil during Sept. 4, 2008. This imaging served as a check of whether soil had stuck to the needles. | NASA's Phoenix Mars Lander inserted the four needles of its thermal and conductivity probe into Martian soil during the 98th Martian day, or sol, of the mission and left it in place until Sol 99 (Sept. 4, 2008).The Surface Stereo Imager on Phoenix took this image on the morning of Sol 99 after the probe was lifted away from the soil. This imaging served as a check of whether soil had stuck to the needles.The thermal and conductivity probe measures how fast heat and electricity move from one needle to an adjacent one through the soil or air between the needles. Conductivity readings can be indicators about water vapor, water ice and liquid water.The probe is part of Phoenix's Microscopy, Electrochemistry and Conductivity suite of instruments. The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.Photojournal Note: As planned, the Phoenix lander, which landed May 25, 2008 23:53 UTC, ended communications in November 2008, about six months after landing, when its solar panels ceased operating in the dark Martian winter. | |
This image from NASA's Mars Odyssey shows part of Ceraunius Fossae. The linear depressions are fault bounded features called graben. | Context imageThis VIS image shows part of Ceraunius Fossae. The linear depressions are fault bounded features called graben. Graben form from tectonic forces that are pulling apart the surface, created space for material to "slide down" along the fault. Alba Mons is surrounded by extensive regions of closely spaced graben. Ceraunius Fossae is located south of Alba Mons.Orbit Number: 78406 Latitude: 27.7831 Longitude: 248.084 Instrument: VIS Captured: 2019-08-18 06:29Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
On Oct. 31, 2010, NASA's Mars Exploration Rover Opportunity tooke this false-color image showing a portion of Endeavour Crater's eastern rim. | NASA's Mars Exploration Rover Opportunity used its panoramic camera to record this eastward horizon view on the 2,407th Martian day, or sol, of the rover's work on Mars (Oct. 31, 2010). The view is presented in false color to make differences in surface materials more visible. A portion of Endeavour Crater's eastern rim, nearly 30 kilometers (19 miles) in the distance, is visible over the Meridiani plain. Endeavour is about 22 kilometers (14 miles) in diameter. The rover team chose Endeavour Crater as a long-term destination for Opportunity in mid-2008, after the rover had investigated the much-smaller Victoria Crater for two years. The rover is headed for a portion of Endeavour's western rim not visible in this image. This view combines exposures taken through three filters of the panoramic camera (Pancam) admitting wavelengths of 752 nanometers, 535 nanometers and 432 nanometers.Opportunity completed its three-month prime mission in April 2004 and has continued working in mission extensions since then. | |
The location where NASA's Perseverance will begin depositing its first cache of samples is shown in this image taken by the Mars rover on Dec. 14, 2022. | Figure AThe location where NASA's Perseverance will begin depositing its first cache of samples is shown in this image taken by the Mars rover on Dec. 14, 2022, the 646th Martian day, or sol, of the mission. This enhanced color image was taken by one of the rover's navigation cameras and is not representative of the way the scene would look to the human eye.Figure A includes an annotation pointing out the location of the sample depot site in the distance.A key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith (broken rock and dust).Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.The Mars 2020 Perseverance mission is part of NASA's Moon to Mars exploration approach, which includes Artemis missions to the Moon that will help prepare for human exploration of the Red Planet.NASA's Jet Propulsion Laboratory, which is managed for the agency by Caltech in Pasadena, California, built and manages operations of the Perseverance rover.For more about Perseverance: mars.nasa.gov/mars2020/ | |
A channel-like feature roughly halfway between the Isidis Basin and Elysium Mons on Mars shows no connection to either a source region or terminal basin is seen in this image from NASA's Mars Odyssey. | Released 22 May 2003A channel-like feature roughly halfway between the Isidis Basin and Elysium Mons shows no connection to either a source region or terminal basin. It may be that this feature is not a channel at all and has instead arisen from the erosion of a once continuous layer of material into remnants that mimic a channel.Image information: VIS instrument. Latitude 20.9, Longitude 105 East (255) meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
These are the first two full-resolution images of the Martian surface from the Navigation cameras on NASA's Curiosity rover, which are located on the rover's 'head' or mast. The rim of Gale Crater can be seen in the distance beyond the pebbly ground. | These are the first two full-resolution images of the Martian surface from the Navigation cameras on NASA's Curiosity rover, which are located on the rover's "head" or mast. The rim of Gale Crater can be seen in the distance beyond the pebbly ground. The topography of the rim is very mountainous due to erosion. The ground seen in the middle shows low-relief scarps and plains. The foreground shows two distinct zones of excavation likely carved out by blasts from the rover's descent stage thrusters.These are full-resolution images, 1024 by 1024 pixels in size. | |
