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This image from NASA's Mars Odyssey shows a small field of sand dunes on the floor of Bamberg Crater.

Context imageToday's VIS image shows a small field of sand dunes on the floor of Bamberg Crater.Orbit Number: 77666 Latitude: 39.3767 Longitude: 356.912 Instrument: VIS Captured: 2019-06-18 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.

This image from NASA's Mars Odyssey shows part of Nili Patera. Nili Patera is the northern caldera in the immense volcanic complex of Syrtis Major Planum.

Context imageToday's VIS image shows part of Nili Patera. Nili Patera is the northern caldera in the immense volcanic complex of Syrtis Major Planum. The dunes are moving westward across the top of these ancient volcanic flows.Orbit Number: 90030 Latitude: 8.95316 Longitude: 67.1774 Instrument: VIS Captured: 2022-04-01 09:05Please 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.

Complex Sulfate Deposits in Coprates Chasma

This image of layered sulfate-containing deposits in the Coprates Chasma region of Mars was taken by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) at 1827UTC (1:27 p.m. EST) on December 12, 2006 near 10.2 degrees south latitude, 68.8 degrees west longitude. The image was taken in 544 colors covering 0.36-3.92 micrometers, and shows features as small as 40 meters (132 feet) across. The image is about 11 kilometers (6.8 miles) wide at its narrowest point.Coprates Chasma forms part of the backbone of the Valles Marineris canyon system. It extends approximately east-west for roughly 966 kilometers (600 miles), and is one of the larger chasmata in the Valles Marineris system.The top panel in the montage above shows the location of the CRISM image on a mosaic taken by the Mars Odyssey spacecraft's Thermal Emission Imaging System (THEMIS). The CRISM data covers an area centered on a knob near the chasma's northern wall.The center left image, an infrared false color image, shows the knob's layered morphology. The center right image unveils the mineralogical signatures of some of those layers, with yellow representing monohydrated sulfates (sulfates with one water molecule incorporated into each molecule of the mineral) and purple representing polyhydrated sulfates (sulfates with multiple waters per mineral molecule).The lower two images are renderings of data draped over topography with 3 times vertical exaggeration. These images provide a view of the topography and reveal how the sulfate deposits relate to that topography. Darker polyhydrated sulfates (purple) lie along the knob's western flank. Brighter, monohydrated sulfates (yellow) appear to be superimposed on polyhydrated sulfate deposits in the southwest corner of the image. These coarsely banded deposits continue along the southeast side of the knob.There are two possible explanations for the compositional banding of these sulfates. The first is deposition of mono- and polyhydrated sulfates in alternating layers. The second is deposition of just one sulfate type, and its subsequent alteration by weathering at the exposed, eroded surface. Further observations and analysis will better determine the origin of these complex banded sulfate deposits.CRISM is one of six science instruments on NASA's Mars Reconnaissance Orbiter. Led by The Johns Hopkins University Applied Physics Laboratory, Laurel, Md., the CRISM team includes expertise from universities, government agencies and small businesses in the United States and abroad. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter and the Mars Science Laboratory for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, built the orbiter.

This image acquired on December 15, 2018 by NASA's Mars Reconnaissance Orbiter, shows a cross-section of a complex crater in Terra Cimmeria.

Map Projected Browse ImageClick on image for larger versionThis image shows a cross-section of a complex crater in Terra Cimmeria. Starting in the center, we see a series of peaks with exposed bedrock. These peaks formed during the impact event when material that was originally several kilometers below the surface was uplifted and exposed. The impact also melted the rocks. This eventually cooled, forming the pitted materials that coat the crater floor around the uplift.The rim of the crater was unstable, and collapsed inwards to form terraces, and we see additional pitted materials between the terraces and the rim. Just outside the crater we can see dark-toned material that was excavated and thrown out after the impact.The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 51.4 centimeters (20.2 inches) per pixel (with 2 x 2 binning); objects on the order of 154 centimeters (60.6 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.

The crater in this image captured by NASA's 2001 Mars Odyssey spacecraft has not only been filled by wind-blown material, but that material has been eroded into the two directions of winnowing by continued wind action.

Context imageThe crater in this VIS image has not only been filled by wind-blown material, but that material has been eroded into the two directions of winnowing by continued wind action.Orbit Number: 45719 Latitude: 7.87791 Longitude: 210.169 Instrument: VIS Captured: 2012-04-04 18:03Please 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.

The dunes in this image from NASA's Mars Odyssey are located on the floor of Arkhangelsky Crater.

Context imageToday's dunes are located on the floor of Arkhangelsky Crater.Orbit Number: 41147 Latitude: -40.5367 Longitude: 335.454 Instrument: VIS Captured: 2011-03-25 07:42Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

This animation shows NASA InSight's heat probe, or 'mole,' digging about a centimeter (half an inch) below the surface.

Click here for animationThis GIF shows NASA InSight's heat probe, or "mole," digging about a centimeter (half an inch) below the surface last week. Using a technique called "pinning," InSight recently pressed against the mole using a scoop on its robotic arm to help the self-hammering heat probe dig so that it can "take the temperature" of Mars.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 Seismic Experiment for Interior Structure (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 Heat Flow and Physical Properties Package (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 the southeastern rim of Toro Crater. Toro Crater is located in Syrtis Major Planum and is 41km (25miles) in diameter.

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 the southeastern rim of Toro Crater. Toro Crater is located in Syrtis Major Planum and is 41km (25miles) in diameter.Orbit Number: 79061 Latitude: 16.8233 Longitude: 72.1675 Instrument: VIS Captured: 2019-10-11 04:54Please 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.

NASA's Mars Global Surveyor shows a small meteorite impact crater in northern Tharsis.

The Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) Extended Mission has included dozens of opportunities to point the spacecraft directly at features of interest so that pictures of things not seen during the earlier Mapping Mission can be obtained. The example shown here is a small meteorite impact crater in northern Tharsis near 17.2°N, 113.8°W. Viking Orbiter images from the late 1970's showed at this location what appeared to be a dark patch with dark rays emanating from a brighter center. The MOC team surmised that the dark rays may be indicating the location of afresh crater formed by impact sometime in the past few centuries (since dark ray are quickly covered by dust falling out of the martian atmosphere). All through MOC's Mapping Mission in 1999 and 2000, attempts were made to image the crater as predictions indicated that the spacecraft would pass over the site, but the crater was never seen. Finally, in June 2001, Extended Mission operations allowed the MOC team to point the spacecraft (and hence the camera, which is fixed to the spacecraft) directly at the center of the dark rays, where we expected to find the crater.The picture on the left (above, A) is a mosaic of three MOC high resolution images and one much lower-resolution Viking image. From left to right, the images used in the mosaic are: Viking 1 516A55, MOC E05-01904, MOCM21-00272, and MOC M08-03697. Image E05-01904 is the one taken in June 2001 by pointing the spacecraft. It captured the impact crater responsible for the rays. A close-up of the crater, which is only 130 meters (427 ft) across, is shown on the right (above, B). This crater is only one-tenth the size of the famous Meteor Crater in northern Arizona.The June 2001 MOC image reveals many surprises about this feature. For one, the crater is not located at the center of the bright area from which the dark rays radiate. The rays point to the center of this bright area, not the crater. Further, the dark material ejected from the crater--immediately adjacent to the crater rim in the picture on the right (above, B)--is not continuously connected to the larger pattern of rays. Asymmetries in crater form and ejecta patterns are generally believed to occur when the impact is oblique to the surface. The offset of the crater from the center of the rays suggests that the meteor struck at an angle, most likely from the bottom/lower right (south/southeast). The strange geometry of the rays is quite different from that seen for rays associated with impact craters on the Moon and other airless bodies; one possible explanation is that they resulted from disruption of dust on the martian surface by winds generated by the shock wave as the meteor plunged through the martian atmosphere before it struck the ground.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 image from NASA's Mars Odyssey shows Granicus Valles originating from fracture systems of the Elysium Volcanic Complex. This channel system was likely produced by volcanic flows.

Context image for PIA10331Granicus VallesGranicus Valles originates from fracture systems of the Elysium Volcanic Complex. This channel system was likely produced by volcanic flows.Image information: VIS instrument. Latitude 26.8N, Longitude 132.9E. 19 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

This unnamed channel drains the highland region near Pulawy Crater as seen by NASA's 2001 Mars Odyssey spacecraft.

Context imageThis unnamed channel drains the highland region near Pulawy Crater.Orbit Number: 42871 Latitude: -37.2946 Longitude: 283.045 Instrument: VIS Captured: 2011-08-14 06:17Please 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.

This observation from NASA's Mars Reconnaissance Orbiter shows an interesting crater floor with what appear to be inverted channels, rounded lobe-like landforms, and light-toned layered deposits along the southern portion of the crater wall.

Map Projected Browse ImageClick on the image for larger versionThis observation shows an interesting crater floor with what appear to be inverted channels, rounded lobe-like landforms, and light-toned layered deposits along the southern portion of the crater wall.High resolution can help study the layers, with an enhanced-color image showing us any variations in composition between those light-toned layers and the darker-toned surfaces.This caption is based on the original science rationale.This is a stereo pair with ESP_031005_1575.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of Hebes Chasma.

Context imageThis VIS image shows a portion of Hebes Chasma.Orbit Number: 56299 Latitude: -1.25997 Longitude: 282.713 Instrument: VIS Captured: 2014-08-23 09:56Please 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 spectacular view, taken by NASA's 2001 Mars Odyssey, shows the sunlit cliffs and basaltic sand dunes in southern Melas Chasma shows Mars in a way rarely seen: in full, realistic color.

