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This image graphs four gases released ('evolved') when powdered rock from the target rock 'Cumberland' was heated inside the Sample Analysis at Mars (SAM) instrument suite on NASA's Curiosity Mars rover. | This image graphs four gases released ("evolved") when powdered rock from the target rock "Cumberland" was heated inside the Sample Analysis at Mars (SAM) instrument suite on NASA's Curiosity Mars rover. The data come from the second Cumberland sample analyzed by SAM. The released gases were detected by SAM's quadrupole mass spectrometer. The graphic shows four gases (oxygen, hydrochloric acid, carbon dioxide, and nitric oxide) evolved.The mass spectrometer signal for each gas is scaled separately so that the same graph can illustrate the temperatures that caused the gas to be released (for example, nitric oxide, NO, has been scaled up 25 times). These evolved gases and the temperatures at which they evolved suggest the presence of oxychlorine compounds, such as perchlorates, and of carbon- and nitrogen-bearing components in the rock-powder sample. The Cumberland target rock is in the "Yellowknife Bay" area of Mars' Gale Crater.NASA's Jet Propulsion Laboratory, Pasadena, Calif., manages the Mars Science Laboratory Project and the mission's Curiosity rover for NASA's Science Mission Directorate in Washington. The rover was designed and assembled at JPL, a division of the California Institute of Technology in Pasadena.More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
This image of 'Neopolitan' from NASA's Mars Exploration Rover Opportunity's 'Eagle Crater' soil survey highlights the border between two different soil types, a lighter, finer-grained unit to the left and a darker, coarser-grained to the right. | Figure 1 (close-up)This panoramic camera image of the soil target whimsically called "Neopolitan" from the Mars Exploration Rover Opportunity's "Eagle Crater" soil survey highlights the border between two different soil types - a lighter, finer-grained unit to the left and a darker, coarser-grained to the right. Scientists are pondering the unusually distinct border between these different soil types. To the lower left and partially hidden by the shadow of the mast is an airbag bounce mark. | |
NASA's Mars Global Surveyor shows a small meteor impact crater with a bright wind streak on its left side. These landforms are located in eastern Kasei Valles on Mars. | 6 November 2004This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a small meteor impact crater (approximately the size of the famous Meteor Crater in northern Arizona) with a bright wind streak on its west (left) side. Generally, winds blowing from the east (right) have stripped away bright dust everywhere but in the lee of the crater. These landforms are located in eastern Kasei Valles near 25.1°N, 60.8°W. The picture covers an area about 3 km (1.9 mi) wide. Sunlight illuminates the scene from the left/lower left. | |
This image from NASA's Mars Odyssey shows part of the floor of Herschel Crater. | Context imageThis false color image shows part of the floor of Herschel Crater.The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image.Orbit Number: 63542 Latitude: -15.0758 Longitude: 131.164 Instrument: VIS Captured: 2016-04-10 20:15Please 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 shows the southwestern flank of Apollinaris Patera, an old volcano on Mars that has undergone extensive erosion. | Context image for PIA09986Another ApollinarisThe major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Today's image shows the southwestern flank of the volcano.Image information: VIS instrument. Latitude -9.2N, Longitude 173.5E. 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. | |
Newly detailed mapping of local variations in Mars' gravitational pull on orbiters (center), combined with topographical mapping of the planet's mountains and valleys (left) yields the best-yet mapping of Mars' crustal thickness (right). | Newly detailed mapping of local variations in Mars' gravitational pull on orbiters (center), combined with topographical mapping of the planet's mountains and valleys (left) yields the best-yet mapping of Mars' crustal thickness (right). These three views of global mapping are centered at 90 degrees west longitude, showing portions of the planet that include tall volcanoes on the left and the deep Valles Marineris canyon system just right of center. Additional views of these global maps are available at http://svs.gsfc.nasa.gov/goto?4436.The new map of Mars' gravity (center) results from analysis of the planet's gravitational effects on orbiters passing over each location on the globe. The data come from many years of using NASA's Deep Space Network to track positions and velocities of NASA's Mars Global Surveyor, Mars Odyssey and Mars Reconnaissance Orbiter. If Mars were a perfectly smooth sphere of uniform density, the gravity experienced by the spacecraft would be exactly the same everywhere. But like other rocky bodies in the solar system, including Earth, Mars has both a bumpy surface and a lumpy interior. As the spacecraft fly in their orbits, they experience slight variations in gravity caused by both of these irregularities, variations which show up as small changes in the velocity and altitude of the three spacecraft.The "free-air" gravity map presents the results without any adjustment for the known bumpiness of Mars' surface. Local gravitational variations in acceleration are expressed in units called gals or galileos. The color-coding key beneath the center map indicates how colors on the map correspond to mGal (milligal) values. The map on the left shows the known bumpiness, or topography, of the Martian surface, using data from the Mars Orbiter Laser Altimeter (MOLA) instrument on Mars Global Surveyor. Mars has no actual "sea level," but does have a defined zero elevation level. The color-coding key beneath this map indicates how the colors correspond to elevations above or below zero, in kilometers.Analysis that subtracts effects of the surface topography from the free-air gravity mapping, combined with an assumption that crust material has a uniform density, leads to the derived mapping of crustal thickness -- or subsurface "lumpiness" -- on the right. Highs in gravity indicate places where the denser mantle material beneath the crust is closer to the surface, and hence where the crust is thinner. The color-coding key for this map indicates how the colors on the map correspond to the thickness of the crust, in kilometers. | |
This image captured by NASA's 2001 Mars Odyssey shows just one of many lava channels located on the Elysium Mons volcanic complex. | Context imageThis VIS image shows just one of many lava channels located on the Elysium Mons volcanic complex.Orbit Number: 37247 Latitude: 13.2645 Longitude: 145.744 Instrument: VIS Captured: 2010-05-08 06:21Please 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. | |
Way to Go Spirit! | This image taken by the front hazard-avoidance camera on the Mars Exploration Rover Spirit demonstrates that the rover successfully completed its second, five-wheeled drive over a distance of 3 meters (9.8 feet). The rover has now traveled a total of 10 meters (32.8 feet) in this fashion. Because Spirit's right front wheel has been showing signs of wear, rover planners will drive it backwards on its remaining five wheels. The sixth wheel will be activated only when it is needed to surmount more demanding terrain. This picture was taken on July 15, 2004, and shows the view from behind the backward-facing rover. | |
This image from NASA's Mars Odyssey shows part of the inner rim of an unnamed crater in Terra Sabaea. | Context imageThis VIS image shows part of the inner rim of an unnamed crater in Terra Sabaea. Numerous dark streaks mark the slopes of the inner rim. There are several suggested mechanisms to form these features. Two of the mechanisms are that the dusty surface has been altered to reveal darker rock beneath from motion of downward moving dust, or the surface is darkening by fluid or other surface staining.Orbit Number: 79499 Latitude: 10.6116 Longitude: 36.6442 Instrument: VIS Captured: 2019-11-16 06:26Please 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 January 20, 2021 by NASA's Mars Reconnaissance Orbiter, shows dark slope streaks, common on steep dust-mantled slopes of Mars. | Map Projected Browse ImageClick on image for larger versionRelatively dark slope streaks are common on steep dust-mantled slopes of Mars. When imaged under high sun illumination they appear to be just a dark stain without topographic relief.However, when imaged with the sun low in the sky (and at high resolution), we can clearly see the topographic signature. Surface material has been removed from the upper slopes and deposited in lobes, as expected from landslides (also called "mass movements").The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. (The original image scale is 27.7 centimeters [10.9 inches] per pixel [with 1 x 1 binning]; objects on the order of 83 centimeters [32.7 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. | |
NASA's Mars Global Surveyor shows a wind ripple-filled trough, a fracture in a rugged and pitted plain, located northwest of Kasei Valles in the Nilus Chaos region of Mars. | 20 April 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a wind ripple-filled trough, a fracture in a rugged and pitted plain, located northwest of Kasei Valles in the Nilus Chaos region.Location near: 26.3°N, 78.8°W Image width: ~3 km (~1.9 mi) Illumination from: lower left Season: Northern Summer | |
This view from NASA's Curiosity rover of the downwind face of 'Namib Dune' on Mars covers 360 degrees, including a portion of Mount Sharp on the horizon. The site is part of the dark-sand 'Bagnold Dunes' field along the northwestern flank of Mount Sharp. | This view of the downwind face of "Namib Dune" on Mars covers 360 degrees, including a portion of Mount Sharp on the horizon. The site is part of the dark-sand "Bagnold Dunes" field along the northwestern flank of Mount Sharp. Images taken from orbit indicate that dunes in the Bagnold field move as much as about 3 feet (1 meter) per Earth year.The component images of this scene were taken on Dec. 18, 2015, by the Mast Camera (Mastcam) on NASA's Curiosity Mars rover during the 1,197th Martian day, or sol, of the rover's work on Mars. The bottom of the dune nearest the rover is about 23 feet (7 meters) from the camera. This downwind face of the dune rises at an inclination of about 28 degrees to a height of about 16 feet (5 meters) above the base. The center of the scene is toward the east; both ends are toward the west.A color adjustment has been made approximating a white balance, so that rocks and sand appear approximately as they would appear under Earth's sunlit sky. A brightness adjustment accommodates including rover hardware in the scene.The mission's examination of dunes in the Bagnold field, along the rover's route up the lower slope of Mount Sharp, is the first close look at active sand dunes anywhere other than Earth.Malin Space Science Systems, San Diego, built and operates the rover's Mastcam. 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 project's Curiosity rover.For more information about Curiosity, visit http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/.Photojournal Note: Also available is the full resolution TIFF file PIA20284_full.tif. This file may be too large to view from a browser; it can be downloaded onto your desktop by right-clicking on the previous link and viewed with image viewing software. | |