This image acquired on April 8, 2018 by NASA's Mars Reconnaissance Orbiter, shows the gullied western slopes of an unnamed crater (about 10 kilometers wide) in Acidalia Planitia. | Map Projected Browse ImageClick on image for larger versionThis image was acquired on April 8, 2018 by NASA's Mars Reconnaissance Orbiter. This image shows the gullied western slopes of an unnamed crater (about 10 kilometers wide) in Acidalia Planitia. These slopes have gone through a complicated history of gully erosion of the bedrock layers in the upper section, followed by the formation of fractures along the lower slopes.As the gullies continued to form, fractures cut across them and their debris fans in the lower part of the slopes. A prominent cliff has been eroded by more recent gully activity. The curved ridges and lobes on the crater floor, downslope of the debris fans, along with multiple fractures, suggest that the subsurface was ice-rich. This is an example of how geologists can utilize the concept of superposition to unravel the relative timing of geological events in the crater's history.The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 29.8 centimeters (11.7 inches) per pixel (with 1 x 1 binning); objects on the order of 89 centimeters (35.0 inches) across are resolved.] North is up.This is a stereo pair with ESP_055320_2185.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
This image from NASA's Mars Odyssey shows part of Margaritifer Terra. | Context imageThe 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.Orbit Number: 77542 Latitude: 18.1396 Longitude: 337.812 Instrument: VIS Captured: 2019-06-08 02:52Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows channels located on the floor of Newton Crater on Mars. | Context image for PIA10323Newton CraterThe channels in this VIS image are located on the floor of Newton Crater.Image information: VIS instrument. Latitude -39.4N, Longitude 200.1E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
In this image from NASA's 2001 Mars Odyssey spacecraft a complex region of multiple overlapping landslide deposits fills most the the frame. In the center of the image the top layer has the lobate edges and radial surface grooves of a low volume slide. | Context image In this VIS image a complex region of multiple overlapping landslide deposits fills most the the frame. In the center of the image the top layer has the lobate edges and radial surface grooves of a low volume slide. It appears to be the top of a complex layering of materials, It is possible that all the lower layers are landslides as well. At the top of the image are a series of smaller lobate shaped landslide deposits Whether the layers formed very close in time of over thousands of years can not be determined in the image. Tithonium Chasma has numerous large landslide deposits. The resistant material of the plateau surface forms the linear ridges of the canyon wall. Large landslides have changed the walls and floor of the canyon. A landslide is a failure of slope due to gravity. They initiate due to several reasons. A lower layer of poorly cemented/resistant material may have been eroded, undermining the wall above which then collapses; earth quake seismic waves can cause the slope to collapse; and even an impact event near the canyon wall can cause collapse. As millions of tons of material fall and slide down slope a scalloped cavity forms at the upper part where the slope failure occurred. At the material speeds downhill it will pick up more of the underlying slope, increasing the volume of material entrained into the landslide. Whereas some landslides spread across the canyon floor forming lobate deposits, very large volume slope failures will completely fill the canyon floor in a large complex region of chaotic blocks.Tithonium Chasma is at the western end of Valles Marineris. Valles Marineris is over 4000 kilometers long, wider than the United States. Tithonium Chasma is almost 810 kilometers long (499 miles), 50 kilometers wide and over 6 kilometers deep. In comparison, the Grand Canyon in Arizona is about 175 kilometers long, 30 kilometers wide, and only 2 kilometers deep. The canyons of Valles Marineris were formed by extensive fracturing and pulling apart of the crust during the uplift of the vast Tharsis plateau. Landslides have enlarged the canyon walls and created deposits on the canyon floor. Weathering of the surface and influx of dust and sand have modified the canyon floor, both creating and modifying layered materials.The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 71,000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water and lava, and a variety of other feature, THEMIS has imaged them all. For the next several months the image of the day will focus on the Tharsis volcanoes, the various chasmata of Valles Marineris, and the major dunes fields. We hope you enjoy these images!Orbit Number: 35746 Latitude: -4.47838 Longitude: 272.133 Instrument: VIS Captured: 2010-01-04 14:22Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
The western Utopia Planitia in the Northern mid-latitudes of Mars is marked by a peculiar type of depression with scalloped edges and by a network of polygonal fractures as seen by NASA's Mars Reconnaissance Orbiter. | Map Projected Browse ImageClick on the image for larger versionThe western Utopia Planitia in the Northern mid-latitudes of Mars is marked by a peculiar type of depression with scalloped edges and by a network of polygonal fractures.The scalloped depressions are typical features; a smooth layered terrain located between 40 and 60 degrees in both hemispheres. Scalloped depressions probably form by removal of ice-rich subsurface material by sublimation (ice transforming directly from a solid to a gaseous state), a process that may still be active today. Isolated scalloped depressions generally have a steep pole-facing scarp and a gentler equator-facing slope. This asymmetry is interpreted as being the result of difference in solar heating. Scalloped depressions may coalesce, leading to the formation of large areas of pitted terrain.The polygonal pattern of fractures resembles permafrost polygons that form in terrestrial polar and high alpine regions by seasonal-to-annual contraction of the permafrost (permanently frozen ground). On Earth, such polygons indicate the presence of ground ice.These landforms most likely show that sub-surface ice is present or has been present geologically recently at these latitudes, and they may slowly be continuing their development at the present time.This is a stereo pair with PSP_002439_2265.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