Released 14 November 2003This spectacular view of the sunlit cliffs and basaltic sand dunes in southern Melas Chasma shows Mars in a way rarely seen: in full, realistic color. The colorization is the result of a collaboration between THEMIS team members at Cornell University and space artist Don Davis, who is an expert on true-color renderings of planetary and astronomical objects. Davis began with calibrated and co-registered THEMIS VIS multi-band radiance files produced by the Cornell group. Using as a guide true-color imaging from the Hubble Space Telescope and his own personal experience at Mt. Wilson and other observatories, he performed a manual color balance to match more closely the colors of previous visual Mars observations. He also did some manual smoothing and other image processing to minimize the effects of residual scattered light in the images. The result is a view of Mars that invites comparisons to Earth; a scene that one might observe out the window on a flight over the southwest United States, but not quite. The basaltic dunes are commonplace on Mars but a rare feature on Earth. The rounded knobs and elongated mesas on the canyon floor show an erosional style as exotic as Utah's Bryce Canyon but wholly familiar on Mars. Although the inhospitable Martian atmosphere cannot be seen, the magnificent Martian landscape on display in this image beckons space-suited human explorers and the sightseers who will follow.Initial image processing and calibration by THEMIS team members J. Bell, T. McConnochie, and D. Savransky at Cornell University; additional processing and final color balance by space artist Don Davis.Image information: VIS instrument. Latitude -12.7, Longitude 288.6 East (71.4 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 taken by NASA's Mars Exploration Rover Opportunity shows the finely-laminated target called 'Cobble Hill' at 'Endurance Crater.' The circle is where the rover's rock abrasion tool cut away the rock's surface to expose the interior.

This mosaic of images taken by the microscopic imager on the Mars Exploration Rover Opportunity shows the finely-laminated target called "Cobble Hill" at "Endurance Crater." Scientists studying the target have determined that the layers within it are rich in sulfate, like many of the rocks in Endurance and "Eagle Crater" that have been investigated so far. This image comprises four separate microscopic images taken on sol 143 (June 19, 2004). The circle is where the rover's rock abrasion tool cut away the rock's surface to expose the interior. It is 4.5 centimeters (1.8 inches) in diameter.

The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false image from NASA's 2001 Mars Odyssey spacecraft shows part of Ophir 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 Ophir Chasma. The wavy edges of the image are a result of elevation variations and a unique period of spacecraft orientation.Orbit Number: 34435 Latitude: -3.7227 Longitude: 287.178 Instrument: VIS Captured: 2009-09-18 15:55Please 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, collected near the end of the southern spring season, from NASA's Mars Odyssey shows part of the south polar cap.

Context imageThis VIS image shows part of the south polar cap. This image was collected near the end of the southern spring season.Orbit Number: 74454 Latitude: -86.2332 Longitude: 299.532 Instrument: VIS Captured: 2018-09-26 18:47Please 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 diagram illustrates how the dimensions of clay minerals' crystal structure are affected by which ions are present in the composition of the mineral. Different clay minerals were identified this way at two sites, 'Yellowknife Bay' and 'Murray Buttes'

This diagram illustrates how the dimensions of clay minerals' crystal structure are affected by which ions are present in the composition of the mineral. Different clay minerals were identified this way at two sites in Mars' Gale Crater: "Murray Buttes" and "Yellowknife Bay."In otherwise identical clay minerals, a composition that includes aluminum and ferric iron ions (red dots) results in slightly smaller crystalline unit cells than one that instead includes magnesium and ferrous iron ions (green dots). Ferric iron is more highly oxidized than ferrous iron. Crystalline cell units are the basic repeating building blocks that define minerals. X-ray diffraction analysis, a capability of the Chemistry and Mineralogy (CheMin) instrument on NASA's Curiosity Mars rover, identifies minerals from their crystalline structure. The graph at PIA21147 depicts CheMin results that detected a difference in clay-mineral crystalline dimensions in samples from Murray Buttes and Yellowknife Bay.Presented at the 2016 AGU Fall Meeting on Dec. 13. in San Francisco, CA.NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington.For more information about Curiosity, visit http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl.

This image from NASA's Curiosity Mars rover, Curiosity, has been white-balanced to show what the rocks would look like if they were on Earth.

Figure AClick on the image for larger version This scene combines images taken by the left-eye camera of the Mast Camera (Mastcam) instrument on NASA's Curiosity Mars rover during the midafternoon, local Mars solar time, of the mission's 526th Martian day, or sol (Jan. 28, 2014). The sand dune in the upper center of the image spans a gap, called "Dingo Gap," between two short scarps. The dune is about 3 feet (1 meter) high. The nearer edge of it is about 115 feet (35 meters) away from the rover's position when the component images were taken, just after a Sol 526 drive of 49 feet (15 meters). The image has been white-balanced to show what the rocks would look like if they were on Earth. A version with 200-centimeter (79-inch) scale bars is available as Figure A. A version with raw color, as recorded by the camera under Martian lighting conditions, is available as Figure B.NASA's Jet Propulsion Laboratory manages the Mars Science Laboratory mission and the mission's Curiosity rover 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. Malin Space Science Systems, San Diego, built and operates Mastcam.More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/.

This color image in dark red hues shows the martian landscape at Meridiani Planum, where NASA's Mars Exploration Rover Opportunity successfully landed. A portion of the rover is in the foreground.

This color image shows the martian landscape at Meridiani Planum, where the Mars Exploration Rover Opportunity successfully landed at 9:05 p.m. PST on Saturday. This is one of the first images beamed back to Earth from the rover shortly after it touched down. The image was captured by the rover's panoramic camera.

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of the northern wall 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 northern wall of Candor Chasma.Orbit Number: 7381 Latitude: -4.72297 Longitude: 283.559 Instrument: VIS Captured: 2003-08-14 03:05Please 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.

Signs of Fluids and Ice in Acidalia Planitia

Click on image for larger versionHiRISE image (PSP_001942_2310) shows a crater approximately 11 km (7 miles) in diameter, located in Acidalia Planitia, part of the Northern Plains. Several features in and around this crater are suggestive of fluids and ice at and near the surface. The south-looking (or equator facing) walls of this crater are cut by numerous gullies such as the ones shown in this image's cutout (500 x 600 m or 550 x 650 yards), with well developed alcoves, sinuous channels, and terminal fan deposits. These gullies seem to originate at the same height, suggesting that the carving agent may have emanated from one single layer exposed in the crater's wall. Contrastingly, no gullies are observed in the north-looking (or pole facing) wall of this crater. Terrestrial gullies very similar to the ones shown in this image are produced by surface water. The arrows in the cutout show fissures that may indicate detachment of surficial materials possibly held together by subsurface ice, sliding en masse down the crater's wall. The muted topography of the crater and its surroundings, the relatively shallow floor (300 m or 330 yards), the convex slope of its walls-all are consistent with ice being present under the surface, mixed with rocks and soil. Ice would have acted as a lubricant, facilitating the flow of rocks and soils and hence smoothing landscape's features such as ridges and craters' rims.The concentric and radial fissures in the crater's floor may indicate decrease of volume due to loss of underground ice. Piles of rocks aligned along these fissures and arranged forming polygons are similar to features observed in terrestrial periglacial regions such as Antarctica. Antarctica's features are produced by repeated expansion and contraction of subsurface soil and ice, due to seasonal temperature oscillations. The funnel-shaped depressions visible in the crater's floor could be collapse pits, further evidence of ice decay; alternatively, they could be smoothed-out impact craters.Observation Toolbox Acquisition date: 12 December 2006Local Mars time: 3:23 PMDegrees latitude (centered): 50.7°Degrees longitude (East): 341.6°Range to target site: 305.9 km (191.2 miles)Original image scale range: from 30.6 cm/pixel (with 1 x 1 binning) to 61.2 cm/pixel (with 2 x 2 binning)Map-projected scale: 25 cm/pixel and north is upMap-projection: EQUIRECTANGULAREmission angle: 1.9°Phase angle: 60.1°Solar incidence angle: 58°, with the Sun about 32° above the horizonSolar longitude: 156.1°, 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.

This image from NASA's Mars Odyssey shows a portion of an unnamed channel in northern Arabia Terra.

Context imageToday's VIS image shows a portion of an unnamed channel in northern Arabia Terra. Numerous channels dissect this region of Arabia Terra where it borders the northern lowlands.Orbit Number: 86537 Latitude: 38.0081 Longitude: 34.2916 Instrument: VIS Captured: 2021-06-17 18:31Please 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 Becquerel 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 part of the floor of Becquerel Crater. The fill material has covered an older crater, which just remains as the arc of rim in the center of the image.Orbit Number: 10810 Latitude: 21.255 Longitude: 352.292 Instrument: VIS Captured: 2004-05-22 12:00Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

NASA's Mars Global Surveyor shows the south polar region of Mars in mid-May 2005.

31 May 2005This picture is a composite of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) daily global images acquired at Ls 211° during a previous Mars year. This month, Mars looks similar, as Ls 211° occurred in mid-May 2005. The picture shows the south polar region 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 Autumn/Southern Spring

This IR image from NASA's 2001 Mars Odyssey spacecraft shows streamlined islands in the channel of Mangala Valles.

Context imageThis IR image shows streamlined islands in the channel of Mangala Valles.Orbit Number: 51226 Latitude: -15.5089 Longitude: 209.731 Instrument: VIS Captured: 2013-07-01 21:39Please 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.

Most larger chasmata contain kilometer-thick light-toned layered deposits composed of sulfates. However, some of the chasmata, like Ius Chasma shown in this image from NASA's Mars Reconnaissance Orbiter, lack these deposits or have much thinner deposits.

Map Projected Browse ImageClick on the image for larger versionSedimentary deposits are common within Valles Marineris. Most of the larger chasmata contain kilometer-thick light-toned layered deposits composed of sulfates. However, some of the chasmata, like Ius Chasma shown in this HiRISE image, either lack these deposits or have much thinner deposits.The light-toned deposits in Ius Chasma are observed both along the floor and inner wallrock materials. Some of the light-toned deposits appear to post-date formation of the chasma floor, whereas other deposits appear to lie beneath wallrock materials, indicating they are older. By examining the stratigraphy using digital terrain models and 3D images, it should be possible to decipher the relative ages of the different geologic units. CRISM data may also provide insight into the mineralogy, which will tell scientists about the aqueous conditions that emplaced the light-toned deposits.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 the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.