NASA's InSight spacecraft flipped open the lens cover on its Instrument Context Camera (ICC) on Nov. 30, 2018, and captured this view of Mars. | NASA's InSight spacecraft flipped open the lens cover on its Instrument Context Camera (ICC) on Nov. 30, 2018, and captured this view of Mars. Located below the deck of the InSight lander, the ICC has a fisheye view, creating a curved horizon. Some clumps of dust are still visible on the camera's lens. One of the spacecraft's footpads can be seen in the lower right corner. The seismometer's tether box is in the upper left corner.JPL manages InSight for NASA's Science Mission Directorate. InSight is part of NASA's Discovery Program, managed by the agency's Marshall Space Flight Center in Huntsville, Alabama. Lockheed Martin Space in Denver built the InSight spacecraft, including its cruise stage and lander, and supports spacecraft operations for the mission.A number of European partners, including France's Centre National d'Études Spatiales (CNES) and the German Aerospace Center (DLR), are supporting the InSight mission. CNES, and the Institut de Physique du Globe de Paris (IPGP), provided the SEIS instrument, with significant contributions from the Max Planck Institute for Solar System Research (MPS) in Germany, the Swiss Institute of Technology (ETH) in Switzerland, Imperial College and Oxford University in the United Kingdom, and JPL. DLR provided the HP3 instrument, with significant contributions from the Space Research Center (CBK) of the Polish Academy of Sciences and Astronika in Poland. Spain's Centro de Astrobiología (CAB) supplied the wind sensors.For more information about the mission, go to https://mars.nasa.gov/insight. | |
This image from NASA's Mars Odyssey shows a short section of Reull Vallis. Reull Vallis starts in Promethei Terra and empties into Hellas Plainitia. | Context imageThis VIS image shows a short section of Reull Vallis. Reull Vallis starts in Promethei Terra and empties into Hellas Plainitia. On the floor of this channel are ridged and grooved materials. In other sections of the channel these materials appear to deflect around obstacles. These features are proposed to be ice-rich materials similar to glaciers on Earth. Reull Vallis is 1051km (653 miles) long.Orbit Number: 91570 Latitude: -41.1029 Longitude: 108.157 Instrument: VIS Captured: 2022-08-06 03:34Please 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 linear depressions, part of Sirenum Fossae. | Context imageThe linear depressions in this VIS image are part of Sirenum Fossae. These depressions are called graben, which form by the down drop of material between two parallel faults. The faults are caused by tectonic stresses in the region. The Sirenum Fossae graben are 2735km (1700 miles) long.Orbit Number: 83493 Latitude: -32.8399 Longitude: 204.159 Instrument: VIS Captured: 2020-10-10 02:18Please 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 full-circle panorama of the landscape surrounding NASA's Curiosity Mars rover on July 31, 2014, offers a view into sandy lower terrain called 'Hidden Valley.' | This panorama of the landscape surrounding NASA's Curiosity Mars rover on July 31, 2014, offers a view into sandy lower terrain called "Hidden Valley," which is on the planned route ahead. The full-circle vista combines several images taken by Curiosity's Navigation Camera in the afternoon of the mission's 705th Martian day, or sol, after completion of Sol 705's drive of about 16 feet (4.9 meters). South is at the center, north at both ends. For the preceding few weeks, Curiosity had been crossing a plateau studded with embedded, sharp rocks. The planned route ahead from this Sol 705 location takes the rover southwestward through Hidden Valley, across sandier ground. The valley is about 150 feet (about 45 meters) wide. For a map showing this area, see PIA18408.For scale, the distance between Curiosity's parallel wheel tracks entering the scene near the left edge is about 9 feet (2.7 meters). The panorama is presented here as a cylindrical projection.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 project's Curiosity rover and the rover's Navcam. | |
NASA's Perseverance captured this image of a sample it cored on June 12. The core shows distinctly colored areas that are individual minerals transported by a river that once flowed into Jezero Crater. | NASA's Perseverance Mars rover captured this image of a rock core nicknamed "Otis Peak" on June 12, 2023, the 822nd day, or sol, of the mission. The image shows the bottom of the Otis Peak core, which was collected from a conglomerate rock called "Emerald Lake." The distinctly colored areas are individual minerals (or rock fragments) transported by the river that once flowed into Mars' Jezero Crater. The image was taken by Perseverance's Sampling and Caching System Camera, or CacheCam, located inside the rover underbelly. The camera looks down into the top of a sample tube to take close-up pictures of the sampled material and the tube as it's prepared for sealing and storage.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 in Southern California built and manages operations of the Mars 2020 Perseverance rover for NASA.For more information about the mission, go to:https://mars.nasa.gov/mars2020 | |
Heading for Next Winter Haven | Approaching its 47th month of a Mars surface mission originally planned to last three months, NASA's Spirit rover was also approaching the northern edge of a low plateau called "Home Plate." The rover's operators selected an area with north-facing slope there as a destination where Spirit would have its best chance of surviving low-solar-energy conditions of oncoming Martian winter.The yellow line on this map of the Home Plate area indicates Spirit's route from early February 2006, entering the mapped area from the north (top), to late November 2007, on the western edge of the bright-toned Home Plate plateau. The map covers an area about 160 meters (525 feet) across from west to east. Labels indicate the area intended for Spirit to spend many months spanning the rover's third Martian winter, the site where it spent about seven months (April to November 2006) spanning its second winter, and the site where it lost use of the drive motor for one of its six wheels.A north-facing slope helps Spirit maximizes electric output from its solar panels during winter months because Spirit is in the southern hemisphere of Mars, so the sun appears only in the northern sky during winter. For the third winter, which will reach its minimum solar-energy days in early June 2008, Spirit faces the challenge of having more dust on its solar panels than it had during its second winter.The base image for this map is a portion of a color image taken on Jan. 9, 2007, by the High Resolution Imaging Science Experiment camera on NASA's Mars Reconnaissance Orbiter. | |
The relatively young Canala Crater and its ejecta overlie the tectonic structures of Labeatis Fossae as seen by NASA's 2001 Mars Odyssey spacecraft. | Context imageThe relatively young Canala Crater and its ejecta overlie the tectonic structures of Labeatis Fossae.Orbit Number: 44281 Latitude: 24.139 Longitude: 279.958 Instrument: VIS Captured: 2011-12-08 09:17Please 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. | |
Long linear ridges and grooves curve, wave, and buckle across most of this image from NASA's 2001 Mars Odyssey spacecraft. | Map Projected Browse ImageClick on the image for larger versionLong linear ridges and grooves curve, wave, and buckle across most of this image. Here, as elsewhere on Mars, these linear ridges and grooves fill a valley floor, hence their name, "lineated valley fill."Because these features are only found in valleys in the middle latitudes (30 to 60 degrees) of the Northern and Southern hemispheres, scientists had long suspected that they were associated with some ancient climate that had prevailed in that latitudinal band. Based on peering beneath the surface using radar, scientists now think that lineated valley fill is probably merely a rocky veneer atop a glacier of nearly pure ice! The rocks that make up the linear ridges and grooves were oriented by the ancient flow of the glacier underneath.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 the NASA Science Mission Directorate, Washington. | |
NASA's Mars Global Surveyor shows exposures of layered material on slopes in the south polar region on Mars. | 4 June 2004This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows exposures of layered material on slopes in the south polar region near 81.9°S, 72.2°W. Layers record the history of a place, but accessing the information contained in these layers may one day require a visit by a human or robotic explorer. The south polar layers, in general, are believed to be accumulations of dust and ice that were built up in the most recent billion years or so. However, they could just as easily be sedimentary rocks from much earlier in martian history. The picture covers an area about 3 km (1.9 mi) across. The scene is illuminated by sunlight from the upper left. | |
Northern Plains | Image PSP_001422_2465 was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on November 15, 2006. The complete image is centered at 66.0 degrees latitude, 125.0 degrees East longitude. The range to the target site was 315.1 km (196.9 miles). At this distance the image scale is 31.5 cm/pixel (with 1 x 1 binning) so objects ~95 cm across are resolved. The image shown here has been map-projected to 25 cm/pixel. The image was taken at a local Mars time of 3:02 PM and the scene is illuminated from the west with a solar incidence angle of 57 degrees, thus the sun was about 33 degrees above the horizon. At a solar longitude of 135.7 degrees, the season on Mars is Northern Summer.NASA'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, acquired by NASA's Mars Reconnaissance Orbiter, shows the rover Opportunity perched on the edge of 'Concepción' crater, a fresh crater with dark rays that clearly overprint the north-trending, wind-shaped ripples, in Meridiani Planum. | This image shows NASA's Mars Exploration Rover Opportunity perched on the edge of "Concepción" crater in Meridiani Planum, Mars. The image was acquired by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter on February 13, 2010, during the 2,153rd Martian day, or sol, of Opportunity's mission on Mars.Concepción crater is a fresh crater, 10 meters (33 feet) in diameter, with dark rays that clearly overprint the north-trending, wind-shaped ripples. North is toward the top. The rover is at the one o'clock position beside the crater. The superimposed arrow in Figure 1 points to the rover. Mid-afternoon sunshine illuminates the scene from the left.The dark rays are produced by shadows cast by blocky ejecta -- material thrown outward by the impact that excavated the crater. The presence of the rays and similar relationships with other fresh craters in Meridiani Planum indicate that this is likely the youngest crater visited by any rover on Mars (estimated to have resulted from an impact thousands to tens of thousands of years ago).Note rover tracks in ripples to the north and northwest of the rover. The rover team uses these high-resolution images (about 25 centimeters or one foot per pixel) to help navigate the rover. In addition, exploring areas with the rover covered by such high-resolution images provides "ground truth" for the orbital observations. This view covers a small portion of HiRISE observation ESP_016644_1780.The University of Arizona, Tucson, operates the 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, Pasadena, manages the Mars Reconnaissance Orbiter for the NASA Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. | |