NASA's Mars Global Surveyor shows Gusev Crater on Mars, in which the Mars Exploration Rover, Spirit, landed on 4 January 2004. | 2 January 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) wide angle image shows the crater in which the Mars Exploration Rover, Spirit, is scheduled to land on 4 January 2004 (around 8:35 p.m., 3 January 2004, Pacific Standard Time). The white ellipse marks the approximate location of Spirit's landing zone. Gusev Crater is about 165 km (103 mi) across. The valley that enters Gusev from the south-southeast (bottom/lower right) is named Ma'adim Vallis. The dark areas on the floor of Gusev, when viewed at higher resolution, are found to be surfaces from which dust devils and wind gusts have removed or disrupted the fine, bright dust that otherwise blankets the crater floor. This image, acquired in November 2003, is located near 14.5°S, 184.6°W. Sunlight illuminates the scene from the lower left. | |
Spirit's Traverse, Sols 1 to 1,386 | Annotated VersionClick on the image for the larger version
NASA's Mars Exploration Rover Spirit was crossing northward on a low plateau called "Home Plate" on the 1,386th Martian day, or sol, (Nov. 26, 2007) of Spirit's time on Mars. By that time, nearly 47 months into a mission originally planned to last three months, Spirit had driven 7,435 meters (4.62 miles). From its landing site near the northwest corner of this map, Spirit crossed a plain to reach the Columbia Hills, climbed over the summit of Husband Hill, and descended into the "Inner Basin" of the range, near the southeast corner of the map. For this map, the yellow line indicating Spirit's route has been overlaid onto a portion of an image taken by the High Resolution Imaging Science Experiment on NASA's Mars Reconnaissance Orbiter on Nov. 22, 2006, That image is catalogued as PSP_001513_1655 (see also PIA01897). The scale bar on the map is 500 meters (1,640 feet) long. North is up. | |
This setup is being used at JPL to test a 16-inch-diameter (40-centimeter-diameter) footpad for a future Mars lander. | This setup is being used at NASA's Jet Propulsion Laboratory to test a 16-inch-diameter (40-centimeter-diameter) footpad for a future Mars lander. The footpad was plunged into a test bed filled with 10,000 pounds (4,536 kilograms) of simulated Martian soil in order to see how deep it would sink – too far, and the lander's belly could scrape against the ground during touchdown, damaging it.The Sample Retrieval Lander, which would be central to NASA's Mars Sample Return campaign, is estimated to weigh as much as 5,016 pounds (2,275 kilograms). It would be the heaviest spacecraft ever to land on the Red Planet. In order to understand how energy would be absorbed during the landing of such a massive spacecraft, JPL engineers have been conducting drop tests of a full-size footpad.Mars Sample Return will revolutionize our understanding of Mars by bringing scientifically selected samples to Earth for study using the most sophisticated instrumentation around the world. NASA's planned Mars Sample Return (MSR) campaign would fulfill one of the highest priority solar system exploration goals identified by the National Academies of Sciences, Engineering and Medicine in the past three decadal surveys. This strategic partnership with the ESA (European Space Agency) features the first mission to return samples from another planet, including the first launch from the surface of another planet. The samples being collected by NASA's Perseverance rover during its exploration of an ancient river delta are thought to be the best opportunity to reveal the early evolution of Mars, including the potential for ancient life. | |
This image from NASA's Mars Odyssey shows part of Sirenum Fossae. The linear depressions in this VIS image are tectonic graben. | Context imageThe 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 Sirenum Fossae. The linear depressions in this VIS image are tectonic graben. Graben are formed by extension of the crust and faulting. When large amounts of pressure or tension are applied to rocks on timescales that are fast enough that the rock cannot respond by deforming, the rock breaks along faults. In the case of a graben, two parallel faults are formed by extension of the crust and the rock in between the faults drops downward into the space created by the extension. Several graben are visible in this THEMIS VIS image, trending from north-northeast to south-southwest. Because the faults defining the graben are formed perpendicular to the direction of the applied stress, we know that extensional forces were pulling the crust apart in the west-northwest/east-southeast direction. The Sirenum Fossae graben are 2735km (1700 miles) long.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 blue intensity image. These three images are then combined to produce a full color, single image. Because the THEMIS color filters don't span the full range of colors seen by the human eye, a color THEMIS image does not represent true color. Also, because each single-filter image is contrast enhanced before inclusion in the three-color image, the apparent color variation of the scene is exaggerated. Nevertheless, the color variation that does appear is representative of some change in color, however subtle, in the actual scene. Note that the long edges of THEMIS color images typically contain color artifacts that do not represent surface variation.Orbit Number: 92540 Latitude: -32.6048 Longitude: 205.563 Instrument: VIS Captured: 2022-10-25 00:23Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey spacecraft is of a dune field on Mars within Nili Patera, the northern caldera of a large volcanic complex in Syrtis Major. | Our topic for the weeks of April 4 and April 11 is dunes on Mars. We will look at the north polar sand sea and at isolated dune fields at lower latitudes. Sand seas on Earth are often called "ergs," an Arabic name for dune field. A sand sea differs from a dune field in two ways: 1) a sand sea has a large regional extent, and 2) the individual dunes are large in size and complex in form.This VIS image shows a dune field within Nili Patera, the northern caldera of a large volcanic complex in Syrtis Major.Image information: VIS instrument. Latitude 9, Longitude 67 East (293 West). 