Twelve orbits a day provide NASA's Mars Global Surveyor MOC wide angle cameras a global 'snapshot' of weather patterns across the planet. Here, bluish-white water ice clouds hang above the Tharsis volcanoes.

Twelve orbits a day provide the Mars Global Surveyor MOC wide angle cameras a global "snapshot" of weather patterns across the planet. Here, bluish-white water ice clouds hang above the Tharsis volcanoes. This computer generated image was created by wrapping the global map found at PIA02066 onto a sphere. The center of this newly [sic] projected sphere is located at 15degrees North, 90 degrees West. This perspective rotates the south pole (which has no data coverage in the original map) away from our field of view.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 right image of a stereo image pair taken on the afternoon of Sol 74 (September 17) shows NASA's Sojourner rover behind the rock 'Chimp.' Sojourner is now a record 12.3 m from the lander. Sol 1 began on July 4, 1997.

This right image of a stereo image pair taken on the afternoon of Sol 74 (September 17) shows the Sojourner rover behind the rock "Chimp." Sojourner is now a record 12.3 m from the lander.This image and PIA01580 (left eye) make up a stereo pair.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 an operating 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.

The bizarre patterns on the floor of this crater in Nilosyrtis Mensae imaged by NASA's Mars Odyssey defy an easy explanation. It is possible that some form of periglacial process combined with the vaporization of ground ice to form these patterns.

The bizarre patterns on the floor of this crater in Nilosyrtis Mensae defy an easy explanation. At 34 degrees north latitude, this location hardly qualifies as "Arctic" yet it is likely that some form of periglacial process possibly combined with the vaporization of ground ice is responsible for this intriguing landscape.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.Image information: VIS instrument. Latitude 10.3, Longitude 24.5 East (284.5 West). 19 meter/pixel resolution.

NASA's Mars Global Surveyor shows

MGS MOC Release No. MOC2-508, 9 October 2003Arabia Terra is a vast, heavily cratered region in the martian northern hemisphere. Much of Arabia Terra is thickly blanketed by dust. From time to time, on steep slopes, the dust will avalanche or slide downhill, creating a streak. The majority of slope streaks are darker than their surroundings, but not all of them are dark. In Arabia, it is common to find bright and dark slope streaks, and to find them together. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows an example, taken from a crater near 10.5°N, 318.4°W. Why some streaks are bright and others are dark is not yet known. This picture covers an area 3 km (1.9 mi) wide and is illuminated by sunlight from the left.

This image shows the bright deposit remaining on the floor of Pollack on Mars as seen by NASA's 2001 Mars Odyssey spacecraft.

Context image for PIA08591Martian Color #7This image shows the bright deposit remaining on the floor of Pollack Crater.This color treatment is the result of a collaboration between THEMIS team members at Cornell University and space artist Don Davis, who is an expert on true-color renderings of planetary and astronomical objects. Davis began with calibrated and co-registered THEMIS VIS multi-band radiance files produced by the Cornell group. Using as a guide true-color imaging from spacecraft and his own personal experience at Mt. Wilson and other observatories, he performed a manual color balance to display the spectral capabilities of the THEMIS imager within the context of other Mars observations. He also did some manual smoothing along with other image processing to minimize the effects of residual scattered light in the images.Image information: VIS instrument. Latitude -8.0N, Longitude 24.9E. 35 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.

Peace' Rock Viewed by Spirit

NASA's Mars Exploration Rover Spirit photographed this scene on the slope of "Husband Hill" during the rover's 369th martian day, or sol (Jan. 5, 2005). The rock at the center of the frame was informally named "Peace." Spirit subsequently inspected the rock with the tools on the rover's robotic arm. This image was taken with the panoramic camera, through the camera's 430-nanometer filter.

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

Context imageThe THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of Coprates Chasma.Orbit Number: 1613 Latitude: -14.2491 Longitude: 304.056 Instrument: VIS Captured: 2002-04-26 07:57Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

This series of images shows NASA's Perseverance rover inspecting and sealing a witness sample tube on June 21, 2021, as it prepares to collect its first sample of Martian rock and sediment.

Click here for animationAs part of its search for signs of ancient life on Mars, Perseverance is the first rover to bring a sample caching system to the Red Planet that will package promising samples for return to Earth by a future mission. This series of images shows NASA's Perseverance rover inspecting and sealing a "witness" sample tube on June 21, 2021 (the 120th sol, or Martian day, of the mission), as it prepares to collect its first sample of Martian rock and sediment.Witness tubes are similar to the sample tubes that will hold Martian rock and sediment, except they have been preloaded with a variety of materials that can capture molecular and particulate contaminants. They are opened on the Martian surface to "witness" the ambient environment near sample collection sites. With samples returned to Earth in the future, the witness tubes would show whether Earth contaminants were present during sample collection. Such information would help scientists tell which materials in the Martian samples may be of Earth origin.The sampling system's dedicated camera, the Cachecam, captured these images. 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

NASA's 2001 Mars Odyssey spacecraft shows the apparent effects of wind and water mark the surface of this region just northeast of Gusev Crater.

Context imageThe apparent effects of wind and water mark the surface of this region just northeast of Gusev Crater.Orbit Number: 47269 Latitude: -12.9541 Longitude: 176.39 Instrument: VIS Captured: 2012-08-10 06:09Please 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.

Elorza Crater is a complex crater located north of Coprates Chasma. This image from NASA's Mars Reconnaissance Orbiter centers on the southwestern portion of the central uplift, characterized by numerous bedrock exposures and coherent impact melt flows.

Map Projected Browse ImageClick on the image for larger versionElorza Crater is an approximately 40-kilometer diameter complex crater located at 304.8 degrees east, 8.76 degrees north, about 300 kilometers north of Coprates Chasma. This image centers on the southwestern portion of the central uplift, and is characterized by numerous bedrock exposures and coherent impact melt flows.The distinguishing feature of this central uplift is the various types of bedrock that are observable at the surface. This image shows uplifted massive fractured bedrock that is visible directly adjacent to dark-toned flow materials, which are interpreted to be impact melt flows.At full resolution, it is possible to distinguish the stratigraphic relationship between these two units; the impact melt appears to be eroding up the slope, exposing the underlying bedrock. Examining an image from the Compact Reconnaissance Imaging Spectrometer for Mars (or CRISM, another instrument on MRO), a spectral signature can be observed that strongly correlates with this exposed bedrock, which is consistent with opaline silica.Directly northwest of this feature is uplifted bedrock with distinct intact layering, a common feature visible in central uplifts of impact craters near Valles Marineris. Understanding where each bedrock unit originated, and how it was subsequently exposed during the impact process, is a complex problem that relies upon synthesizing several remote sensing data sets available for Mars.Refer to the caption for ESP_021551_1710 for an image covering almost the full width of Elorza's central uplift.HiRISE is one of six instruments on NASA's Mars Reconnaissance Orbiter. 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 the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.

This image shows the rocky road NASA's Mars Exploration Rover Spirit traveled to reach its ultimate destination the Columbia Hills.

Figure 1 (labels)This image shows the rocky road the Mars Exploration Rover Spirit will travel to reach its ultimate destination - the Columbia Hills. The hills, seen here in the background, are located 2.3 kilometers (1.4 miles) away in the southeast direction. Rover planners estimate the journey will take about two months, or 60 sols, including stops at interesting targets along the way. As of sol 81 (March 26, 2004), Spirit has traveled 492 meters (1614 feet).

Spirit Begins Third Martian Year

As it finished its second Martian year on Mars, NASA's Mars Exploration Rover Spirit was beginning to examine a group of angular rocks given informal names corresponding to peaks in the Colorado Rockies. A Martian year— the amount of time it takes Mars to complete one orbit around the sun—lasts for 687 Earth days. Spirit completed its second Martian year on the rover's 1,338th Martian day, or sol, corresponding to Oct. 8, 2007.Two days later, on sol 1,340 (Oct. 10, 2007), Spirit used its front hazard-identification camera to capture this wide-angle view of its robotic arm extended to a rock informally named "Humboldt Peak." For the rocks at this site on the southern edge of the "Home Plate" platform in the inner basin of the Columbia Hills inside Gusev Crater, the rover team decided to use names of Colorado peaks higher than 14,000 feet. The Colorado Rockies team of the National League is the connection to the baseball-theme nomenclature being used for features around Home Plate.The tool facing Spirit on the turret at the end of the robotic arm is the Moessbauer spectrometer.

This channel feature in Ceraunius Fossae on Mars looks like a hooded cobra spitting venom as seen by NASA's Mars Odyssey spacecraft.

Context image for PIA09160THEMIS ART #78This channel feature in Ceraunius Fossae looks like a hooded cobra spitting venom.Image information: VIS instrument. Latitude 28.3N, Longitude 250.2E. 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.

NASA's Curiosity Mars rover is depicted in this 3D rendering of Gediz Vallis Ridge that was created using science data and imagery captured from space by the agency's Mars Reconnaissance Orbiter.

NASA's Curiosity Mars rover can be seen in this 3D rendering of Gediz Vallis Ridge, a formation the mission's science team has long sought to explore. It took the mission four attempts over three years to finally reach the ridge in mid-August 2023. This rendering was created using science data and imagery captured from space by NASA's Mars Reconnaissance Orbiter.Curiosity team member Alex Bryk made the rendering using the same software the team uses to chart Curiosity's route up Mount Sharp, which the rover has been ascending since 2014. Where Curiosity appears in this image, the ridge is estimated to be nearly 70 feet (21 meters) tall. After spending Aug. 14-25 at the ridge, Curiosity departed to drive farther up the mountain; the rover's team will be searching for a path to the left side of the channel that's seen at the top of this image.Curiosity was built by NASA's Jet Propulsion Laboratory, which is managed by Caltech in Pasadena, California. JPL leads the mission on behalf of NASA's Science Mission Directorate in Washington.For more about Curiosity, visit: http://mars.nasa.gov/msl

This image from NASA's Mars Odyssey shows part of the large hill near the eastern edge of Candor Chasma.