In this image from NASA's Mars Reconnaissance Orbiter, lower wall rock spurs are found that spread dark materials onto a dune field, suggesting local wall materials are a nearby sediment source for dunes. | Map Projected Browse ImageClick on the image for larger versionIn this image, lower wall rock spurs are found that spread dark materials onto a dune field, suggesting local wall materials are a nearby sediment source for dunes. This subimage shows the interface between wall materials and dunes in the northwest portion of the main image.Dune sand, wall spurs, and boulders are all partially composed of olivine (according to CRISM data), a common mineral formed in volcanic processes, supporting the notion for local sourcing of dunes.Olivine is highly susceptible to weathering by aqueous processes indicating these dunes and the wall debris formed after any such activity. Interestingly, clay minerals (known as phyllosilicates) are detected farther up the wall suggesting that aqueous alteration of wall materials has occurred in the ancient past.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 the NASA Science Mission Directorate, Washington. | |
The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows windstreaks on the floor of Gusev Crater. | 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 windstreaks on the floor of Gusev Crater.Orbit Number: 3415 Latitude: -14.1644 Longitude: 175.424 Instrument: VIS Captured: 2002-09-21 16:02Please 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 its 256th orbit of Mars, the camera on-board NASA's Mars Global Surveyor spacecraft successfully observed the vicinity of the Mars Pathfinder landing site. 3D glasses are necessary to identify surface detail. | On its 256th orbit of Mars, the camera on-board the Mars Global Surveyor spacecraft successfully observed the vicinity of the Pathfinder landing site. The images shown are a stereoscopic image pair in anaglyph format, made from the overlapping area of MOC 25603 and 23703. This image is reproduced at a scale of 5 m (16.4 feet) per pixel. Image 23703 was acquired on 13 April at 7:50 AM PDT; Image 25603 was acquired on 22 April at 1:11 PM PDT. The P237 observation was made from a distance of 675 km while the P256 measurement was made from 800 km. The viewing angle for 23703 was 21.2°, for 25603, 30.67°, giving an angular difference of about 9.5°. Owing to the relief on "Big Crater," this relatively small angular difference was in this case sufficient to show good stereo parallax.The resolution of the MOC image that covered the Pathfinder landing site (MOC 25603) was about 3.3 m or 11 feet per pixel. The Pathfinder lander and airbags form a roughly equilateral triangle 5 m on a side. Noting that the camera has not yet been focussed (it needs to be in the stable temperature conditions of the low altitude, circular mapping orbit in order to achieve best focus) and the hazy atmospheric conditions, the effective scale of the image is probably closer to 5 m (16.4 feet). Thus, the scale of the image was insufficient to resolve the lander (more than one pixel is needed to resolve a feature). In addition, the relatively high sun angle of the image (the sun was 40° above the horizon) reduced the length of shadows (for example, only a few boulders are seen), also decreasing the ability to discriminate small features. Work continues to locate intermediate-scale features in the lander and orbiter images in the hope of identifying the precise landing site based on these comparisons.Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. | |
This scene from NASA's Mars Odyssey spacecraft shows several interesting geologic features associated with impact craters on Mars. | Today marks the 45th anniversary of the dawn of the Space Age (October 4, 1957). On this date the former Soviet Union launched the world's first satellite, Sputnik 1. Sputnik means fellow traveler. For comparison Sputnik 1 weighed only 83.6 kg (184 pounds) while Mars Odyssey weighs in at 758 kg (1,671 pounds).This scene shows several interesting geologic features associated with impact craters on Mars. The continuous lobes of material that make up the ejecta blanket of the large impact crater are evidence that the crater ejecta were fluidized upon impact of the meteor that formed the crater. Volatiles within the surface mixed with the ejecta upon impact thus creating the fluidized form. Several smaller impact craters are also observed within the ejecta blanket of the larger impact crater giving a relative timing of events. Layering of geologic units is also observed within the large impact crater walls and floor and may represent different compositional units that erode at variable rates. Cliff faces, dissected gullies, and heavily eroded impact craters are observed in the bottom half of the image at the terminus of a flat-topped plateau.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 Phoenix Mars Lander shows flat ground strewn with tiny pebbles and marked by small-scale polygonal cracking, a pattern seen widely in Martian high latitudes. | This image, one of the first captured by NASA's Phoenix Mars Lander, shows flat ground strewn with tiny pebbles and marked by small-scale polygonal cracking, a pattern seen widely in Martian high latitudes and also observed in permafrost terrains on Earth. The polygonal cracking is believed to have resulted from seasonal contraction and expansion of surface ice.Phoenix touched down on the Red Planet at 4:53 p.m. Pacific Time (7:53 p.m. Eastern Time), May 25, 2008, in an arctic region called Vastitas Borealis, at 68 degrees north latitude, 234 degrees east longitude.This image was acquired at the Phoenix landing site by the Surface Stereo Imager on day 1 of the mission on the surface of Mars, or Sol 0, after the May 25, 2008, landing. 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 acquired on December 21, 2019 by NASA's Mars Reconnaissance Orbiter, shows the boundary between north polar ice and nearby polar sand dunes. | Map Projected Browse ImageClick on image for larger versionThis image covers the boundary between north polar ice and nearby polar sand dunes. The color data clearly distinguishes between the bright ice, dark sand, and reddish dust. An animation compares an exact same area to how it appeared in March 2009 at the same Martian time of year. The dark sand appears to be on the move, covering much of this area that was formerly bright ice or dust-covered ice. However, this may also show year-on-year variability of seasonal processes. In other words, this area may have looked similar in 2009 a month or so after the HiRISE image was acquired. The seasonal defrosting patterns vary from year to year, perhaps depending on dust storm activity. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. (The original image scale is 31.9 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, 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 one of the many channel forms found radial to the Elysium Mons volcanic complex. | Context imageToday's VIS image contains a section of one of the many channel forms found radial to the Elysium Mons volcanic complex. In this case the fossae are located to the west of Elysium Mons. Elysium Fossae are comprised of both linear and sinuous channels, usually interpreted to have both fluid and tectonic forces playing a part in the formation. The linear depression resembles a graben (formed by tectonic forces) and sinuous channels more closely resembles features caused by fluid flow – either lava or water created by melting subsurface ice due to volcanic heating. The Elysium Fossae system is 1044 km (649 miles) in length.Orbit Number: 93983 Latitude: 27.1871 Longitude: 142.629 Instrument: VIS Captured: 2023-02-20 20:54Please 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 several of the graben that make up Ceraunius Fossae. | Context imageToday's VIS image shows several of the graben that make up Ceraunius Fossae. These fault bounded valleys are located south of Alba Mons and are part of the extensive graben system that surround this large volcano.Orbit Number: 62103 Latitude: 34.4816 Longitude: 249.2 Instrument: VIS Captured: 2015-12-14 08:05Please 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 Ingenuity Mars Helicopter took this image with its color camera from beneath the Perseverance rover after the rover had deployed the rotorcraft to the surface of Mars. Image was taken on April 3, 2021. | This low-resolution view of the floor of Mars' Jezero Crater and a portion of two wheels of NASA's Perseverance Mars rover was captured by the color imager aboard the agency's Ingenuity Mars helicopter. The image was taken on April 3, 2021, while the solar-powered rotorcraft was still beneath the rover after being deployed. A few higher-resolution images are expected to be acquired by this imager during each of Ingenuity's test flights.NASA's Jet Propulsion Laboratory built and manages operations of Perseverance and Ingenuity for the agency. Caltech in Pasadena, California, manages JPL for NASA. The Mars helicopter technology demonstration activity is supported by NASA's Science Mission Directorate, the NASA Aeronautics Research Mission Directorate, and the NASA Space Technology Mission Directorate.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.For more about Perseverance: mars.nasa.gov/mars2020/.For more about Ingenuity: go.nasa.gov/ingenuity. | |
This image from NASA's Mars Reconnaissance Rover shows a degraded impact crater in the southern highlands. Part of the crater rim is visible at the top and bottom of the image, with the boulder-covered crater floor in the center. | This image from NASA's Mars Reconnaissance Rover (MRO) shows a degraded impact crater in the southern highlands. Part of the crater rim is visible at the top and bottom of the image, with the boulder-covered crater floor in the center.The subdued appearance of the crater indicates that it has been highly modified since it formed. In the southern part of the crater floor a smaller impact crater overlies the larger crater. However, it too has been heavily eroded, such that it can only be identified by the circular pattern of boulders near the rim and the relatively boulder-free ejecta farther from the rim, which covers the boulder-rich floor of the large crater. The boulders in this image range in size from approximately 1 meter (3 feet) to approximately 6 meters (20 feet).Other craters in the region around this HiRISE image have a similar appearance (heavily modified with boulder-rich floors) as seen in this CTX image which covers this crater imaged by HiRISE, as well as a crater directly to the north. This indicates that the processes that have modified this crater are regional in nature.The dark lines crisscrossing the whole image are dust devil tracks that are formed when dust devils move across the surface and pick up bright dust, leaving darker coarse material behind. The subimage shows dust devil tracks along with part of the boulder-rich rim of the smaller crater.The University of Arizona, Tucson, operates the 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, Pasadena, manages the Mars Reconnaissance Orbiter for the NASA Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the spacecraft development and integration contractor for the project and built the spacecraft.