19 meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image shows NASA's Mars Exploration Rover Opportunity sitting along the rim of 'Endurance Crater' in the Meridiani Planum region of Mars on May 15, 2004. | This right eye in a stereo pair of views was assembled from three navigation camera frames that NASA's Mars Exploration Rover Opportunity acquired on sol 109, May 15, 2004. It is presented in a cylindrical-perspective projection. Opportunity is sitting along the rim of "Endurance Crater" in the Meridiani Planum region.See PIA05965 for 3-D view and PIA05966 for left eye view of this right eye cylindrical-perspective projection. | |
This image from NASA's Mars Odyssey shows many channels that dissect the surface in this region of Promethei Terra. | Context imageMany channels dissect the surface in this region of Promethei Terra.Orbit Number: 83490 Latitude: -38.5185 Longitude: 106.431 Instrument: VIS Captured: 2020-10-09 20:57Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of Daedalia Planum. | Context image This VIS image shows a small portion of Daedalia Planum. The lava flows in this region originated at Arsia Mons, one of the large Tharsis volcanoes. Several different elevations of lava flow are visible in this image, some much smoother in appearance than others.Orbit Number: 66838 Latitude: -18.1894 Longitude: 231.819 Instrument: VIS Captured: 2017-01-07 07:45Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image acquired on August 8, 2019 by NASA's Mars Reconnaissance Orbiter, shows layered sediments on the floor of eastern Coprates Chasma in Valles Marineris, the grandest canyon on Mars. | Map Projected Browse ImageClick on image for larger versionLayered sedimentary rocks are key to understanding the geologic history of a planet, recording the sequence of deposition and the changes over time in the materials that were deposited. These layered sediments are on the floor of eastern Coprates Chasma in Valles Marineris, the grandest canyon on Mars. They are erosional remnants of a formerly much more extensive sedimentary deposit that once filled the floor of the canyon but is nowadays reduced to isolated mesas.The origin of the deposits is not yet known. Various theories attribute the sediments to wind blown dust and sand, or to volcanic materials, or accumulations of debris from avalanches originating from the canyon walls, or even to lakebed sediments laid down when the canyons were filled with liquid water. Some sediments are devoid of boulders or blocks larger than the limit of resolution (about 0.5 meters), so avalanche debris is unlikely. We see fine laminations with a horizontal spacing of about 2 meters and a vertical separation less than 2 meters. No previous orbital observations were capable of resolving such fine scale layering.The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. (The original image scale is 26.9 centimeters [10.6 inches] per pixel [with 1 x 1 binning]; objects on the order of 81 centimeters [31.9 inches] across are resolved.) North is up.The University of Arizona, in Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., in Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
This image from NASA's Mars Odyssey shows a section of Granicus Valles. Granicus Valles is a complex channel system located west of Elyisum Mons. | Context imageA section of Granicus Valles crosses the center of this VIS image. Granicus Valles is a complex channel system located west of Elyisum Mons. The channel system is approximately 750km long. It is likely that both water and lava played a part in creating the channel.Orbit Number: 77886 Latitude: 27.6994 Longitude: 131.153 Instrument: VIS Captured: 2019-07-06 10:48Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows yardangs which are formed when winds erode poorly cemented materials, such as these that form Zephyria Planum. | Context image for PIA10894YardangsThe linear features in this VIS image are called yardangs. Yardangs are formed when winds erode poorly cemented materials, like those that form Zephyria Planum.Image information: VIS instrument. Latitude 1.1N, Longitude 150.9E. 18 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image released on Oct 18, 2004 from NASA's 2001 Mars Odyssey shows Reull Vallis, located in the Martian southern highlands, just east of Hellas Basin. | This week we will be examining images of Reull Vallis. Reull Vallis is located in the Martian southern highlands, just east of Hellas Basin. This extensive channel system records an interesting fluvial and mass wasting geologic history of the area. In many images show interesting patterns of mass wasted material in the bottom of the channel. For more information on the geology of Reull Vallis see http://viking.eps.pitt.edu/public/IcarusPub/Geol_RVR_Icarus.html.Image information:VIS instrument. Latitude -41.1, Longitude 100.3 East (259.7 West). 19 meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows part of the floor of Becquerel Crater, including a large layered deposit and small individual sand dunes. | Context imageThe 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 Becquerel Crater, including a large layered deposit (cream color) and small individual sand dunes (dark blue). Becquerel Crater is located in Arabia Terra and is 165km (102 miles) in diameter.Orbit Number: 77816 Latitude: 21.3881 Longitude: 351.798 Instrument: VIS Captured: 2019-06-30 16:25Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This artist's concept depicts NASA's Mars 2020 rover on the surface of Mars. The mission takes the next step by not only seeking signs of habitable conditions on Mars in the ancient past, but also searching for signs of past microbial life itself. | Photojournal Note: This artist's concept was updated in November 2017. See PIA22111.