Context imageToday's VIS image shows part of the large hill near the eastern edge of Candor Chasma. Layering is visible toward the bottom of the image. The sides of the hill are deeply incised by erosion, probably including both wind and water processes. Candor Chasma is one of the largest canyons that make up Valles Marineris. It is approximately 810 km long (503 miles) and has is divided into two regions - eastern and western Candor. Candor is located south of Ophir Chasma and north of Melas Chasma. The border with Melas Chasma contains many large landslide deposits. The floor of Candor Chasma includes a variety of landforms, including layered deposits, dunes, landslide deposits and steep sided cliffs and mesas. Many forms of erosion have shaped Candor Chasma. There is evidence of wind and water erosion, as well as significant gravity driven mass wasting (landslides).Orbit Number: 88687 Latitude: -7.91852 Longitude: 294.829 Instrument: VIS Captured: 2021-12-11 18:58Please 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.

NASA's Mars Exploration Rover Spirit acquired this imageMarch 15, 2004, after digging its wheel into the drift dubbed 'Serpent' creating the scar that allowed the rover's instruments to see below the drift surface.

The Mars Exploration Rover Spirit acquired this navigation camera image on the 72nd martian day, or sol, of its mission (March 15, 2004), after digging its wheel into the drift dubbed "Serpent." Creating the commands that would generate this "scar" was not an easy task for rover controllers. Essentially, they had to choreograph an intricate dance for Spirit, maneuvering it up the side of the dune, shimmying its left front wheel a number of times to create the scuff, and then reversing to attain proper positioning for miniature thermal emission spectrometer observations. Before the task was finished, Spirit moved forward to put the scuff within proper reach of the rover's arm. This scar allows the rover's instruments to see below the drift surface, to determine the composition of the materials. Initial results indicate that the drift material is similar to the basaltic sands that have been seen throughout Spirit's journey to the large crater dubbed "Bonneville." The material does not seem to be the same as that inside the crater.Scientists are now looking to answer two questions: Why is the dark sand in the crater not the same as the dark sand in the drift? And why are there two different dark soil-type deposits in such a small place?

This image from NASA's Mars Odyssey shows some of the tectonic faults in the Tharsis region.

Context imageThe Tharsis region of Mars is an immense region of volcanos, lava flows, and tectonic faulting. The entire area is a topographic bulge, with extensional stresses. The extension allowed magma to rise to the surface, creating the largest areal (Alba Mons) and tallest (Olympus Mons) volcanoes in the solar system. The extension also created faults and fractures. This VIS image shows some of the tectonic faults in the region.Orbit Number: 81214 Latitude: 10.0823 Longitude: 240.355 Instrument: VIS Captured: 2020-04-05 11:31Please 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 several windstreaks located on the volcanic plains of Daedalia Planum.

Context imageThis VIS images shows several windstreaks located on the volcanic plains of Daedalia Planum. The dark and bright material forming "tails" behind the craters were created by surface winds funneled over and around the crater. The raised rims and bowls of impact craters causes a complex interaction such that the wind vortex in the lee of the crater can both scour away the surface dust and deposit it back in the center of the lee. The "tail" shows the direction of the wind, in this case blowing from the right to the left.Orbit Number: 80441 Latitude: -13.1034 Longitude: 223.8 Instrument: VIS Captured: 2020-02-01 19:50Please 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 Reconnaissance Orbiter captured this image of a meteoroid impact that was first detected by the agency's InSight lander using its seismometer. This crater was formed on Feb. 18, 2021.

NASA's Mars Reconnaissance Orbiter captured this image of a meteoroid impact that was first detected by the agency's InSight lander using its seismometer. This crater was formed on Feb. 18, 2021.MRO's High Resolution Imaging Science Experiment (HiRISE) camera captured this scene in color. The ground is not actually blue; this enhanced-color image highlights certain hues in the scene to make details more visible to the human eye – in this case, dust and soil disturbed by the impact.NASA's Jet Propulsion Laboratory in Southern California manages both InSight and MRO for the agency's Science Mission Directorate in Washington. The University of Arizona, in Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., in Boulder, Colorado.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 provided the Seismic Experiment for Interior Structure (SEIS) instrument to NASA, with the principal investigator at IPGP (Institut de Physique du Globe de Paris). Significant contributions for SEIS came from IPGP; the Max Planck Institute for Solar System Research (MPS) in Germany; the Swiss Federal Institute of Technology (ETH Zurich) in Switzerland; Imperial College London and Oxford University in the United Kingdom; and JPL. DLR provided the Heat Flow and Physical Properties Package (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 temperature and wind sensors.

Two name plates mounted on the Mars Perseverance rover's robotic arm are visible in this composite image, made from photos taken by the rover's left Navcam on Sol 12 of its mission (March 2, 2021).

Two name plates mounted on the Mars Perseverance rover's robotic arm are visible in this composite image, made from photos taken by the rover's left Navcam on Sol 12 of its mission (March 2, 2021). The rover's name, "Perseverance," is inscribed on the plate attached to its forearm, and the mission name, "Mars 2020," is shown on its upper arm. Running vertically along the right side of the mission name plate is a string of 17 letters and numbers. These characters form a unique product identification number (PIN) similar to the Vehicle Identification Number (VIN) on vehicles on Earth, but signifying that this is an off-road vehicle. Issued in part by the Society of Automotive Engineers, a PIN or VIN number provides a unique vehicle identifier, while encoding information about the vehicle's characteristics and manufacture. Perseverance's PIN can be decoded to reveal clues about its destination, mission objective and power source.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: mars.nasa.gov/mars2020

This image captured by NASA's 2001 Mars Odyssey spacecraft shows layering in the south polar cap.

Context imageToday's VIS image shows layering in the south polar cap.Orbit Number: 56524 Latitude: -84.4456 Longitude: 315.349 Instrument: VIS Captured: 2014-09-10 22:04Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

This observation from NASA's Mars Reconnaissance Orbiter is of one many that highlights new discoveries; one of these is that many sand dunes and ripples are moving, some at rates of several meters per year.

Having operated at Mars for more than seven years, MRO and the HiRISE camera continue to make new discoveries. One of these is that many sand dunes and ripples are moving, some at rates of several meters per year.In this observation, a dune field in a Southern hemisphere crater was observed approximately one Mars year apart, first on 2 September 2011 and then again on 11 July 2013 (a year on Mars is 687 Earth days). By taking images at the same time of year, solar illumination angles are the same, so that subtle apparent changes can be linked to true displacement on the surface and not artifacts.In these two images, there is little distortion (a digital elevation model would remove more distortion). Here, we focus on the southern and northern part of two adjacent dunes. With an animated image, the displacement of ripples on the dunes relative to nearby rocks and dark ripples are clearly visible. It seems that the ripples on the southern dune are moving northeast, while those on the northern dune are moving west, indicating complex winds in this area. The static dark ripples may be composed of larger grains than those in the dunes and are therefore harder to move.In most areas of Mars, darker-toned ripples are more mobile than lighter ones. This area is different, demonstrating that continued imaging of the Martian surface results in new findings and revisions of ideas.This is a stereo pair with ESP_032748_1275.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. Data from the filters can be combined in many ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows the region just west of the dune/polar cap image from earlier this week.

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 the region just west of the dune/polar cap image from earlier this week. The polar cap is at the bottom of the image.Orbit Number: 17045 Latitude: -71.5569 Longitude: 142.96 Instrument: VIS Captured: 2005-10-17 18:56Please 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.

Pot of Gold' and 'Rotten Rocks'

This false-color image taken by the panoramic camera on the Mars Exploration Rover Spirit shows the rock dubbed "Pot of Gold" (upper left), located near the base of the "Columbia Hills" in Gusev Crater. Scientists are intrigued by this unusual-looking, nodule-covered rock and plan to investigate its detailed chemistry in coming sols. This picture was taken on sol 159 (June 14, 2004).To the right is a set of rocks referred to as "Rotten Rocks" for their resemblance to rotting loaves of bread. The insides of these rocks appear to have been eroded, while their outer rinds remain more intact. These outer rinds are reminiscent of those found on rocks at Meridiani Planum's "Eagle Crater." This image was captured on sol 158 (June 13, 2004).

NASA's Mars Reconnaissance Orbiter captured this image of the Claritas Fossae region, characterized by systems of 'graben.' A graben forms when a block of the planet's crust drops down between two faults, due to extension, or pulling, of the crust.

The Claritas Fossae region is characterised by systems of "graben" running mainly north-west to south-east. A graben forms when a block of the planet's crust drops down between two faults, due to extension, or pulling, of the crust.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, 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 & Technologies Corp., Boulder, Colo.Originally released July 13, 2011

This image acquired on October 27, 2021 by NASA's Mars Reconnaissance Orbiter, shows the crater that defines where zero longitude is on Mars, like the Greenwich Observatory does for the Earth.

Map Projected Browse ImageClick on image for larger versionThe crater in the center of this HiRISE image defines where zero longitude is on Mars, like the Greenwich Observatory does for the Earth.Originally, the larger crater that this crater sits within, called Airy Crater, defined zero longitude for the Red Planet. But as higher resolution images became available, a smaller feature was needed. This crater, called Airy-0 (zero), was selected because it would require no adjustment of existing maps.These days, longitude on Mars is measured even more precisely using radio tracking of landers such as InSight, but everything is still defined to keep zero longitude centered on this crater.The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. (The original image scale is 59.1 centimeters [23.3 inches] per pixel [with 2 x 2 binning]; objects on the order of 177 centimeters [69.7 inches] across are resolved.) North is up.This is a stereo pair with ESP_070869_1750.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, part of THEMIS art month, taken by NASA's Mars Odyssey features a portion of Mars' landscape looking like a link from a bicycle chain.