Originally released on July 7, 2010 | |
NASA has named the landing site of the agency's Perseverance rover after the science fiction author Octavia E. Butler, as seen in this image from the High Resolution Imaging Experiment camera aboard NASA's Mars Reconnaissance Orbiter. | NASA has named the landing site of the agency's Perseverance rover "Octavia E. Butler Landing," after the science fiction author Octavia E. Butler. The landing location is marked with a star in this image from the High Resolution Imaging Experiment (HiRISE) camera aboard NASA's Mars Reconnaissance Orbiter (MRO).MRO's mission is managed by NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, for NASA's Science Mission Directorate. Lockheed Martin Space in Denver built the spacecraft. The University of Arizona in Tucson provided and operates HiRISE.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 built and manages operations of the Perseverance rover.For more about Perseverance: mars.nasa.gov/mars2020/ | |
This stereo image from the Mast Camera (Mastcam) on NASA's Mars rover Curiosity shows a rock outcrop called 'Hottah,' cited as evidence for vigorous flow of water in a long-ago Martian stream. You need 3D glasses to view this image. | This stereo image from the Mast Camera (Mastcam) on NASA's Mars rover Curiosity shows a rock outcrop called "Hottah," cited as evidence for vigorous flow of water in a long-ago Martian stream. The scene covers an area roughly 1 yard or meter across at the near edge. It appears three-dimensional when viewed through red-blue glasses with the red lens on the left.Curiosity found evidence for an ancient, flowing stream on Mars at a few sites, including this outcrop named after Hottah Lake in Canada. It may look like a broken sidewalk, but this geological feature on Mars is actually exposed bedrock made up of smaller fragments cemented together, or what geologists call a sedimentary conglomerate. Scientists theorize that the bedrock was disrupted in the past, giving it the tilted angle, most likely via impacts from meteorites. The key evidence for the ancient stream comes from the size and rounded shape of the gravel in and around the bedrock. Hottah has pieces of gravel embedded in it, called clasts, up to a couple inches (few centimeters) in size and located within a matrix of sand-sized material. Some of the clasts are round in shape, leading the science team to conclude they were transported by a vigorous flow of water. The grains are too large to have been moved by wind. Erosion of the outcrop results in gravel clasts that protrude from the outcrop and ultimately fall onto the ground, creating the gravel pile at left. Curiosity's Mastcam acquired component images of this scene on the 39th Martian day, or sol, of the mission (Sept. 14, 2012 PDT/Sept. 15 GMT). Mastcam has two cameras, a telephoto right eye (Mastcam 100) with a 100-millimeter-focal-length lens, and a moderately wide-angle left eye (Mastcam 34) with a 34-millimeter lens. This stereo image combines images from each eye. A right-eye-only version of the scene is at PIA16156. | |
This image acquired on July 10, 2018 by NASA's Mars Reconnaissance Orbiter, shows a clear view of the summit of the giant volcano Elysium Mons. | Map Projected Browse ImageClick on image for larger versionDuring the 2018 Mars dust storm, we obtained a clear view of the summit of the giant volcano Elysium Mons. We see the western rim and floor of the caldera, and a chain of pits (called a "catena") extending from the caldera towards the north. The chain of pits likely formed by volcanic processes, such as the collapse of a lava tube after it drained. Or by a tectonic process, such as a rift in the rocks below that drained loose material from the surface.An unexpected feature of this catena is the presence of avalanches in two of the pits (marked A and B in the cutout, with the uphill direction towards the top of the image.) The flows in both pits could be ancient, produced during the formation of the catena, but they are not found in the other pits in the chain. They might have formed more recently by the collapse of steep dust deposits like those in a degraded crater to the left of the catena (marked C). The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 54.3 centimeters (21.4 inches) per pixel (with 2 x 2 binning); objects on the order of 163 centimeters (64.2 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. | |
Phyllosilicate and Olivine around a Fracture in Nili Fossae | The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) took this observation of part of the Nili Fossae region at the western margin of the Isidis impact basin at 3:07 (UTC) on December 12, 2006, near 21.9 degrees north latitude, 78.2 degrees east longitude. The image was taken in 544 colors covering 0.36-3.92 micrometers, and shows features as small as 18 meters (60 feet) across. The image is about 11 kilometers (7 miles) wide at its narrowest point.The Isidis basin resulted from a gigantic impact on the surface of Mars early in the planet's history. The image of the Isidis basin at the top left is the colored elevation data from the Mars Orbiter Laser Altimeter (MOLA) overlain on a digital image mosaic from the Viking mission. Reds represent higher elevations, and blue lower elevations. The western rim of the Isidis basin has numerous, concentric troughs (or "fossae") which may have formed during faulting associated with the impact event. Since then, the Nili Fossae region has since been heavily eroded, and is one of the most mineralogically diverse spots on Mars. This CRISM image targets one of region's smaller fractures. The image is shown overlain on the Viking digital image mosaic at lower left. The lower right CRISM image was constructed from three visible wavelengths (0.71, 0.60 and 0.53 microns in the red, green and blue image planes, respectively) and is close to what the human eye would see. The blue on the right of the image is an artifact from light scattering in the atmosphere. The upper right image was constructed from three infrared channels (2.38, 1.80 and 1.15 microns in the red, green and blue image planes, respectively) to highlight the mineralogy of the area. The bright green areas are rich in "phyllosilicates," a category of minerals including clays. The purple material along the walls of the fracture likely contains small amounts of the iron- and magnesium-rich mineral pyroxene. The yellow-brown material contains the iron- and magnesium-rich mineral olivine. Olivine and pyroxene are minerals associated with igneous activity. Overlaying CRISM data with images from the High-Resolution Imaging Science Experiment (HiRISE) camera shows that the phyllosilicates are in small, eroded outcrops of rock. The olivine is most abundant in sand dunes on the surface. The use of these two instruments together reveals more about the history of the region: Olivine sands covered the area shown in the image after the interaction of water and rock formed the phyllosilicates and after the fracture formed. The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) is one of six science instruments on NASA's Mars Reconnaissance Orbiter. Led by The Johns Hopkins University Applied Physics Laboratory, the CRISM team includes expertise from universities, government agencies and small businesses in the United States and abroad. | |
This wide view of Mars' Jezero Crater was taken by NASA's Perseverance rover on July 15, 2021. | Figure 1Figure 2Figure 3Click on images for larger versionsThis wide view of Mars' Jezero Crater was taken by NASA's Perseverance rover on July 15, 2021 (the 143rd sol, or Martian day, of its mission). The rover has driven nearly a mile (1.5 kilometers) south of its landing site, "Octavia E. Butler Landing," into a region the team has nicknamed the "Crater Floor Fractured Rough" unit. The stones that appear light-colored and flat in this image (Figure 1) are informally referred to as the "paver rocks" and will be the first type from which Perseverance will collect a sample for planned return to Earth by subsequent missions. Small hills to the south of the rover and the sloping inner walls of the Jezero Crater rim fill the distant background of this view. Five images from the rover's Mastcam-Z instrument were calibrated and combined to make this mosaic. One version (main image), presented in natural color, simulates the approximate view that we would see with our own eyes if we were there. Another version (Figure 2) is presented in enhanced color to exaggerate the subtle red, green, and blue color differences among the materials in this scene.A third version (Figure 3) combines the five images from both the left and right Mastcam-Z cameras into an anaglyph (for red-blue glasses) that simulate a 3D view of the scene in enhanced color.Perseverance has been exploring the floor of Jezero since landing on Feb. 18, 2021.The Mastcam-Z investigation is led and operated by Arizona State University in Tempe, working in collaboration with Malin Space Science Systems in San Diego, California, 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.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.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.NASA's Jet Propulsion Laboratory in Southern California built and manages operations of the Mars 2020 Perseverance rover for NASA.For more information about the mission, go to: https://mars.nasa.gov/mars2020 | |
This pair of images released on June 14, 2004 from NASA's 2001 Mars Odyssey shows a comparison of daytime and nighttime of crater ejecta in the Terra Meridiani region on Mars. | Released 14 June 2004This pair of images shows crater ejecta in the Terra Meridiani region.Day/Night Infrared PairsThe image pairs presented focus on a single surface feature as seen in both the daytime and nighttime by the infrared THEMIS camera. The nighttime image (right) has been rotated 180 degrees to place north at the top. Infrared image interpretationDaytime:Infrared images taken during the daytime exhibit both the morphological and thermophysical properties of the surface of Mars. Morphologic details are visible due to the effect of sun-facing slopes receiving more energy than antisun-facing slopes. This creates a warm (bright) slope and cool (dark) slope appearance that mimics the light and shadows of a visible wavelength image. Thermophysical properties are seen in that dust heats up more quickly than rocks. Thus dusty areas are bright and rocky areas are dark. Nighttime:Infrared images taken during the nighttime exhibit only the thermophysical properties of the surface of Mars. The effect of sun-facing versus non-sun-facing energy dissipates quickly at night. Thermophysical effects dominate as different surfaces cool at different rates through the nighttime hours. Rocks cool slowly, and are therefore relatively bright at night (remember that rocks are dark during the day). Dust and other fine grained materials cool very quickly and are dark in nighttime infrared images.Image information: IR instrument. Latitude -1.6, Longitude 4.1 East (355.9 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 2001 Mars Odyssey spacecraft shows a portion of Mamers Valles. Mamers Valles is a large and complex channel system on the northern margin of Arabia Terra. | Context imageThis VIS image shows a portion of Mamers Valles. Mamers Valles is a large and complex channel system on the northern margin of Arabia Terra.Orbit Number: 61587 Latitude: 33.0496 Longitude: 17.9071 Instrument: VIS Captured: 2015-11-01 20:11Please 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 Exploration Rover Spirit shows the left panorama of the rover's landing site. | Left Panorama of Spirit's Landing SiteThis is a version of the first 3-D stereo image from the rover's navigation camera, showing only the view from the left stereo camera onboard the Mars Exploration Rover Spirit. The left and right camera images are combined to produce a 3-D image. | |