This artist's concept depicts NASA's Mars 2020 rover on the surface of Mars. The mission takes the next step by not only seeking signs of habitable conditions on Mars in the ancient past, but also searching for signs of past microbial life itself. The Mars 2020 rover introduces a drill that can collect core samples of the most promising rocks and soils and set them aside on the surface of Mars. A future mission could potentially return these samples to Earth. Mars 2020 is targeted for launch in July/August 2020 aboard an Atlas V 541 rocket from Space Launch Complex 41 at Cape Canaveral Air Force Station in Florida. NASA's Jet Propulsion Laboratory will build and manage operations of the Mars 2020 rover for the NASA Science Mission Directorate at the agency's headquarters in Washington.For more information about the mission, go to https://mars.nasa.gov/mars2020/. | |
This image from NASA's Mars Odyssey shows part of the summit of Ceraunius Tholus. | Context imageThis VIS image shows part of the summit of Ceraunius Tholus.Orbit Number: 38703 Latitude: 24.0838 Longitude: 262.683 Instrument: VIS Captured: 2010-09-05 03:36Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
Extensional forces in the volcanic province of Tharsis, shown in this image from NASA's Mars Odyssey spacecraft, have produced a fractured terrain that resembles wrinkled skin. | Extensional forces in the volcanic province of Tharsis have produced a fractured terrain that resembles wrinkled skin.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Global Surveyor shows the landing site of Viking 2 in Utopia Planitia, west of Mie Crater on Mars on 3 September 1976. | Figure 1Figure 23 September 2006Viking 2 landed 30 years ago today, on 3 September 1976. It was the second of the two Viking landings on Mars. Viking 1 touched down on 20 July 1976. Since the Viking missions of the 1970s, only 3 additional spacecraft have successfully landed and conducted their scientific investigations: Mars Pathfinder (1997), Mars Exploration Rover Spirit (2004-present), and Mars Exploration Rover Opportunity (2004-present). Two new U.S. Mars landed missions are currently in the works: Phoenix, launching in August 2007, and MSL (Mars Science Laboratory), launching in 2009.As with the 30th anniversary of the Viking 1 landing in July (see PIA08616), for the Viking 2 30th anniversary, we show here the best Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) view of the landing site.On that day 30 years ago, Viking 2 landed in Utopia Planitia, west of Mie Crater, near 48.0°N, 225.7°W. At the time, it was considered that this might be a good place to look for evidence of life in the martian regolith. This middle north latitude site is often obscured by clouds in the winter and dust hazes in the spring. The surface was observed by the lander to be dusted by thin coatings of frost during the winter months.The exact location of the Viking 2 lander was uncertain until MOC obtained the high resolution view, shown above, in 2004. These images were previously released by the MOC team on 5 May 2005, along with what was then considered to be the best candidate for the Mars Polar Lander site (see "MGS Finds Viking 2 Lander and Mars Polar Lander (Maybe)"). The candidate Polar Lander site was further imaged in 2005 and found not to be the lander (see PIA03044).Figure 1 shows (A) a mosaic of Viking Orbiter images obtained in the 1970s at a resolution of 75 m/pixel, (B) a typical MGS MOC narrow angle camera view at about 3 meters/pixel (25x higher resolution than the Viking images), and (C, D) sections of a MOC image obtained at ~0.5 m/pixel. Figure 2 shows an extreme enlargement of the feature identified as Viking Lander 2, compared to a schematic drawing of the lander in the orientation determined during the Viking mission. | |
NASA's Mars Global Surveyor shows eroded remnants of layered sedimentary rock in northern Sinus Meridiani on Mars. The layering is seen in a circular meteor impact crater that was once filled and buried beneath the sedimentary rocks. | 19 November 2004This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows eroded remnants of layered sedimentary rock in northern Sinus Meridiani. The layering is best seen in the circular feature at the center/right, which is an old meteor impact crater that was once filled and buried beneath the sedimentary rocks, then later exhumed and eroded to its present state. All of the sedimentary rocks exposed in this portion of northern Sinus Meridiani are probably older than the rocks in central Sinus Meridiani that have been examined this year by the Mars Exploration Rover, Opportunity. Like the rocks visited by the rover, these, too, may contain detailed clues regarding a wetter Mars in the distant past. These landforms are located near 6.0°N, 2.0°W. The image covers an area approximately 3 km (1.9 mi) wide. Sunlight illuminates the scene from the left/lower left. | |
NASA's Mars Global Surveyor shows | MGS MOC Release No. MOC2-576, 16 December 2003The Cerberus Fossae are a series of long troughs and cracks that run southeastward from the Elysium volcanic region. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) picture shows a view looking down into two of the troughs. Dark specks in the troughs are boulders that have come loose from the walls and rolled to a stop on the floors. In recent years, some Mars scientists have speculated that the Cerberus Fossae troughs were the source of volcanic eruptions, and perhaps also the source of water that produced catastrophic floods. However, no evidence for either process is found at this particular location. The picture is located near 10.1°N, 202.0°W. The image covers an area 3 km (1.9 mi) wide; sunlight illuminates the scene from the lower left. | |