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!With this, we end our second annual art month. So that's where that link from my bicycle chain got to...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 small portion of Kasei Valles. The channel rim at the top of the image shows a complex series of processes.

Context imageThis VIS image shows a small portion of Kasei Valles. The channel rim at the top of the image shows a complex series of processes. The crater was the source of the landslide material - either as emplacement of ejecta or from collapse of the rim. To the right of the crater is a semi-circular feature that appears to have collapsed and created blocks of material. A relative time relationship in this image seems to be creation of the channel, impact formation and the ejecta/collapse of the crater, and then the collapse of the material in the semi-circular feature. These events could have happened days apart or millions of years apart.Orbit Number: 62563 Latitude: 24.1942 Longitude: 297.136 Instrument: VIS Captured: 2016-01-21 05:16Please 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.

This unnamed channel is located east of Baetis Chaos as seen by NASA's 2001 Mars Odyssey spacecraft.

Context imageThis unnamed channel is located east of Baetis Chaos.Orbit Number: 48738 Latitude: -0.645607 Longitude: 301.829 Instrument: VIS Captured: 2012-12-09 03:40Please 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.

This artist's depiction shows the close encounter between comet Siding Sprng and Mars in 2014. The comet's powerful magnetic field temporarily merged with, and overwhelmed, the planet's weak magnetic field.

The close encounter between comet Siding Spring and Mars in 2014 flooded the planet with an invisible tide of charged particles from the comet's coma. The dense inner coma reached the surface of the planet, or nearly so. The comet's powerful magnetic field temporarily merged with, and overwhelmed, the planet's weak magnetic field, as shown in this artist's depiction.NASA's Mars Atmosphere and Volatile Evolution (MAVEN) mission used the orbiter's magnetometer to monitor how the passing comet affected the magnetic field around Mars.NASA Goddard Space Flight Center in Greenbelt, Maryland, manages the MAVEN project for NASA's Science Mission Directorate, Washington, and built the mission's magnetometer. MAVEN's principal investigator is based at the University of Colorado's Laboratory for Atmospheric and Space Physics in Boulder. Lockheed Martin Space Systems, Denver, built and operates the spacecraft. For more information about MAVEN, visit http://www.nasa.gov/maven and http://lasp.colorado.edu/home/maven/.For more information about NASA's Mars Exploration Program, see http://marsprogram.jpl.nasa.gov.

Olivine in the Southern Isidis Basin

The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) took this observation of the transition region between Libya Montes and the Isidis Basin on Mars at 17:16 UTC (12:16 p.m. EST) on January 2, 2007, near 3.6 degrees north latitude, 84.1 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 of a gigantic impact on the surface of Mars early in the planet's history. The southern rim, where this target is located, is a region of complex geology and part of the planetary dichotomy boundary that separates the older southern highlands from the lower, younger northern plains. The image on the left was constructed from three visible wavelengths (RGB: 0.71, 0.60, 0.53 microns) and is a close approximation of how the surface would appear to the human eye. The image on the right was constructed from three infrared wavelengths (RGB: 2.49, 1.52, 1.08 microns) chosen to highlight variations in the mineralogy of the area. Of interest is that features in this image not only differ in color, but also in texture and morphology. The gray areas absorb similarly at all wavelengths used in this image, but display absorptions at other wavelengths related to the iron- and magesium-rich mineral pyroxene. The reddest areas absorb strongly at the wavelengths used for green and blue, which is attributable to another iron- and magesium-rich mineral, olivine. The brownish areas show subdued mineral absorptions and could represent some type of mixture between the other two materials. The presence of the mineral olivine is particularly interesting because olivine easily weathers to other minerals; thus, its presence indicates either the lack of weathering in this region or relatively recent exposure.CRISM's mission: Find the spectral fingerprints of aqueous and hydrothermal deposits and map the geology, composition and stratigraphy of surface features. The instrument will also watch the seasonal variations in Martian dust and ice aerosols, and water content in surface materials -- leading to new understanding of the climate.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.

Geologists aren't quite sure what to make of the dark splotch in the middle of this image from NASA's Mars Reconnaisance Orbiter (MRO), one of several similar dark splotches that extend east and west for over 100 kilometers.

Map Projected Browse ImageClick on the image for larger versionGeologists aren't quite sure what to make of the dark splotch in the middle of this image from NASA's Mars Reconnaisance Orbiter (MRO) -- one of several similar dark splotches that extend east and west for over 100 kilometers. From measurements made in infrared, this and other dark splotches have what we call "high thermal inertia," meaning that it heats up and cools down slowly. Scientists use thermal inertia to assess how rocky, sandy, or dusty a place is. A higher thermal inertia than the surrounding area means it's less dusty.Wavy, banded patterns in the dark splotch (possibly due to cross bedding from sand dunes that once occupied the area) were lithified into sandstone, and then eroded away. These clues could help geologists figure out what's going on there.This is a stereo pair with PSP_008935_1975. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 28.1 centimeters (11 inches) per pixel (with 1 x 1 binning); objects on the order of 56.3 centimeters (22.2 inches) across are resolved.] North is up. The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.

This image captured by NASA's 2001 Mars Odyssey spacecraft continues to follow the channel seen in the past two images. The rover landing site is at the top margin of this image.

Context imageDuring the month of April Mars will be in conjunction relative to the Earth. This means the Sun is in the line-of-sight between Earth and Mars, and communication between the two planets is almost impossible. For conjunction, the rovers and orbiting spacecraft at Mars continue to operate, but do not send the data to Earth. This recorded data will be sent to Earth when Mars moves away from the sun and the line-of-sight between Earth and Mars is reestablished. During conjunction the THEMIS image of the day will be a visual tour of Gale Crater, the location of the newest rover Curiosity. Today's image continues to follow the channel seen in the past two images. The rover landing site is at the top margin of this image.Orbit Number: 1494 Latitude: -5.03202 Longitude: 137.326 Instrument: VIS Captured: 2002-04-16 12:47 Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

Shadows cast by the high walls and high hills within Candor Chasma are visible in this image from NASA's 2001 Mars Odyssey spacecraft. The local time is near 5:00 in the afternoon.

Context imageShadows cast by the high walls and high hills within Candor Chasma are visible in this image. The Odyssey spacecraft and THEMIS camera are passing over the surface of Mars at a local time near 5 in the afternoon. The sun is close to the western horizon and shadows are being created by tall topographic features.Orbit Number: 52547 Latitude: -6.7789 Longitude: 290.464 Instrument: VIS Captured: 2013-10-18 14:20Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

This image, taken by NASA's Mars Reconnaissance Orbiter spacecraft, is of an area on the lower southeastern flank of the volcano Elysium Mons. A small, dark pristine-appearing pit is clearly visible among the numerous small impact craters.

Map Projected Browse ImageClick on the image for larger versionThis image was taken of an area on the lower southeastern flank of the volcano Elysium Mons. In the center is a small, dark pristine-appearing pit approximately 130 meters in diameter, which is clearly visible among the numerous small impact craters that are heavily covered by dust and sediment. These pit craters are usually appear in the younger Tharsis volcanic region, but this is one of the first seen in the older Elysium volcanic region.Garden variety craters are excavated by impacts and are characterized by raised rims, sloped walls and surrounded by ejecta blankets, but pit craters are simply sink holes in the ground with near vertical walls and floors that are only visible when the sun is high in the sky. They are deep holes that may lead to underground caves in volcanic terrain. This isolated pit crater is located in a lava field that is crisscrossed by long, linear troughs.A commonly invoked hypothesis to explain these troughs is that they are collapsed lava tubes, essentially tunnels formed by underground rivers of lava. Lava tube collapse may begin with the buckling of its roof at one location where the roof is thinnest. At this point, light enters into the permanent darkness of the cave from above, forming a skylight. Pits or skylights are distinct from impact craters: they appear as dark, roughly circular shadowed holes because of their steep walls, while the shadows cast by impact craters generally shade only a portion of the crater floor, because the slopes of the walls are shallower. When this picture was taken, sunlight directly lit part of the floor of this pit crater, illuminating the large boulders (see close up image) on its southeastern slope.The first skylights were discovered in 2007 on Mars, and in 2009 on the Moon. The famous Devil's Throat is Hawaii is a good Earth-example: it's 50 meters wide and accessible by foot. Pit craters provide a window into the subsurface structure of Mars, and prior to collapse, might have also provided potential habitats where organisms could be protected from the harsh, sterilizing UV radiation experienced at the surface.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.

This image shows part of the large unnamed crater located on Acheron Fossae. Numerous channels dissect the crater rim and the crater floor has a rugged texture on Mars as seen by NASA's Mars Odyssey spacecraft.

Context image for PIA09136 Large CraterThis image shows part of the large unnamed crater located on Acheron Fossae. Numerous channels dissect the crater rim and the crater floor has a rugged texture.Image information: VIS instrument. Latitude 39.4N, Longitude 224.5E. 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 Global Surveyor shows a very small portion of the hundreds-of-kilometers-long Marte Vallis system and results of catastrophic flooding. Marte is the Spanish word for Mars.