NASA's Phoenix Mars Lander shows the exhaust from its descent engine has blown soil off to reveal either rock or ice on the martian surface beneath it. | This image shows the landing site of NASA's Phoenix Mars Lander on the fourth Martian day of the mission, or Sol 4 (May 29, 2008). The image was taken by Phoenix's Robotic Arm Camera (RAC). As seen in the top center, the exhaust from the descent engine has blown soil off to reveal either rock or ice, which has not yet been determined.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 2001 Mars Odyssey released on April 14, 2004 shows the surface of Mars during the southern summer season in Orson Welles Crater. | Released 14 April 2004The Odyssey spacecraft has completed a full Mars year of observations of the red planet. For the next several weeks the Image of the Day will look back over this first mars year. It will focus on four themes: 1) the poles - with the seasonal changes seen in the retreat and expansion of the caps; 2) craters - with a variety of morphologies relating to impact materials and later alteration, both infilling and exhumation; 3) channels - the clues to liquid surface flow; and 4) volcanic flow features. While some images have helped answer questions about the history of Mars, many have raised new questions that are still being investigated as Odyssey continues collecting data as it orbits Mars. This daytime VIS image was collected on November 13, 2003 during the southern summer season in Orson Welles Crater.Image information: VIS instrument. Latitude -0, Longitude 313.4 East (46.6 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 dark slope streaks prevalent on these isolated hills near the Tartarus Montes on Mars. | Context image for PIA11257Dark Slope StreaksDark slope streaks are prevalent on these isolated hills near the Tartarus Montes.Image information: VIS instrument. Latitude 21.5N, Longitude 178.8E. 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 Mars rover Curiosity used its Mast Camera (Mastcam) to take the images combined into this mosaic of the drill area, called 'John Klein,' where the rover ultimately performed its first sample drilling. | Annotated versionRaw color versionClick on an individual image for larger viewsNASA's Mars rover Curiosity used its Mast Camera (Mastcam) to take the images combined into this mosaic of the drill area, called "John Klein." The label "Drill" indicates where the rover ultimately performed its first sample drilling. Shown on this mosaic are the four targets that were considered for drilling, all of which were analyzed by Curiosity's instrument suite. At "Brock Inlier," data from the Alpha Particle X-ray Spectrometer (APXS) and images from the Mars Hand Lens imager (MAHLI) were collected. The target "Wernecke" was brushed by the Dust Removal Tool (DRT) with complementary APXS, MAHLI, and Chemistry and Camera (ChemCam) analyses. Target "Thundercloud" was the subject of the drill checkout test known as "percuss on rock." The target Drill was interrogated by APXS, MAHLI and ChemCam.The scene was imaged on Sol 166, the 166th Martian day of Curiosity's work on Mars (January 23, 2013). The color has been white-balanced to show what the rocks would like if they were on Earth.Photojournal Note: Also available is the full resolution JPEG file for the annotated version shown above PIA16686_full.jpg. This file may be too large to view from a browser; it can be downloaded onto your desktop by right-clicking on the previous link and viewed with image viewing software.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 gullies running down a slope on the side of a mesa in a pit in the south polar region of Mars. The dark material in this scene is windblown sand. | 15 December 2004This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows gullies running down a slope on the side of a mesa in a pit in the south polar region of Mars. The dark material in this scene is windblown sand. These landforms are located near 70.9°S, 357.3°W. The image covers an area approximately 3 km (1.9 mi) wide and is illuminated by sunlight from the upper left. | |
NASA's Mars Exploration Rover Opportunity used its navigation camera to take the images combined into this stereo view of the rover's surroundings on sol (or Martian day) 959 of its surface mission. | NASA's Mars Exploration Rover Opportunity used its navigation camera to take the images combined into this stereo view of the rover's surroundings on sol (or Martian day) 959 of its surface mission.This view is presented as a polar projection with geometric seam correction. | |
This image captured by NASA's 2001 Mars Odyssey spacecraft shows windstreaks on the volcanic surface between Alba Mons and Acheron Fossae. | Context imageToday's VIS image shows windstreaks on the volcanic surface between Alba Mons and Acheron Fossae.Orbit Number: 53722 Latitude: 31.5024 Longitude: 233.118 Instrument: VIS Captured: 2014-01-23 08:04Please 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. | |
The arc shaped feature at the bottom of this image captured by NASA's 2001 Mars Odyssey spacecraft is the remaining rim of a crater. | Context imageThe arc shaped feature at the bottom of this VIS image is the remaining rim of a crater. The dunes of Olympia Undae have surrounded the rim and small individual dunes are creeping up the slope of the rim.Orbit Number: 62485 Latitude: 79.8969 Longitude: 220.255 Instrument: VIS Captured: 2016-01-14 19:30Please 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 Curiosity rover used the Mars Hand Lens Imager (MAHLI) to capture the set of thumbnail images stitched together to create this full-color self-portrait. | On Sol 84 (Oct. 31, 2012), the Curiosity rover used the Mars Hand Lens Imager (MAHLI) to capture the set of thumbnail images stitched together to create this full-color self-portrait. This self-portrait documents the state of the rover and allows mission engineers to track changes over time, such as dust accumulation and wheel wear. Due to its location on the end of the robotic arm, only MAHLI is able to image some parts of the rover, including port-side wheels.The mosaic shows the rover at "Rocknest," the spot in Gale Crater where the mission's first scoop sampling took place. Scoop scars can be seen in the regolith in front of the rover. A portion of Mount Sharp appears on the right side. Mountains in the background to the left are the northern wall of Gale Crater.When the rover returns the full-resolution MAHLI frames of the scene, the team plans to generate a more detailed portrait of Curiosity in its Martian neighborhood.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://mars.jpl.nasa.gov/msl. | |
This image, taken NASA's Sojourner's front right camera, was taken when the rover was next to Poohbear (rock at left) and Piglet (not seen) as it looked out toward Mermaid Dune. Sol 1 began on July 4, 1997. | This image, taken by Sojourner's front right camera, was taken when the rover was next to Poohbear (rock at left) and Piglet (not seen) as it looked out toward Mermaid Dune. The textures differ from the foreground soil containing a sorted mix of small rocks, fines and clods, from the area a bit ahead of the rover where the surface is covered with a bright drift material. Soil experiments where the rover wheels dug in the soil revealed that the cloudy material exists underneath the drift.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 false color image from NASA's Mars Reconnaissance Orbiter indicates that the volcanic cone in the Nili Patera caldera on Mars has hydrothermal mineral deposits on the southern flanks and nearby terrains. | Annotated VersionClick on the image for larger imageThis volcanic cone in the Nili Patera caldera on Mars has hydrothermal mineral deposits on the southern flanks and nearby terrains. Two of the largest deposits are marked by arrows, and the entire field of light-toned material on the left of the cone is hydrothermal deposits. The cone is about 5 kilometers (3 miles) in diameter at the base.The deposits are evidence for a past local environment that was warm and wet or steamy, possibly hospitable to microbial life, as reported in a November 2010 Nature Geoscience paper by J.R. Skok, of Brown University, Providence, R.I., and co-authors. This image is in false color derived from observation in infrared wavebands with the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on NASA's Mars Reconnaissance Orbiter. The CRISM spectral data is overlaid on imagery from the Context Camera on that orbiter. A stereo pair of Context Camera images provided topographic information for a digital terrain model produced with NASA Ames Stereo Pipeline software. The image uses no vertical exaggeration. | |
This image from NASA's Mars Odyssey shows Olympia Undae, a vast dune field in the north polar region of Mars. | Context imageThis VIS image of Olympia Undae was collected early in north polar spring. The dunes are still covered by the winter frosts; as the region heats up the frost will dissipate to reveal the dark sand beneath. The density of dunes and the alignments of the dune crests varies with location, controlled by the amount of available sand and the predominant winds over time.Olympia Undae is a vast dune field in the north polar region of Mars. It consists of a broad sand sea or erg that partly rings the north polar cap from about 120° to 240°E longitude and 78° to 83°N latitude. The dune field covers an area of approximately 470,000 km2 (bigger than California, smaller than Texas). Olympia Undae is the largest continuous dune field on Mars. Olympia Undae is not the only dune field near the north polar cap, several other smaller fields exist in the same latitude, but in other ranges of longitude, e.g. Abolos and Siton Undae. Barchan and transverse dune forms are the most common. In regions with limited available sand individual barchan dunes will form, the surface beneath and between the dunes is visible. In regions with large sand supplies, the sand sheet covers the underlying surface, and dune forms are found modifying the surface of the sand sheet. In this case transverse dunes are more common. Barchan dunes "point" down wind, transverse dunes are more linear and form parallel to the wind direction. The "square" shaped transverse dunes in Olympia Undae are due to two prevailing wind directions.Orbit Number: 93727 Latitude: 79.5915 Longitude: 159.786 Instrument: VIS Captured: 2023-01-30 19:25Please 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 image shows the first holes drilled by NASA's Mars rover Curiosity at Mount Sharp. The loose material near the drill holes is drill tailings and an accumulation of dust that slid down the rock during drilling. | Annotated VersionClick on the image for larger annotated versionThis image shows the first holes drilled by NASA's Mars rover Curiosity at Mount Sharp. The loose material near the drill holes is drill tailings and an accumulation of dust that slid down the rock during drilling.The site is on a patch of flat rock called "Confidence Hills" in the "Pahrump Hills" area of Mars' Gale Crater. This is Curiosity's first drill site since reaching the base of Mount Sharp in September 2014.An annotated version of the image, indicating scale in the scene, is provided above.For other images related to this drill site, see PIA19037 and PIA19038.The view combines several exposures taken by the Mastcam's left-eye camera during the 759th Martian day, or sol, of the rover's work on Mars (Sept. 24, 2014). The component images have been calibrated, linearly scaled and brightened, which results in colors that resemble those that would be seen under daytime lighting conditions on Earth.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 project's Curiosity rover. Malin Space Science Systems, San Diego, built and operates the rover's Mastcam.More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
The Ingenuity Mars Helicopter's navigation camera captures the helicopter's shadow on the surface of Jezero Crater during rotorcraft's second experimental test flight on April 22, 2021. | The downward-looking navigation camera aboard NASA's Ingenuity Mars Helicopter took this image of the rotorcraft's shadow on the surface of Jezero Crater during helicopter's second experimental test flight on April 22, 2021. The helicopter's navigation camera autonomously tracks the ground during flight.The Ingenuity Mars Helicopter was built by JPL, which also manages this technology demonstration project for NASA Headquarters. It is supported by NASA's Science Mission Directorate, Aeronautics Research Mission Directorate, and Space Technology Mission Directorate. NASA's Ames Research Center and Langley Research Center provided significant flight performance analysis and technical assistance during Ingenuity's development.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 is part of THEMIS art month, taken by NASA's Mars Odyssey featuring a portion of Mars' landscape looking like a pleasant cloudburst falling from Martian dunes. | Welcome to the second annual THEMIS ART MONTH. From Jan. 31 through March 4 we will be showcasing images for their aesthetic value, rather than their science content. Portions of these images resemble things in our everyday lives, from animals to letters of the alphabet. We hope you enjoy our fanciful look at Mars!A pleasant cloudburst seems to fall from these Martian dunes.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 dunes in this image captured by NASA's 2001 Mars Odyssey spacecraft are located in an unnamed crater in Sisyphi Planum. | Context imageThe dunes in today's VIS image are located in an unnamed crater in Sisyphi Planum.Orbit Number: 42494 Latitude: -59.7021 Longitude: 351.602 Instrument: VIS Captured: 2011-07-14 05:03Please 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. | |