Individual dunes are seen on the floor of Arkhangelsky Crater in Noachis Terra by NASA's Mars Odyssey. | Context imageIndividual dunes exist on the floor of Arkhangelsky Crater in Noachis Terra.Orbit Number: 40860 Latitude: -40.5861 Longitude: 334.914 Instrument: VIS Captured: 2011-03-01 16:33Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Exploration Rover Opportunity used the wire brush of its rock abrasion tool to scour dust from a circular target area on a rock called 'Marquette Island.' | NASA's Mars Exploration Rover Opportunity used the wire brush of its rock abrasion tool during the rover's 2,070th Martian day, or sol (Nov. 19, 2009), to scour dust from a circular target area on a rock called "Marquette Island." The brushed target area, called "Peck Bay," is visible as a dark circle about 5 centimeters (2 inches) in diameter just below the tool turret at the end of the rover's robotic arm in this image. The image was taken later the same sol by the rover's front hazard-avoidance camera.Opportunity is performing an extensive analysis of this rock, which initial investigation suggests may be a stony meteorite. | |
This image shows the wall of a scuffmark NASA's Curiosity made in a windblown ripple of Martian sand with its wheel. The upper half of the image shows a small portion of the side wall of the scuff and a little bit of the floor of the scuff. | This image shows the wall of a scuffmark NASA's Curiosity made in a windblown ripple of Martian sand with its wheel. The upper half of the image shows a small portion of the side wall of the scuff and a little bit of the floor of the scuff (bottom of this image). The prominent depression with raised rims at the bottom center of the image was formed by one of the treads on Curiosity's front right wheel.The largest grains in this image are about 0.04 to 0.08 inches (1 to 2 millimeters) in size. Those large grains were on top of the windblown ripple and fell down to this location when the scuff was made. The bulk of the sand in the ripple is smaller, in the range below 0.002 to 0.008 inches (50 to 200 microns).The full scuffmark is 20 inches (50 centimeters) wide, which is the width of Curiosity's wheel. This image from the Mars Hand Lens Imager (MAHLI) is the product of merging eight images acquired at eight slightly different focus settings to bring out details on the wall, slopes, and floor of the wheel scuff. The merge was performed onboard the MAHLI instrument to reduce downlinked data volume. The image was acquired by MAHLI with the lens about 4.7 inches (12 centimeters) from the target. The pixel scale is about 0.002 inches (50 microns) per pixel. The image covers an area, roughly 3 by 2 inches (8 by 6 centimeters). The image was obtained on Oct. 4, 2012, or sol 58, the 58th Martian day of operations on the surface.JPL manages the Mars Science Laboratory/Curiosity for NASA's Science Mission Directorate in Washington. The rover was designed, developed and assembled at JPL, a division of the California Institute of Technology in Pasadena.For more about NASA's Curiosity mission, visit: http://www.jpl.nasa.gov/msl, http://www.nasa.gov/mars, and http://marsprogram.jpl.nasa.gov/msl. | |
This image from NASA's 2001 Mars Odyssey released on Jan 13, 2004 shows the western side of Gusev crater, the landing site of Mars Exploration Rover Spirit. | Released 13 January 2004Long before the MER landers were named or launched, the two orbiters at Mars were asked to examine landing sites. Both the Odyssey and Mars Global Surveyor spacecraft have been collecting landing site data for the past two years. The MGS and ODY data were used as part of the decision making process in the final selection of the two landing sites. The types of data collected by the two orbiters included not only images of the surface but also thermal data about the surface composition, atmospheric data about the climate at each location, and the tracking of major dust storms in the region prior to landing. The presence of, and data collected by, the MGS and ODY orbiters have proven invaluable in MER mission planning.This image, the infrared counterpart to this visual image, covers the western side of Gusev crater.Image information: IR instrument. Latitude -12.3, Longitude 175 East (185 West). 100 meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows Lycus Sulci, a broad tectonic terrain that surrounds the western and northern parts of Olympus Mons. Dark slope streaks and wind erosion in valleys are typical in Lycus Sulci. | Context image for PIA11296Lycus SulciLycus Sulci is a broad tectonic terrain that surrounds the western and northern parts of Olympus Mons. Dark slope streaks and wind erosion in valleys are typical in Lycus Sulci.Image information: VIS instrument. Latitude 21.3N, Longitude 215.3E. 19 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Perseverance Mars rover captured this scene at a location nicknamed Skrinkle Haven using its Mastcam-Z camera between Feb. 28 and March 9, 2023. | Figure AMain image - maximum resolution version, 43783 x 14997 pixels (152 MB)Figure A image - maximum resolution version, 43783 x 14997 pixels (236 MB)Scientists think that the bands of rocks seen in this image may have been formed by a very fast, deep river – the first of its kind evidence has been found for on Mars. NASA's Perseverance Mars rover captured this mosaic at a location nicknamed "Skrinkle Haven" using its Mastcam-Z camera between Feb. 28 and March 9, 2023 (between the 721st and 729th Martian days, or sols, of the mission). The mosaic is made up of 203 