16 December 2005This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows the results of catastrophic flooding in Marte Vallis, Mars. Marte is the Spanish word for Mars. Many of the major valleys on the red planet are named for the word for "Mars" in the various languages of Earth. This image shows just a very small portion of the hundreds-of-kilometers-long Marte Vallis system.Location near: 17.4°N, 174.7° Image width: width: ~3 km (~1.9 mi)Illumination from: lower left Season: Northern Winter

Dust Accumulation on Mars

Since landing on Mars a year ago, NASA's pair of six-wheeled geologists have been constantly exposed to martian winds and dust. As a result, the Spirit rover has gradually experienced a slight decline in power as a thin layer of dust has accumulated on the solar panels, blocking some of the sunlight that is converted to electricity. In this enlarged image of a postage-stamp-size (3-centimeter-square, 1.2-inch-square) portion of one of Spirit's solar panels, a fine layer of martian dust coats electrical connections and metal surfaces. Individual silt grains or clumps of dust are visible where sediment has accumulated in crevices between solar cells and circuits. The upper right half of the image shows the edge of one of the rover's solar cells. The lower left half shows electrical wires bonded with silicon adhesive to the underlying composite surface; the circular abrasions are the result of sanding by hand on Earth. The braided wire is connected to a thermocouple used to measure temperature based on electrical resistance. Spirit took this image with its microscopic imager on martian day, or sol, 350 (Dec. 26, 2004).

Spirit Nears North-Tilting Site for Winter Haven

NASA's Mars Exploration Rover Spirit made daily progress in early December 2007 toward the northern edge of a low plateau called "Home Plate." The rover's operators selected an area with north-facing slope there (indicated by the blue-outlined rectangle) as a destination where Spirit would have its best chance of surviving low-solar-energy conditions of oncoming Martian winter.As indicated by the yellow line tracing the path Spirit has driven, the rover was near the western edge of the plateau on Sol (Martian day) 1,390 of the mission (Nov. 30, 2007), but nearing the northern edge by Sol 1,397 (Dec. 8, 2007).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.

NASA's Mars Global Surveyor shows

29 December 2003Small dust storms are common in the south polar region during summer. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows an example of a south polar dust-raising event caught by the narrow angle camera. The small, somewhat circular features at the lower right of the frame are pits in the martian surface. Moving from the bottom to top of the image, first there is a view of the pitted surface, followed by a zone of long, thin streamers of dust being lifted from the surface, followed by -- at the top one third of the image -- the billowy clouds of the dust storm. This image is important because it shows long, thin streamers of dust actually being raised from the martian surface to feed the dust storm. The picture is located near 87.0°S, 170.6°W. The area shown is about 3 km (1.9 mi) wide; sunlight illuminates the scene from the upper left.

This image captured by NASA's 2001 Mars Odyssey spacecraft crosses the summit of Ceraunius Tholus.

Context imageToday's VIS image crosses the summit of Ceraunius Tholus.Orbit Number: 55057 Latitude: 24.5638 Longitude: 263.026 Instrument: VIS Captured: 2014-05-13 05:27Please 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.

These dark streaks, also known as slope streaks, resulted from dust avalanches on Mars. The HiRISE camera aboard NASA's Mars Reconnaissance Orbiter captured them on Dec. 26, 2017.

These dark streaks, also known as "slope streaks," on Mars resulted from dust avalanches. They were captured by NASA's Mars Reconnaissance Orbiter using its High-Resolution Imaging Science Experiment (HiRISE) camera on Dec. 26, 2017.NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages MRO for NASA's Science Mission Directorate in Washington. The University of Arizona, in Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., in Boulder, Colorado.

This image from NASA's Mars Reconnaissance Orbiter shows the west-facing side of an impact crater in the mid-latitudes of Mars' northern hemisphere. This crater has gullies along its walls that are composed of alcoves, channels and debris aprons.

This image shows the west-facing side of an impact crater in the mid-latitudes of Mars' northern hemisphere. The High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter took the image on April 13, 2010. It is one of 600 recent HiRISE observations newly released to NASA's Planetary Data System.Like many mid-latitude Martian craters, this one has gullies along its walls that are composed of alcoves, channels and debris aprons. The origins of these gullies have been the subject of much debate; they could have been formed by flowing water, liquid carbon dioxide or dry granular flows. The orientation of these gullies is of interest because many craters contain gullies only on certain walls, such as those that are pole-facing. This could be due to changes in orbital conditions affecting long-term climate cycles and differences in solar heating along specific walls.Many of the other features observed in and around this crater are indicative of an ice-rich terrain, which may lend credence to the water formation hypothesis for these gullies. The most notable of these features is "scalloped" terrain in and around the crater. This type of terrain has been interpreted as a sign of surface caving, perhaps due to sublimation of underlying ice. (Sublimation is the process of a solid changing directly to a gas.)Another sign of ice is the presence of parallel lines and pitted material on the crater floor, similar to what is referred to as concentric crater fill. Parallel linear cracks are also observed along the crater wall over the gullies, which could be due to thermal contraction of ice-rich material.All of these features taken together are evidence for ice-rich material having been deposited in this region during different climatic conditions, material that has subsequently begun to melt and/or sublimate under current conditions. More recently, wind-blown deposits have accumulated around the crater, as evidenced by the parallel ridges dominating the landscape. Dust devil streaks are also visible crossing the wind-sculpted ridges.This image spans a distance of about 1.2 kilometers (three-fourths of a mile) and is presented in false color, which aids in distinguishing among surface materials and textures. It is a portion of the HiRISE observation catalogued as ESP_017405_2270, of an area centered at 46.7 degrees north latitude, 90.2 degrees east longitude. Other image products from this observation are available at http://hirise.lpl.arizona.edu/ESP_017405_2270. 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, 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 & Technologies Corp., Boulder, Colo.

NASA's Mars Global Surveyor shows a circular depression and a suite of eroding mesas of carbon dioxide. These features occur in the south polar residual cap of Mars.

14 August 2005This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a circular depression and a suite of eroding mesas of carbon dioxide. These features occur in the south polar residual cap of Mars. The eroding carbon dioxide creates landforms reminiscent of "Swiss cheese." The circular feature might indicate the location of a filled, buried impact crater.Location near: 86.8°S, 111.0°W Image width: width: ~3 km (~1.9 mi) Illumination from: upper left Season: Southern Spring

Two of NASA's Mars Exploration Rover Spirit's potential target rocks, which are near the rock called Adirondack in Gusev Crater.

These are the first images sent back from the panoramic camera on the Mars Exploration Rover Spirit since the rover experienced communications problems on the 18th sol, or martian day, of its mission. They were acquired at Gusev Crater, Mars, on Sol 26 (Jan. 29, 2004), showing that the camera's health remained excellent during Spirit's recovery. Two of Spirit's potential target rocks, which are near the rock called Adirondack, can be seen on the lower left and right. The rock on the left has been named "Cake," and the white rock on the right has been named "Blanco."In the upper left is a color image of the panoramic camera calibration target, also known as the martian sundial. The color panel of the calibration target looks almost exactly like it did on Earth, indicating that the color shown of Mars, though approximated, is close to true color.The monochrome image in the upper right shows the sun, magnified five times. This image was acquired by the panoramic camera as part of a routine sequence of images designed to monitor the dust abundance in the martian atmosphere. The dust abundance appears to be decreasing slowly with time, consistent with the atmosphere continuing to clear after the large dust storm of last December.

Spirit Sol 154, Driving By

This image was taken by NASA's Mars Exploration Rover Spirit's front hazard avoidance camera during Spirit's 154th martian day, or sol, on June 9, 2004. The "Columbia Hills" appear against the horizon. Directly in front of the rover is the highest of the hills, "Husband Hill," approximately 90 meters (295 feet) tall. The rock in the foreground is larger than other surrounding rocks, approximately 35 centimeters (14 inches) across, but was not an observation target for Spirit. The tread marks in front of the rock are not a trench, but simply evidence that the rover passed by as it continued its journey toward the Columbia Hills.

This image from NASA's Mars Odyssey spacecraft shows the summit of Arsia Mons.

Context image for PIA09994Arsia MonsThis VIS image was collected during the major Martian dust storm of 2007. The amount of dust filled atmosphere was thinner over the high altitude summits of the Tharsis volcanoes. This image shows the summit of Arsia Mons.Image information: VIS instrument. Latitude -9.6N, Longitude 238.7E. 35 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

This image from the Mars Exploration Rover Opportunity focuses on a target called 'Goal 5' a wind-rippled spot on the upper part of the crater, higher in hematite content compared to other soils within the crater.

This image from the Mars Exploration Rover Opportunity's front hazard-avoidance camera focuses on a target called "Goal 5." Goal 5, examined during the "Eagle Crater" soil survey, is a wind-rippled spot on the upper part of the crater, which the miniature thermal emission spectrometer shows is higher in hematite content compared to other soils within the crater. The light soil in the center of the image is referred to as "Lanikai" -- an inspiration from the white sand beaches of Hawaii. The dark soil is referred to as "Punaluu" after the black sand Hawaiian beaches.

This image from NASA's Mars Odyssey shows a small portion of the immense lava flows that originated from Arsia Mons.

Context imageToday's VIS image shows a small portion of the immense lava flows that originated from Arsia Mons. Arsia Mons is the southernmost of the three large aligned volcanoes in the Tharsis region. Arsia Mons last eruption was 10s of million years ago. The youngest volcano in the region is Olympus Mons, the largest volcano in our solar system.Orbit Number: 74945 Latitude: -18.9808 Longitude: 225.731 Instrument: VIS Captured: 2018-11-06 05:00Please 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.

A thin layer of water frost is visible on the ground around NASA's Phoenix Mars Lander in this image taken August 14, 2008. Enhanced details of the polygons, troughs and rocks are seen around the landing site.

A thin layer of water frost is visible on the ground around NASA's Phoenix Mars Lander in this image taken by the Surface Stereo Imager at 6 a.m. on Sol 79 (August 14, 2008), the 79th Martian day after landing. The frost begins to disappear shortly after 6 a.m. as the sun rises on the Phoenix landing site.The sun was about 22 degrees above the horizon when the image was taken, enhancing the detail of the polygons, troughs and rocks around the landing site.This view is looking east southeast with the lander's eastern solar panel visible in the bottom lefthand corner of the image. The rock in the foreground is informally named "Quadlings" and the rock near center is informally called "Winkies."This false color image has been enhanced to show color variations.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 approximate true-color image taken by NASA's Mars Exploration Rover Opportunity shows an unusual, lumpy rock informally named 'Wopmay' on the lower slopes of 'Endurance Crater' on Mars.