Yardangs within a Large Crater | Click on image for larger versionThis HiRISE image (PSP_001545_1885) shows a part of a central mound in an impact crater in Arabia Terra. At low resolution, the mound is relatively smooth and featureless, although elsewhere in the mound a Mars Orbiter Camera (MOC) image shows fine layers. The mound is broad, filling much of the crater, although it now appears to be eroding. Images like this can be used to explore the nature of the deposit, and provide clues about how it formed. At high resolution the material still appears relatively uniform and featureless, without boulders or obvious fine layers. This indicates a relatively weak, fine-grained material. The large, elongated features in the image are yardangs. These are characteristic of aeolian (wind) erosion. They form roughly parallel with the direction of the prevailing wind, and the streamlined shape (often compared with the hull of a boat) is created by persistent flow from this direction. Yardangs on Earth often form from relatively unconsolidated material, supporting the inference made from the appearance of the deposit. Observation Toolbox Acquisition date: 11 November 2006Local Mars time: 3:31 PMDegrees latitude (centered): 8.3°Degrees longitude (East): 21.0°Range to target site: 273.1 km (170.7 miles)Original image scale range: from 27.3 cm/pixel (with 1 x 1 binning) to 109.3 cm/pixel (with 4 x 4 binning)Map-projected scale: 25 cm/pixel and north is upMap-projection: EQUIRECTANGULAREmission angle: 0.1°Phase angle: 51.9°Solar incidence angle: 52°, with the Sun about 38° above the horizonSolar longitude: 140.4°, 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 dunes in this image captured by NASA's 2001 Mars Odyssey are located in an unnamed crater in Terra Cimmeria. | Context imageThe dunes in this VIS image are located in an unnamed crater in Terra Cimmeria.Orbit Number: 37311 Latitude: -13.5817 Longitude: 124.677 Instrument: VIS Captured: 2010-05-13 11:00Please 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. | |
NASA's Mars Global Surveyor shows a small impact crater with a 'butterfly' ejecta pattern. The butterfly pattern results from an oblique impact. | 22 June 2005This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a small impact crater with a "butterfly" ejecta pattern. The butterfly pattern results from an oblique impact. Not all oblique impacts result in an elliptical crater, but they can result in a non-radial pattern of ejecta distribution. The two-toned nature of the ejecta -- with dark material near the crater and brighter material further away -- might indicate the nature of subsurface materials. Below the surface, there may be a layer of lighter-toned material, underlain by a layer of darker material. The impact throws these materials out in a pattern that reflects the nature of the underlying layers.Location near: 3.7°N, 348.2°W Image width: ~3 km (~1.9 mi) Illumination from: lower left Season: Northern Autumn | |
This dark mound, called 'Ireson Hill,' rises about 16 feet (5 meters) above redder layered outcrop material of the Murray formation on lower Mount Sharp, Mars, near a location where NASA's Curiosity rover examined a linear sand dune in February 2017. | Click on the image for larger imageThis dark mound, called "Ireson Hill," rises about 16 feet (5 meters) above redder layered outcrop material of the Murray formation on lower Mount Sharp, Mars, near a location where NASA's Curiosity rover examined a linear sand dune in February 2017.Researchers used the rover's Mast Camera (Mastcam) on Feb. 2, 2017, during the 1,598th Martian day, or sol, of Curiosity's work on Mars, to take the 41 images combined into this scene. The mosaic has been white-balanced so that the colors of the rock and sand materials resemble how they would appear under daytime lighting conditions on Earth. The view extends from west-southwest on the left to north-northwest on the right. The faint horizon in the distance beyond Ireson Hill is part of the rim of Gale Crater. The rover's Sol 1598 location is mapped at https://mars.nasa.gov/multimedia/images/2017/curiositys-traverse-map-through-sol-1598 .Figure 1 is an annotated version with scale bars indicating dimensions at two distances from the rover. The nearer scale bar, in meters, refers to features near the base of the hill, about 46 feet (14 meters) away from the camera. The farther one, in centimeters, refers to features at the top of the hill, about 85 feet (26 meters) from the camera.Malin Space Science Systems, San Diego, built and operates the Mastcam. NASA's Jet Propulsion Laboratory, a division of the Caltech in Pasadena, California, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the project's Curiosity rover. Malin Space Science Systems, San Diego, built and operates the Mastcam. NASA's Jet Propulsion Laboratory, a division of the Caltech in Pasadena, California, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the project's Curiosity rover. More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
This NASA 2001 Mars Odyssey spacecraft image shows two different types of linear depressions. The wide depression at the top of the frame is Elysium Fossae, which most likely formed due to tectonic activity. | Context imageCredit: NASA/JPL/MOLAThis VIS image shows two different types of linear depressions. The wide depression at the top of the frame is Elysium Fossae, which most likely formed due to tectonic activity. The fossae is probably bounded on both sides by faults. The narrow depression at the bottom of the frame is a lava channel called Patapsco Vallis. This channel has lava flows on both sides which were probably formed by over spilling of lava as it flowed down the channel. Both these features are located east of Elysium Mons.Image information: VIS instrument. Latitude 24.1N, Longitude 152.8E. 21 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 360-degree panorama was acquired by the Mast Camera (Mastcam) on NASA's Curiosity Mars rover as the rover neared features called 'Murray Buttes' on lower Mount Sharp. | This 360-degree panorama was acquired by the Mast Camera (Mastcam) on NASA's Curiosity Mars rover as the rover neared features called "Murray Buttes" on lower Mount Sharp.The view combines more than 130 images taken on Aug. 5, 2016, during the afternoon of the mission's 1,421st sol, or Martian day, by Mastcam's left-eye camera. This date also was the fourth anniversary of Curiosity's landing.The dark, flat-topped mesa seen to the left of Curiosity's robotic arm is about 300 feet (about 90 meters) from the rover's position. It stands about 50 feet (about 15 meters) high. The horizontal ledge near the top of the mesa is about 200 feet (about 60 meters) across. An upper portion of Mount Sharp appears on the distant horizon to the left of this mesa.The relatively flat foreground is part of a geological layer called the Murray formation, which formed from lakebed mud deposits. The buttes and mesas rising above this surface are eroded remnants of ancient sandstone that originated when winds deposited sand after lower Mount Sharp had formed. Curiosity closely examined that layer -- the Stimson formation -- during the first half of 2016 while crossing a feature called "Naukluft Plateau" between two exposures of the Murray formation. The buttes and mesas of Murray Buttes are capped by material that is relatively resistant to erosion, just as is the case with many similarly shaped buttes and mesas on Earth. The informal naming honors Bruce Murray (1931-2013), a Caltech planetary scientist and director of NASA's Jet Propulsion Laboratory, Pasadena, California.The scene is presented with a color adjustment that approximates white balancing, to resemble how the rocks and sand would appear under daytime lighting conditions on Earth. The rover's location when its Mastcam acquired the component images of this scene was the site it reached in its Sol 1417 drive. (See map at http://mars.nasa.gov/msl/multimedia/images/?ImageID=7963.) Malin Space Science Systems, San Diego, built and operates Mastcam. JPL, a division of Caltech, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington, and built the project's Curiosity rover. For more information about Curiosity, visit http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl. | |
This pair of pictures from NASA's Viking Lander 1 at Mars' Chryse Planitia shows the only unequivocal change in the Martian surface seen by either lander. A high boulder nicknamed 'Big Joe' is shown next to a small-scale slump feature. | This pair of pictures from Viking Lander 1 at Mars' Chryse Planitia shows the only unequivocal change in the Martian surface seen by either lander. Both images show the one-meter (3-foot) high boulder nicknamed 'Big Joe.' Just to the lower right of the rock (right photo) is a small-scale slump feature. The picture at left shows a smooth, dust-covered slope; in the picture at right the top surface layer can be seen to have slipped downslope. The event occurred sometime between Oct. 4, 1976, and Jan 24, 1977. (Pictures taken before Oct. 4 do not show the slump; the first picture in which it appears was taken Jan. 24.) The surface layer, between one-half and one centimeter (one-fifth to one-third inch) thick, is apparently less cohesive than the underlying material. The layer that slipped formed a 30-centimeter-long (11.8-inch) 'tongue' of soil and a patch of exposed underlying material. The triggering mechanism for the event is unknown, but could have been temperature variations, wind gusts, a seismic event, or perhaps the lander's touchdown on July 20, 1976. | |
This plot shows the first-ever look at the deuterium to hydrogen ratio measured from the surface of Mars, as detected by the Sample Analysis at Mars instrument, or SAM, on NASA's Curiosity rover. | This plot shows the first-ever look at the deuterium to hydrogen ratio measured from the surface of Mars, as detected by the Sample Analysis at Mars instrument, or SAM, on NASA's Curiosity rover. Deuterium is a heavier version of the hydrogen atom. Scientists look at the deuterium to hydrogen ratios on Mars (or D/H levels) along with isotopes of other elements to study how its atmosphere has changed over time. Mars, which has less gravity than Earth and lacks a strong enough magnetic field to shield its atmosphere from the sun, is slowly losing its atmosphere. As this process occurs, the lighter hydrogen atoms are preferentially lost compared to the heavier deuterium ones. SAM measured the D/H ratios in water released upon heating of sand samples taken from the wind drift called "Rocknest." The results show the water vapor consists of more deuterium than that of Earth's water, i.e. the water is heavier. This is to be expected since the lighter hydrogen atoms in the Martian atmosphere are escaping faster than the heavier ones. 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://mars.jpl.nasa.gov/msl. | |
This image from NASA's Mars Odyssey shows part of the complex caldera at the summit of Ascraeus Mons. | Context imageThis VIS image shows part of the complex caldera at the summit of Ascraeus Mons. Ascraeus Mons is the northernmost and tallest of the three large aligned Tharsis volcanoes. Calderas are found at the tops of volcanoes and are the source region for magma that rises from an underground lava source to erupt at the surface. Volcanoes are formed by repeated flows from the central caldera. The final eruptions can pool within the summit caldera, leaving a flat surface as they cool. Calderas are also a location of collapse, creating rings of tectonic faults that form the caldera rim. Ascraeus Mons has several caldera features at its summit. Ascraeus Mons is 18 km (11 miles) tall, for comparison Mauna Kea – the tallest volcano on Earth – is 10 km tall (6.2 miles, measured from the base below sea level).Orbit Number: 86205 Latitude: 11.3492 Longitude: 255.876 Instrument: VIS Captured: 2021-05-21 10:18Please 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 part of Ariadnes Colles. The term colles means hills or knobs. | 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 Ariadnes Colles. The term colles means hills or knobs. In this false color combination the hills stand out against the darker surrounding plains. This difference is due to the amount of dust covering the hills versus the plains.Orbit Number: 81254 Latitude: -34.5362 Longitude: 172.495 Instrument: VIS Captured: 2020-04-08 18:19Please 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 pits and channels located along the margin between Arabia Terra and Acidalia Planitia. | Context imageThe pits and channels in the VIS image are located along the margin between Arabia Terra and Acidalia Planitia. Arabia Terra is one of the oldest surface regions on Mars and contains a large variety of surface features.Orbit Number: 77916 Latitude: 30.7624 Longitude: 345.182 Instrument: VIS Captured: 2019-07-08 22:06Please 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 bright features in this image captured by NASA's Mars Odyssey are the tops of clouds north of Alba Mons. | Context imageThe bright features in this VIS image are the tops of clouds north of Alba Mons.Orbit Number: 38802 Latitude: 64.7511 Longitude: 294.894 Instrument: VIS Captured: 2010-09-13 07:01Please 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 2001 Mars Odyssey spacecraft shows part of the margin of the north polar cap and the surrounding plains. The layering of the ice is easily visible due to the dust that is deposited on the top of the ice every year. | Context image This VIS image shows part of the margin of the north polar cap and the surrounding plains. The layering of the ice is easily visible due to the dust that is deposited on the top of the ice every year, creating layering over millions of years.Orbit Number: 71835 Latitude: 83.7224 Longitude: 117.158 Instrument: VIS Captured: 2018-02-23 01:58Please 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 spacecraft shows dark slope streaks in an unnamed crater in Terra Sabaea. These features are believed to be formed by material moving downslope, removing the dust cover and revealing darker material. | Context imageToday's VIS image shows dark slope streaks in an unnamed crater in Terra Sabaea. These features are believed to be formed by material moving downslope, removing the dust cover and revealing darker material.Orbit Number: 56045 Latitude: 11.9172 Longitude: 46.5184 Instrument: VIS Captured: 2014-08-02 12:09Please 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 several wind streaks in Syrtis Major Planum. | Context image The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows several wind streaks in Syrtis Major Planum.Orbit Number: 50693 Latitude: -0.448856 Longitude: 68.374 Instrument: VIS Captured: 2013-05-19 02:56Please 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. | |