individual images that were stitched together after being sent back from Mars. This natural color view is approximately how the scene would appear to an average person if they were on Mars.Figure A is an enhanced color view that exaggerates subtle color differences in the scene."Skrinkle Haven" offers the clearest example of these curved rock layers – called "the curvilinear unit" – that had previously only been seen from space. Scientists are now debating what kind of powerfully flowing water formed those curves: a river like the Mississippi, which winds snakelike across the landscape, or a braided river like Nebraska's Platte, which forms small islands of sediment called sandbars.When viewed from the ground, the curved layers are arranged in rows, and appear to ripple out across the landscape. They could be the remnants of a river's banks that shifted over time – or the remnants of sandbars that formed in the river. The layers were likely much taller in the past; scientists suspect that after these piles of sediment turned to rock, they were sand-blasted by wind over the course of eons and carved down to their present size.Arizona State University leads the operations of the Mastcam-Z instrument, working in collaboration with Malin Space Science Systems in San Diego, on the design, fabrication, testing, and operation of the cameras, and in collaboration with the Niels Bohr Institute of the University of Copenhagen on the design, fabrication, and testing of the calibration targets.A key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith (broken rock and dust).Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.The Mars 2020 Perseverance mission is part of NASA's Moon to Mars exploration approach, which includes Artemis missions to the Moon that will help prepare for human exploration of the Red Planet.NASA's Jet Propulsion Laboratory, which is managed for the agency by Caltech in Pasadena, California, built and manages operations of the Perseverance rover.For more about Perseverance:mars.nasa.gov/mars2020/ | |
Two Southern Hemisphere Craters | This HiRISE image (PSP_001750_1425) shows two southern hemisphere craters. These craters are about the same size, approximately 800-900 meters in diameter, and appear to have experienced parallel histories. Both craters show dunes and gullies with similar orientations.Several generations of dunes can be seen in the interior of these craters. The largest barchan dunes trend northwest-southeast with their slip faces facing the southeast, indicating that the winds forming them came from the northwest.There are smaller dunes that superpose the large dunes with a different orientation. Different dune orientations are a sign of a changing dominant wind direction. Both craters have similar dune orientations, which is expected because of their proximity.The two craters also both have gullies originating at layers on their south-facing walls. The gullies are mostly in shadow, but adjusting the brightness and contrast of the image allows them to be seen (see subimage). The subimage is approximately 300 meters across and shows the gullies in the crater on the right. Gullies are thought to form by liquid water flowing down slopes, but the source of the water and how it is involved in gully erosion is often debated. One theory proposes that near-surface ground ice melts to form the gullies. An important part of this theory is the direction and amount of insolation (sunlight) a slope receives. Since these craters are close to each other, they receive similar insolation, which could explain why the gullies are in the same location in them. Another theory suggests that subsurface water from an aquifer forms the gullies. If an extensive aquifer existed, it would flow downslope. If the regional slope trends towards the south, that could explain why the gullies are where they are (the water would come from behind the slope to form the gullies).HiRISE is showing us unprecedented details of the gullies and will no doubt bring us closer to understanding how these mysterious features form.Observation Toolbox Acquisition date: 12 December 2006Local Mars time: 3:40 PMDegrees latitude (centered): -37.2°Degrees longitude (East): 194.2°Range to target site: 253.6 km (158.5 miles)Original image scale range: 25.4 cm/pixel (with 1 x 1 binning) so objects ~76 cm across are resolvedMap-projected scale: 25 cm/pixel and north is upMap-projection: EQUIRECTANGULAREmission angle: 6.2°Phase angle: 77.1°Solar incidence angle: 72°, with the Sun about 18° above the horizonSolar longitude: 148.4°, Northern SummerNASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. | |
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 captured by NASA's 2001 Mars Odyssey spacecraft shows part of Coprates Chasma. | Context imageThe 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 Coprates Chasma. The blue tone over the lower elevation of the chasma may indicate atmospheric haze.Orbit Number: 1838 Latitude: -11.5884 Longitude: 295.298 Instrument: VIS Captured: 2002-05-14 20:28Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This portion of an image from NASA's Mars Reconnaissance Orbiter has been annotated to show the relative positions between NASA's Curiosity rover (right) and the impact site of its sky crane, or descent stage. | This portion of an image from the High Resolution Imaging Science Experiment (HiRISE) on NASA's Mars Reconnaissance Orbiter has been annotated to show the relative positions between NASA's Curiosity rover (right) and the impact site of its sky crane, or descent stage. The azimuth from north of the rover is about 290 degrees (north is up and zero degrees).