Click on the image for 'Wopmay' Rock (QTVR)This approximate true-color image taken by NASA's Mars Exploration Rover Opportunity shows an unusual, lumpy rock informally named "Wopmay" on the lower slopes of "Endurance Crater." The rock was named after the Canadian bush pilot Wilfrid Reid "Wop" May. Like "Escher" and other rocks dotting the bottom of Endurance, scientists believe the lumps in Wopmay may be related to cracking and alteration processes, possibly caused by exposure to water. The area between intersecting sets of cracks eroded in a way that created the lumpy appearance. Rover team members plan to drive Opportunity over to Wopmay for a closer look in coming sols. This image was taken by the rover's panoramic camera on sol 248 (Oct. 4, 2004), using its 750-, 530- and 480-nanometer filters.

Taken by NASA's Imager for Mars Pathfinder (IMP), this image shows the rock dubbed 'Flat Top' at center. Dust has accumulated on the top of Flat Top, but is not present on the sides due to the steep angles of the rock.

Taken by the Imager for Mars Pathfinder (IMP), this image shows the rock dubbed "Flat Top" at center. Dust has accumulated on the top of Flat Top, but is not present on the sides due to the steep angles of the rock. This dust may have been placed by dust storms moving across the Martian surface. Areas of darker and brighter reddish soil are distributed between rocks.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 an operating division of the California Institute of Technology (Caltech). The Imager for Mars Pathfinder (IMP) was developed by the University of Arizona Lunar and Planetary Laboratory under contract to JPL. Peter Smith is the Principal Investigator. 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.

The THEMIS camera contains 5 filters. Data from different filters can be combined in many ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows the sand sheet with surface dune forms on the floor of Matara Crater.

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 the sand sheet with surface dune forms on the floor of Matara Crater in Noachis Terra.Orbit Number: 57868 Latitude: -49.5535 Longitude: 34.766 Instrument: VIS Captured: 2014-12-30 14:00Please 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.

On Aug 9, 2005, NASA's Mars Exploration Rover Opportunity after the rover had ground a hole in the rock called 'Ice Cream' and conducted various scientific experiments, it took this final microscopic image of the hole before driving away.

After Opportunity ground a hole in the rock called "Ice Cream" and conducted various scientific experiments, it took this final microscopic image of the hole before driving away. When the image arrived at Earth, scientist discovered that the hole had been filled with dust. Apparently, a blast of wind had picked up some of the tailings produced by the grinding of the rover's rock abrasion tool and swept them back into the hole. In recent months, both rovers have experienced the effects of wind. The Spirit rover on the other side of Mars has tracked the progress of numerous dust devils moving across the plains.Opportunity took this mosaic of images on martian day, or sol, 549 (Aug. 9, 2005). The area shown is approximately 6 centimeters (2.4 inches) wide. The darker portions in the upper left corner of each quadrangle in the mosaic are shadows cast by the rover's robotic arm.

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 in the middle 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: 89612 Latitude: 0.716663 Longitude: 247.469 Instrument: VIS Captured: 2022-02-25 22:59Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of Hyperboreae Undae, which is located between Escorial Crater and the margin of Chasma Boreale.

Context imageSeveral dunes fields are found near the north polar cap. Today's VIS image shows part of Hyperboreae Undae, which is located between Escorial Crater and the margin of Chasma Boreale.Orbit Number: 63061 Latitude: 78.0712 Longitude: 309.216 Instrument: VIS Captured: 2016-03-02 05:57Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

This self-portrait of NASA's Mars Exploration Rover Spirit taken in Aug 27, 2005 shows its solar panels still gleaming in Martian sunlight and carrying only a thin veneer of dust two years after the rover landed and began exploring the red planet.

This bird's-eye view combines a self-portrait of the spacecraft deck and a panoramic mosaic of the Martian surface as viewed by NASA's Mars Exploration Rover Spirit. The rover's solar panels are still gleaming in the sunlight, having acquired only a thin veneer of dust two years after the rover landed and commenced exploring the red planet. Spirit captured this 360-degree panorama on the summit of "Husband Hill" inside Mars' Gusev Crater. During the period from Spirit's Martian days, or sols, 583 to 586 (Aug. 24 to 27, 2005), the rover's panoramic camera acquired the hundreds of individual frames for this largest panorama ever photographed by Spirit.This image is an approximately true-color rendering using the camera's 750-nanometer, 530-nanometer and 480-nanometer filters for the Martian surface, and the 600-nanometer, 530-nanometer, and 480-nanometer filters for the rover deck. This polar projection is a compromise between a cylindrical projection ( http://marsrovers.jpl.nasa.gov/gallery/press/spirit/20051205a.html; https://photojournal.jpl.nasa.gov/catalog/PIA03610), which provides the best view of the terrain, and a vertical projection, which provides the best view of the deck but distorts the terrain far from the rover. The view is presented with geometric seam correction.

NASA's Mars Global Surveyor shows a pair of gully channels that emerge, fully-born at nearly their full width, from beneath small overhangs on the north wall of Dao Vallis on Mars.

Figure A Annotated ImageFigure B Annotated Image No AnnotationFigure C Annotated Image No AnnotationSince their discovery early during the Mars Global Surveyor's Mars Orbiter Camera investigation, as first reported in June 2000, Martian gullies have presented a puzzle for the Mars science community: what fluid was responsible for the erosion that created the channels, and where did it come from? The gullies seem to be quite young in a geologic sense (millions of years or less), yet modern and geologically-recent Mars is an extremely dry place, where water ice sublimates directly to gas when the temperature is warm enough. Since June 2000, many hypotheses have been discussed at scientific meetings, in the scientific journals and elsewhere. The original June 2000 hypothesis held that the fluid was liquid water (either pure, salty, acidic, etc.) that came to the surface where slopes intersected conduits of groundwater. Such slopes include crater walls, valley walls, hills, massifs and crater central peaks. Later investigators explored the possibility that rather than liquid groundwater, the source was ground ice, which, under some climate conditions, melted to produce liquid runoff. Still others noted that thick mantles covered a fraction of the gully-bearing slopes, suggesting that the mantles were ancient, dust-covered snow or ice packs that might melt at the base to make liquid water runoff. Water was not the only fluid considered by various colleagues; carbon dioxide can be fluid at some pressures and temperatures. Fluid carbon dioxide was also proposed as a candidate fluidizing agent. Even dry mass movement, or land sliding, of unconsolidated granular material can exhibit some fluid-like behavior. Such mass movements were considered as an explanation for the gullies. The presence of channels primarily formed by erosion but also displaying features representing along-channel deposition, such as levees and meanders, and terminal depositional aprons consisting of dozens to hundreds of individual flow lobes, contributed to the general acceptance of the hypothesis that gullies involved the action of liquid water. Throughout the Mars Global Surveyor mission, the Mars Orbiter Camera team continued to image gullies at every opportunity, looking for new gullies, taking higher resolution images of previously identified gullies, and monitoring the gullies for changes that might occur. Among the results of this extensive survey are numerous examples of gullies that have geological relations to other things in their vicinity. This provides support for the hypothesis that the fluid responsible for the gullies came from beneath the ground, either as groundwater or melting of ice in the Martian subsurface. Three of the best examples are presented here. Figure A: The first picture shows a pair of gully channels that emerge, fully-born at nearly their full width, from beneath small overhangs on the north wall of Dao Vallis. These overhangs are probably created by the presence of a hard-rock layer. Liquid, probably water, percolated through permeable layers just beneath these harder, more resistant rock layers. The arrow points to the place where one of the two neighboring channels emerges. This is a sub-frame of an image acquired on Jan. 10, 2006, located near 34.2 degrees south latitude, 268.1 degrees west longitude. The 150-meter scale bar is about 164 yards wide. Figure B: The second picture shows a gully that formed on the wall of a crater that intersected a mare-type ridge. The term, mare, is from the dark volcanic plains of Earth's moon, for example Mare Tranquilitatis was the plain on which the Apollo 11 crew landed in 1969. The lunar maria (maria is the plural form of mare), when viewed from above, have many "wrinkle" ridges. These ridges are the surface expression of thrust faults. The mare-type ridge in the picture shown here is thus the product of faulting, as rocks on the west (left) side of the image were thrust toward the east (right). Finding a gully associated with a fault is excellent evidence for the groundwater hypothesis, because ground water percolates through cracks and pores in the ground. On Earth, springs (where groundwater comes to the surface) are often found along fault lines. What is most important about this particular Martian gully is that it occurs equatorward of 30 degrees south, which is extremely unusual. The only gully in this crater is the one associated with the fault. It is essentially the site of a spring, now dried up perhaps. This picture is a sub-frame of an image located near 29.1 degrees south latitude, 207.5 degrees west longitude, acquired on Jan. 17, 2005. Figure C: The third picture shows a small crater on the rim of a larger crater. Only a small portion of the wall of this larger crater is captured in the image. Immediately beneath the small crater occurs a group of gullies. The presence of these gullies also supports the groundwater hypothesis because impacting meteors will fracture the rocks into which they form a crater. In this case, there would be an initial set of subsurface fractures caused by the large impact that created the original, large crater. Then, when the smaller crater formed, it would have created additional fractures in its vicinity. These extra fractures would then have provided pathways, or conduits, through which ground water would come to the surface on the wall of the larger crater, thus creating the gullies observed. One might speculate that the group of gullies was formed by the impact that made the small crater, because of the heat and fracturing of rock during the impact process. However, the gullies are much younger than the small crater; the ejecta from the small crater has been largely eroded away or buried, and the crater partially filled, while the gullies appear sharp, crisp and fresh. This is a portion of an image located near 33.9 degrees south latitude, 160 degrees west longitude, acquired on March 31, 2006. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by NASA's Jet Propulsion Laboratory, Pasadena, Calif., a division of the California Institute of Technology, also in Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera.For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html.