This image from NASA's Mars Odyssey shows part of Cerberus Fossae. These large graben cut across the Tartarus Montes in Elysium Planitia. | Context imageToday's VIS image shows part of Cerberus Fossae. These large graben cut across the Tartarus Montes in Elysium Planitia. A graben is formed when large blocks of material slid downward between paired faults in regions of extensional stresses.Orbit Number: 77648 Latitude: 10.0918 Longitude: 160.48 Instrument: VIS Captured: 2019-06-16 20:19Please 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 cross section of Pavonis Mons, including part of the summit caldera. | Context imageThis VIS image shows a cross section of Pavonis Mons, including part of the summit caldera (circular region near the top of the image). Pavonis Mons is the central volcano of the three large Tharsis volcanoes. In order from north to south the volcanoes are Ascreaus Mons, Pavonis Mons and Arsia Mons. All three volcanoes form a line located along a tectonic bulge caused by extensional forces in the region. Along this trend there are increased tectonic features and additional lava flows that arose from the flanks of the volcanoes rather than just the summit. Like the other large volcanoes in the region, Pavonis Mons is a shield volcano. Shield volcanoes are formed by lava flows originating near or at the summit, building up layers upon layers of lava. In shield volcanoes summit calderas are typically formed where the surface collapses into the void formed by an emptied magma chamber. Pavonis Mons is the smallest of the three volcanoes with a summit of only 14km (8.7 miles) and a width of 375 km (233 miles). Like most shield volcanoes the surface has a low profile. In the case of Pavonis Mons the average slope is only 4 degrees. Pavonis means peacock in Latin, making it's name peacock mountain.Orbit Number: 91047 Latitude: 0.277333 Longitude: 248.096 Instrument: VIS Captured: 2022-06-24 02:47Please 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 an unnamed crater, located on the northern margin of Aonia Terra, interacting with one of the fossa, also called a graben. | Context imageLocated on the northern margin of Aonia Terra, this unnamed crater interacts with one of the fossa, also called a graben. In this image, it is apparent that the tectonic depression crosses the crater, which means the crater was created before the depression. The ability to relatively date the different features allows for interpretations of the series of events that created the features in this image.Orbit Number: 74806 Latitude: -42.6506 Longitude: 273.295 Instrument: VIS Captured: 2018-10-25 18:22Please 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. | |
This image from NASA's Mars Odyssey spacecraft was acquired of Candor Chasma within Valles Marineris and shows the effects of erosion on a sequence of dramatically layered rocks. | This image from the camera system on NASA. Mars Odyssey was acquired of Candor Chasma within Valles Marineris, centered near 5 degrees south latitude, 283 degrees east longitude. This visible color image shows the effects of erosion on a sequence of dramatically layered rocks. These layers were initially deposited within Candor Chasma and have subsequently been eroded by a variety of processes, including wind and down-slope motion due to gravity. Relatively dark materials appear to mantle some areas of the layered deposits; these dark materials are likely sand. Few impact craters of any size can be seen in this image, indicating that the erosion and transport of material is occurring at a relatively rapid rate, so that any craters that form are rapidly buried or eroded. This image was acquired using the thermal infrared imaging system.s visible bands 1 (centered at 420 nanometers), 2 (centered at 550 nanometers), and 3 (centered at 650 nanometers), and covers an area approximately 19 kilometers (12 miles) in width by 50 kilometers (50 miles) in length.This and several other new color images can be obtained from the NASA Planetary Photojournal website.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 possible exit path, pictured on the far right of this image where the outcrop is punctuated, was eventually deemed too hazardous for NASA's Mars Exploration Rover Opportunity to attempt. | As NASA's Mars Exploration Rover Opportunity was making its way back toward its original entry path into "Endurance Crater," scientists and engineers spotted what they hoped might be a shortcut for climbing out of the crater. The possible exit path, pictured on the far right of this image where the outcrop is punctuated, was eventually deemed too hazardous for the rover to attempt. Opportunity would have had to cross terrain with a slope of 28 degrees and face a tall rock outcropping very close to the exit chute opening which, itself, is too narrow for the rover to pass. This stereo view combines several frames taken by the rover's navigation camera during Opportunity's 297th sol on Mars (Nov. 24, 2004). It is presented in a cylindrical-perspective projection with geometric seam correction. The location from which the image was taken has been designated as Opportunity's Site 38, Position 97. | |
NASA's Mars Exploration Rover Opportunity used its front hazard-identification camera to obtain this image at the end of a drive on the rover's 1,271st sol, or Martian day (Aug. 21, 2007). | NASA's Mars Exploration Rover Opportunity used its front hazard-identification camera to obtain this image at the end of a drive on the rover's 1,271st sol, or Martian day (Aug. 21, 2007).Due to sun-obscuring dust storms limiting the rover's supply of solar energy, Opportunity had not driven since sol 1,232 (July 12, 2007). On sol 1,271, after the sky above Opportunity had been gradually clearing for more than two weeks, the rover rolled 13.38 meters (44 feet). Wheel tracks are visible in front of the rover because the drive ended with a short test of driving backwards.Opportunity's turret of four tools at the end of the robotic arm fills the center of the image. Victoria Crater, site of the rover's next science targets, lies ahead. | |
This image from NASA's Mars Odyssey shows several craters located in Terra Cimmeria. | 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 several craters located in Terra Cimmeria.Orbit Number: 70002 Latitude: -16.4105 Longitude: 144.043 Instrument: VIS Captured: 2017-09-25 01:08Please 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 image from NASA's Mars Odyssey shows a section of one of the numerous channels that dissect the northern margin on Arabia Terra. | Context imageThis VIS image shows a section of one of the numerous channels that dissect the northern margin on Arabia Terra.Orbit Number: 80460 Latitude: 36.1968 Longitude: 28.8173 Instrument: VIS Captured: 2020-02-03 09:40Please 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. | |
Why are these dunes different colors? Sand on Mars is typically dark in tone, as it commonly derived from volcanic rocks like lava flows as shown by NASA's Mars Reconnaissance Orbiter. | Map Projected Browse ImageClick on the image for larger versionWhy are these dunes different colors? Sand on Mars is typically dark in tone, as it commonly derived from volcanic rocks like lava flows. In HiRISE enhanced color, which operates in long infrared wavelengths (beyond what the human eye can detect), surfaces like these dune crests are dark blue to purple. Sand comes in sizes that are ideal for surface transport by the wind, where sand "hops" along forming bedforms, like these dunes after large amounts of time.The lighter toned "tan" or "reddish" surfaces are indeed composed of a different material, but not as sand sized particle that makes up the bulk of these dunes. Rather, the light-toned smooth surfaces that dominate the lower, flatter areas of the dunes are a thin coating of global dust. Dust on Mars is composed of a variety of materials, including oxidized iron, like rust.For a given wind gust, speeds are not constant at different heights. Rather, wind speeds are greater with height above the ground and wind energy drops to nearly zero at the surface. Dust persists on flatter dune areas, because wind energy there has not been sufficient to remove it, whereas "dust free" higher-lying dune crests are subject to more intense winds, which ultimately conspire to make the appearance of two-color dunes. 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 the NASA Science Mission Directorate, Washington. | |
Sand dunes on the floor of Rabe Crater are brighter in this infrared image from NASA's 2001 Mars Odyssey spacecraft than the surrounding materials. This is because the sand is warmer than the surrounding rock. | Context imageSand dunes on the floor of Rabe Crater are brighter in this infrared image than the surrounding materials. This is because the sand is warmer than the surrounding rock.Orbit Number: 57712 Latitude: -43.7612 Longitude: 34.3755 Instrument: IR Captured: 2014-12-17 17:16Please 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 VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of the floor of Candor Chasma. | 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 Candor Chasma.Orbit Number: 10963 Latitude: -5.19848 Longitude: 283.975 Instrument: VIS Captured: 2004-06-04 00:30Please 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 part of Granicus Valles. Granicus Valles is a complex channel system located west of Elysium Mons. | Context imageThis VIS image shows part 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: 94832 Latitude: 28.5187 Longitude: 217.227 Instrument: VIS Captured: 2023-05-01 18:38Please 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. | |
This image from NASA's Mars Exploration Rover Opportunity's view shows the rover's tracks visible at the original spot where the rover attempted unsuccessfully to exit its landing site crater in 2004. | This image shows the Mars Exploration Rover Opportunity's view on its 56th sol on Mars, before it left its landing-site crater. To the right, the rover tracks are visible at the original spot where the rover attempted unsuccessfully to exit the crater. After a one-sol delay, Opportunity took another route to the plains of Meridiani Planum. This image was taken by the rover's navigation camera. | |
This image from NASA's Mars Global Surveyor shows a small volcano in the Syria Planum region of Mars. The lava flows that compose this small volcano are nearly hidden by a mantle of rough-textured, perhaps somewhat cemented, dust. | 23 July 2006This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a small volcano in the Syria Planum region of Mars. Today, the lava flows that compose this small volcano are nearly hidden by a mantle of rough-textured, perhaps somewhat cemented, dust. The light-toned streaks that cross the scene were formed by passing dust devils, a common occurrence in Syria.Location near: 13.0°S, 102.6°W Image width: ~3 km (~1.9 mi) Illumination from: upper left Season: Southern Autumn | |
The dunes and landslides in this image occur within Coprates Chasma on Mars as seen by NASA's 2001 Mars Odyssey spacecraft. | Context image for PIA08451Slides and DunesThe dunes and landslides in this image occur within Coprates Chasma.Image information: VIS instrument. Latitude -14.5N, Longitude 303.4E. 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 color full-resolution image showing the heat shield of NASA's Curiosity rover was obtained during descent to the surface of Mars. This image shows the inside surface of the heat shield, with its protective multi-layered insulation. | This color full-resolution image showing the heat shield of NASA's Curiosity rover was obtained during descent to the surface of Mars on Aug. 5 PDT (Aug. 6 EDT). The image was obtained by the Mars Descent Imager instrument known as MARDI and shows the 15-foot (4.5-meter) diameter heat shield when it was about 50 feet (16 meters) from the spacecraft. This image shows the inside surface of the heat shield, with its protective multi-layered insulation. The bright patches are calibration targets for MARDI. Also seen in this image is the Mars Science Laboratory Entry, Descent, and Landing Instrument (MEDLI) hardware attached to the inside surface.At this range, the image has a spatial scale of 0.4 inches (1 cm) per pixel. It is the 36th MARDI image, obtained about three seconds after heat shield separation and about two and one-half minutes before touchdown. The original image from MARDI has been geometrically corrected to look flat. The thumbnail version of this image is available at PIA15988.Curiosity landed inside of a crater known as Gale Crater.