This information was used to determine whether the rover was pointed in the right direction to have captured an image of the plume from the crash of the descent stage using its rear-facing Hazard-Avoidance cameras. The gyrocompass on Curiosity indicates that the rover is pointed at 112 degrees, which, after subtracting 180 degrees since the picture was taken from the rear, gives the same direction of the sky crane crash to within 2 degrees.
HiRISE is one of six instruments on NASA's Mars Reconnaissance Orbiter. The University of Arizona, Tucson, operates the orbiter's HiRISE camera, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, built the spacecraft. | |
Spirit Tracks on Mars, Sol 151 (Left Eye) | This is the left-eye half of a stereo pair of 360-degree views assembled from frames taken by the navigation camera on NASA's Mars Exploration Rover Spirit during Spirit's 151st martian day, or sol, on Junr 5, 2004. The view is presented in a cylindrical-perspective projection with geometric seam correction. The rover sits at site 63, still more than 100 meters (328 feet) from the base of the "Columbia Hills." As suggested by the rover tracks fading off in the distance, Spirit made great progress on this sol, roving 73 meters (240 feet) to get to this point.See PIA06053 for 3-D view and PIA06055 for right eye view of this left eye cylindrical-perspective projection. | |
NASA's Mars Global Surveyor shows a ridged mound that was first seen and informally named 'White Rock' located in Pollack Crater on Mars. | "White Rock" is a ridged mound that was first seen and informally named "White Rock" in pictures from the Mariner 9 orbiter in 1972. In black-and-white photos, the feature appears much brighter than its surrounding terrain, giving the impression that the material is white. Later analyses of Mariner 9, Viking, and Mars Global Surveyor (MGS) data showed that the feature isn't actually white, it is somewhat red and reflects only about 20-25% of the sunlight that falls upon it (a white surface would reflect 100%).Located in Pollack Crater, a 95 km (59 mile) wide impact basin at 7.9°S, 334.7°W, White Rock is the light-red/orange feature with the rectangular white box drawn on it in the context view above. The white box indicates the location of a sub-frame of a MGS Mars Orbiter Camera (MOC) image acquired in September 2000, shown in PIA02848. The light-toned material that gives White Rock its name forms steep cliffs with valleys between them covered by dark, windblown, rippled sand. This release image shows a close-up of a portion of PIA02848, illustrating that the bright material is layered (arrow, "layers") and that there is an old impact crater (arrow, "crater") that has been partly uncovered from beneath the White Rock material.The layering in White Rock suggests that the material is sediment deposited at some time in the distant past within Pollack Crater. The fact that the material erodes to form steep cliffs suggests that it is hard like rock. Thus, White Rock is interpreted to be an outcrop of sedimentary rock. It is probably a small remnant of a larger body of rock that may have once covered the entire floor of Pollack Crater; this view is supported by the observation that more extensive layered rocks are seen in other craters across the surface of the red planet (e.g., the crater at 8°N, 7°W).Both pictures shown here are illuminated by sunlight from the upper left, north is up. Pollack Crater was named in 1997 for James B. Pollack (1938-1994), a NASA Ames Research Center scientist known in the Mars research community for his atmospheric research with Mariner 9 and Viking data and the development of key computer models used to investigate the red planet's winds, storms, and climate. | |
This diagram illustrates how the Dynamic Albedo of Neutrons (DAN) instrument on NASA's Curiosity Mars rover detects hydrogen in the ground beneath the rover. | This diagram and the one at PIA16917 illustrate how the Dynamic Albedo of Neutrons (DAN) instrument on NASA's Curiosity Mars rover detects hydrogen in the ground beneath the rover. Detected hydrogen is interpreted as hydroxyl groups or water molecules, such as those bound into the structure of hydrated minerals. DAN shoots neutrons into the ground and measures the timing and energy levels of neutrons reflected back up. This diagram depicts the case of a neutron that does not collide with any hydrogen atoms before it reaches DAN's detector. It is detected in a characteristically short time -- about one millisecond -- after being emitted by DAN's neutron generator, and with a characteristic energy. The companion diagram illustrates the case of a neutron that does collide with hydrogen in the ground. Russia's Space Research Institute, in Moscow, developed the DAN instrument in close cooperation with the N.L. Dukhov All-Russia Research Institute, Moscow, and the Joint Institute of Nuclear Research, Dubna.NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the rover. More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
NASA's Mars Global Surveyor shows a wide angle view of the giant martian volcano, Olympus Mons. | MGS MOC Release No. MOC2-479, 10 September 2003This is a red camera wide angle view of the giant martian volcano, Olympus Mons, acquired by the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC). The volcano is large enough to cover much of the U.S. state of New Mexico. This view was taken looking west toward the sunward limb of the planet. The limb is the horizon to the left; the dark band is outer space. Sunlight illuminates this scene from the lower left. |
Subsets and Splits