This image acquired on January 22, 2022 by NASA's Mars Reconnaissance Orbiter shows pristine-looking gullies in equatorial Valles Marineris.

Map Projected Browse ImageClick on image for larger versionAlthough actively-forming gullies are common in the middle latitudes of Mars, there are also pristine-looking gullies in equatorial regions.In this scene, the gullies have very sharp channels and different colors where the gullies have eroded and deposited material. Over time, the topography becomes smoothed over and the color variations disappear, unless there is recent activity.Changes have not been visible here from before-and-after images, and maybe such differences are apparent compared to older images, but nobody has done a careful comparison. What may be needed to see subtle changes is a new image that matches the lighting conditions of an older one. Equatorial gully activity is probably much less common — perhaps there is major downslope avalanching every few centuries — so we need to be lucky to see changes.MRO has now been imaging Mars for over 16 years, and the chance of seeing rare activity increases as the time interval widens between repeat images.The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. (The original image scale is 26.5 centimeters [10.4 inches] per pixel [with 1 x 1 binning] to 53.1 centimeters [20.9 inches] per pixel [with 2 x 2 binning]) 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 Exploration Rover Opportunity shows the rocky path lying due east of the rover. Boulders as large as 1.6 feet dot the landscape here near Bonneville Crater. The east hills, over 1.3 miles away, can be seen to the far right.

This image taken by the Mars Exploration Rover Spirit's navigation camera shows the rocky path lying due east of the rover. Boulders as large as half a meter (1.6 feet) dot the landscape here near Bonneville Crater. The east hills, over two kilometers away (1.3 miles), can be seen to the far right. Spirit will most likely drive toward the rim of Bonneville crater along a safer route to the north of this area.

This image from NASA's Mars Odyssey shows an unnamed crater in Acidalia Planitia.

Context imageToday's false color image shows an unnamed crater in Acidalia Planitia. The dark blue feature on the crater floor is a mound of sand. The sand is tall enough to cast a shadow, with the sun is coming from the left (west). The texture on the surface of the sand are dune features created by wind action.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: 63180 Latitude: 61.4065 Longitude: 311.579 Instrument: VIS Captured: 2016-03-12 01:24Please 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 where NASA's Curiosity rover aimed two different instruments to study a rock known as 'Jake Matijevic.' The red dots are where ChemCam zapped the rock with its laser.

Unannotated versionClick on the image for full-res version This image shows where NASA's Curiosity rover aimed two different instruments to study a rock known as "Jake Matijevic." The red dots are where the Chemistry and Camera (ChemCam) instrument zapped it with its laser on Sept. 21, 2012, and Sept. 24, 2012, which were the 45th and 48th sol, or Martian day of operations. The circular black and white images were taken by ChemCam to look for the pits produced by the laser. The purple circles indicate where the Alpha Particle X-ray Spectrometer trained its view. This image was obtained by Curiosity's Mast Camera on Sept. 21, 2012 PDT (Sept. 22 UTC), or sol 46. Scientists white-balanced the color in this view to increase the inherent differences visible within the rock. 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.

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 the northern tip of Baetis Mensa.

Context imageThe THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows the northern tip of Baetis Mensa. In false color images dark blue is often basaltic sands. In this image it is possible to trace the sands from the erosion of Beatis Mensa moving down the canyon gullies to the floor of Ophir Chasma.Orbit Number: 42247 Latitude: -4.17728 Longitude: 287.975 Instrument: VIS Captured: 2011-06-23 21:11Please 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 released on August 26, 2004 from NASA's 2001 Mars Odyssey shows Gordii Dorsa, one of the largest ridges on Mars. Dorsa mean ridge; Gordii means Gordian knot.

Released August 26, 2004The THEMIS Image of the Day will be exploring the nomenclature of Mars for the next three weeks.Gordii DorsaDorsa: ridgeGordii: the Gordian knot, this complex knot was tied to King Gordius of Phrygia's chariot. An oracle said that whomever untied the knot would be the next king of Asia. Alexander the Great cut open the knot with his sword.Gordii Dorsa is one of the largest ridges on Mars. The outlined area shows the margins of the dorsa on this daytime IR image. The area between the arrows is the dorsa, which rises above the surrounding plains. Gordii Dorsa is an area of intense study, as we are not yet sure how this ridge was formed. The surface of this ridge is undergoing erosion by the wind, which indicates that the material that makes up the ridge is not solid rock.Nomenclature Fact of the Day: Some mythological accounts say that Zeus was hidden in a cave on Mt. Ida after his birth, so craters on the asteroid Ida are named for caverns and grottos all over the world.Image information: IR instrument. Latitude 1.3, Longitude 214.6 East (145.4 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.

NASA's Mars Global Surveyor shows house-sized boulders and layered volcanic rock exposed in a pit on the north flank of the giant Tharsis volcano, Ascraeus Mons on Mars. The pit most likely formed by collapse.

29 December 2005This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows house-sized boulders and layered volcanic rock exposed in a pit on the north flank of the giant Tharsis volcano, Ascraeus Mons. The pit most likely formed by collapse. Dust mantles much of the surrounding terrain and the pit floor.Location near: 12.9°N, 101.6°W Image width: ~3 km (~1.9 mi) Illumination from: lower left Season: Southern Winter

On Dec. 5, 2006, NASA's Mars Exploration Rover Opportunity examined a section of the scalloped rim called Bottomless Bay in Victoria Crater on Mars. The upper portion of the crater wall contains a jumble of material.

As part of its investigation of "Victoria Crater," NASA's Mars Exploration Rover Opportunity examined a section of the scalloped rim called "Bottomless Bay" (or "Bahia sin Fondo"). This view shows the northeastern side of Bottomless Bay as seen from the southwest. The exposures combined into this mosaic were taken by the rover's panoramic camera through a 750-nanometer filter during the 1,019th Martian day, or sol, of Opportunity's Mars-surface mission (Dec. 5, 2006). Contrast has been altered to improve the visibility of details in shadowed areas.

These small spherules on the Martian surface are near Fram Crater, visited by NASA's Mars Exploration Rover Opportunity during April 2004. The area shown is 1.2 inches (3 centimeters) across.

The small spherules on the Martian surface in this close-up image are near Fram Crater, visited by NASA's Mars Exploration Rover Opportunity during April 2004. The area shown is 1.2 inches (3 centimeters) across. The view comes from the microscopic imager on Opportunity's robotic arm, with color information added from the rover's panoramic camera.These are examples of the mineral concretions nicknamed "blueberries." Opportunity's investigation of the hematite-rich concretions during the rover's three-month prime mission in early 2004 provided evidence of a watery ancient environment. This image was taken during the 84th Martian day, or sol, of the rover's work on Mars (April 19, 2004). The location is beside Fram Crater, which Opportunity passed on its way from Eagle Crater, where it landed, toward Endurance Crater, where it spent most of the rest of 2004. A context image is online at PIA05822.JPL manages the Mars Exploration Rover Project for NASA's Science Mission Directorate in Washington. For more information about Spirit and Opportunity, visit http://marsrovers.jpl.nasa.gov.

Sojourner's left rear wheel is perched on the rock 'Wedge' in this image, taken on Sol 47 by the Imager for NASA's Mars Pathfinder (IMP).

Sojourner's left rear wheel is perched on the rock "Wedge" in this image, taken on Sol 47 by the Imager for Mars Pathfinder (IMP). The rover's Alpha Proton X-ray Spectrometer (APXS) is the cylindrical object extending from the back of the rover.This image and PIA01556 (left eye) make up a stereo pair.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 an operating division of the California Institute of Technology (Caltech). Photojournal note: Sojourner spent 83 days of a planned seven-day mission exploring the Martian terrain, acquiring images, and taking chemical, atmospheric and other measurements. The final data transmission received from Pathfinder was at 10:23 UTC on September 27, 1997. Although mission managers tried to restore full communications during the following five months, the successful mission was terminated on March 10, 1998.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows the southern rim of Lockyer Crater and part of its ejecta blanket.

Context imageToday's VIS image shows the southern rim of Lockyer Crater and part of its ejecta blanket.Orbit Number: 45209 Latitude: 27.0419 Longitude: 160.366 Instrument: VIS Captured: 2012-02-22 18:29Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

Spirit's Route in Black and White

The Mars Orbital Camera on NASA's Mars Global Surveyor spacecraft took this image of the topography traversed by NASA's Mars Exploration Rover Spirit in months prior to the rover's 318th martian day (Dec. 4, 2004). The yellow line traces the rover's path up to and across the "West Spur" of the "Columbia Hills."

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

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 Aureum Chaos.Orbit Number: 9913 Latitude: -4.41938 Longitude: 333.031 Instrument: VIS Captured: 2004-03-09 13:43Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

This image from NASA's 2001 Mars Odyssey released on March 19, 2004 shows what a typical crater on Mars would look like.

Released 19 March 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 February 15, 2003 during the northern summer season. This image shows what a typical crater would look like.Image information: VIS instrument. Latitude 54.7, Longitude 190.7 East (169.3 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.

There is a large deposit of material on the floor of Nicholson Crater, as seen in this image from NASA's 2001 Mars Odyssey spacecraft. This pile of material appears to be undergoing erosion by the wind.

Context imageThere is a large deposit of material on the floor of Nicholson Crater, as seen in this image. This pile of material appears to be undergoing erosion by the wind.Orbit Number: 44958 Latitude: 0.112352 Longitude: 195.448 Instrument: VIS Captured: 2012-02-02 02:46Please 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.