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. | |
NASA's Mars Global Surveyor shows a surface in Mars' south polar region, covered by carbon dioxide frost. | 29 May 2005This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a surface in the south polar region, covered by carbon dioxide frost. In this springtime scene, the frost has begun to sublime or change character so that sandy surfaces exhibit an abundance of dark spots. The circular depression is probably the remains of an impact crater. In summer, the spotted surfaces in this image would be darker than their surroundings, because they are patches of windblown sand.Location near: 67.6°S, 254.3°WImage width: ~3 km (~1.9 mi Illumination from: upper left Season: Southern Spring | |
NASA Mars Odyssey observations are used in this global view of Mars in intermediate-energy, or epithermal, neutrons. Soil enriched by hydrogen is indicated by the deep blue colors on the map, which show a low intensity of epithermal neutrons. | Observations by NASA's 2001 Mars Odyssey spacecraft show a global view of Mars in intermediate-energy, or epithermal, neutrons. Soil enriched by hydrogen is indicated by the deep blue colors on the map, which show a low intensity of epithermal neutrons. Progressively smaller amounts of hydrogen are shown in the colors light blue, green, yellow and red. The deep blue areas in the polar regions are believed to contain up to 50 percent water ice in the upper one meter (three feet) of the soil. Hydrogen in the far north is hidden at this time beneath a layer of carbon dioxide frost (dry ice). Light blue regions near the equator contain slightly enhanced near-surface hydrogen, which is most likely chemically or physically bound because water ice is not stable near the equator. The view shown here is a map of measurements made during the first three months of mapping using the neutron spectrometer instrument, part of the gamma ray spectrometer instrument suite. The central meridian in this projection is zero degrees longitude. Topographic features are superimposed on the map for geographic reference.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. Investigators at Arizona State University in Tempe, the University of Arizona in Tucson, and NASA's Johnson Space Center, Houston, operate the science instruments. The gamma-ray spectrometer was provided by the University of Arizona in collaboration with the Russian Aviation and Space Agency, which provided the high-energy neutron detector, and the Los Alamos National Laboratories, New Mexico, which provided the neutron spectrometer. Lockheed Martin Astronautics, Denver, is the prime contractor for the 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 Global Surveyor shows the Acidalia/Mare Erythraeum face of Mars in mid-August, 2006. | 8 August 2006This picture is a composite of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) daily global images acquired at Ls 93° during a previous Mars year. This month, Mars looks similar, as Ls 93° occurs in mid-August 2006. The picture shows the Acidalia/Mare Erythraeum face of Mars. Over the course of the month, additional faces of Mars as it appears at this time of year are being posted for MOC Picture of the Day. Ls, solar longitude, is a measure of the time of year on Mars. Mars travels 360° around the Sun in 1 Mars year. The year begins at Ls 0°, the start of northern spring and southern autumn.Season: Northern Summer/Southern Winter | |
This image taken by NASA's Mars Reconnaissance Orbiter features three newly-formed slope streaks. These are features which occur on crater walls, hills, and other slopes on Mars. | This observation features three newly-formed slope streaks. These are features which occur on crater walls, hills, and other slopes on Mars.They always begin at a point source and widen downslope, sometimes weaving around existing topographic features (such as dunes or craters), but other times they flow over them. Many slope streaks do not show topographic relief in available images, and there are no observable deposits of displaced materials surrounding their borders.In general, slope streaks tend to be many hundreds of meters long and less than 200 meters wide. They are observed in varying shades of darkness, where lighter-toned streaks appear to be older than darker ones. The formation mechanism responsible for slope streaks is still under debate; theories range from dry dust avalanches (most widely-accepted theory) to briney water seepage.Slope streak formation is among the few surface processes known to be currently active on Mars, making slope streaks some of the youngest features on Mars. A comparison of this HiRISE image with MOC image E04-01817 shows that three new slope streaks have formed during the six years separating these images (2001-2007). The shortest time frame in which new slope streaks have been observed to form is six months (MOC images SP2-37303 and E02-02379), though it is not yet known how long it actually takes for a slope streak to form.MOC image E04-01817 courtesy of NASA/JPL/Malin Space Science Systems.The University of Arizona, Tucson, operates the 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, Pasadena, manages the Mars Reconnaissance Orbiter for the NASA Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the spacecraft development and integration contractor for the project and built the spacecraft. | |
NASA's Mars Global Surveyor shows lava flows and channels on the flanks of the Alba Patera volcano on Mars, mostly obscured by a covering of eroded, lumpy-textured material of unknown origin. This picture was taken in July 1998. | The lava flows and channels on the flanks of the Alba Patera volcano are mostly obscured by a covering of eroded, lumpy-textured material of unknown origin. This picture was taken in July 1998. | |
Spirit's View Beside 'Home Plate' on Sol 1823 | NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this 180-degree view of the rover's surroundings during the 1,823rd Martian day, or sol, of Spirit's surface mission (Feb. 17, 2009).The center of the view is toward the south-southwest.The rover had driven 7 meters (23 feet) eastward earlier on Sol 1823, part of maneuvering to get Spirit into a favorable position for climbing onto the low plateau called "Home Plate." However, after two driving attempts with negligible progress during the following three sols, the rover team changed its strategy for getting to destinations south of Home Plate. The team decided to drive Spirit at least partway around Home Plate, instead of ascending the northern edge and taking a shorter route across the top of the plateau.Layered rocks forming part of the northern edge of Home Plate can be seen near the center of the image. Rover wheel tracks are visible at the lower edge.This view is presented as a cylindrical projection with geometric seam correction. | |
This image from NASA's Mars Odyssey shows a channel, Tinto Vallis. This northward flowing channel is 180 km (112 miles) long and is located in northern Hesperia Planum. | Context imageThe channel in the center of this VIS image is Tinto Vallis. This northward flowing channel is 180 km (112 miles) long and is located in northern Hesperia Planum. Tinto Vallis arises in the plains of Herperia Planum and empties into Palos Crater.Orbit Number: 88032 Latitude: -3.35203 Longitude: 110.907 Instrument: VIS Captured: 2021-10-18 20:36Please 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. | |
Spirit Guidepost, 'Plymouth Rock' | NASA's Mars Exploration Rover Spirit took this panoramic camera image during Spirit's 152nd sol, on June 7, 2004. The rock, informally named "Plymouth Rock," is approximately 90 centimeters (35 inches) across and 50 centimeters (20 inches) tall. Spirit did not spend any time studying Plymouth Rock, but rover controllers used it as a guide to maneuver Spirit closer to the "Columbia Hills." Like most of the rocks found at the Gusev crater location, Plymouth is most likely a basalt. The tiny vesicles pitting the rock's surface further indicate its volcanic origin. | |
Opportunity's Travels | This overview map made from Mars Orbiter camera images illustrates the path that the Mars Exploration Rover Opportunity has taken from its first sol on the red planet through its 87th sol. After thoroughly examining its "Eagle Crater" landing-site, the rover moved onto the plains of Meridiani Planum, stopping to examine a curious trough and a target within it called "Anatolia." Following that, Opportunity approached and remotely studied the rocky dish called "Fram Crater." As of its 91st sol (April 26, 2004), the rover sits 160 meters (about 525 feet) from the rim of "Endurance Crater." | |
This synthetic image of NASA's Spirit Mars Exploration Rover on top of a rock called 'Jibsheet' was produced using 'Virtual Presence in Space' technology. | This synthetic image of the Spirit Mars Exploration Rover on top of a rock called "Jibsheet" was produced using "Virtual Presence in Space" technology. Developed at NASA's Jet Propulsion Laboratory, Pasadena, Calif., this technology combines visualization and image-processing tools with Hollywood-style special effects. The image was created using a photorealistic model of the rover and a false-color mosaic. The size of the rover in the image is approximately correct and was based on the size of the rover tracks in the mosaic. The mosaic was assembled from frames taken by the panoramic camera on the rover's 489th Martian day, or sol (May 19, 2005); see PIA07997.Because this synthesis provides viewers with a sense of their own "virtual presence" (as if they were there themselves), such views can be useful to mission teams in planning exploration by enhancing perspective and a sense of scale. | |
This 2001 Mars Odyssey spacecraft image of the western portion of Sirenum Fossae on Mars shows mesa formation. | Context image for PIA11893Sirenum FossaeThis VIS image of the western portion of Sirenum Fossae shows mesa formation.Image information: VIS instrument. Latitude -26.4N, Longitude 219.4E. 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. | |
Dark slope streaks mark the inner rim of this unnamed crater in Arabia Terra as seen by NASA's 2001 Mars Odyssey spacecraft. | Context imageDark slope streaks mark the inner rim of this unnamed crater in Arabia Terra.Orbit Number: 52743 Latitude: 20.8045 Longitude: 14.9941 Instrument: VIS Captured: 2013-11-03 19:15Please 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. |
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