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https://photojournal.jpl.nasa.gov/catalog/PIA06696	/content/Nasa_Mars_Images/PIA06696_modest.jpg	NASA's Mars Global Surveyor shows mesa tops and depressions formed in layered carbon dioxide ice in Mars' south polar residual cap.	19 July 2004This full-resolution (1.5 meters, 5 feet, per pixel) Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows mesa tops and depressions formed in layered carbon dioxide ice in the south polar residual cap. The image is located near 87.0°S, 341.9°W, and covers an area about 1.5 km (0.9 mi) wide. Sunlight illuminates the scene from the upper left.
https://photojournal.jpl.nasa.gov/catalog/PIA25358	/content/Nasa_Mars_Images/PIA25358_modest.jpg	This image acquired on May 11, 2022 by NASA's Mars Reconnaissance Orbiter shows a 280-kilometer diameter crater center that has experienced a long history of water activity.	Map Projected Browse ImageClick on image for larger versionThis 280-kilometer diameter crater center has experienced a long history of water activity. Within the crater is a heavily faulted and fractured terrain called Aram Chaos that consists of darker volcanic rocks that were disrupted as a result of water and/or magma withdrawal in the subsurface.Above this chaotic terrain are brighter materials made up of different kinds of sulfates that formed when water filled the crater. CRISM data collected along with HiRISE images indicate that the sulfates consist of monohydrated, polyhydrated, and ferric hydroxysulfate, with each composition representing a different geochemical environment within the waters that once resided within Aram Chaos. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. (The original image scale is 28.6 centimeters [11.3 inches] per pixel [with 1 x 1 binning] to 57.1 centimeters [22.5 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.
https://photojournal.jpl.nasa.gov/catalog/PIA18768	/content/Nasa_Mars_Images/PIA18768_modest.jpg	The linear depressions (termed graben) in this image captured by NASA's 2001 Mars Odyssey spacecraft are part of Memnonia Fossae.	Context imageThe linear depressions (termed graben) in today's VIS image are part of Memnonia Fossae.Orbit Number: 56489 Latitude: -20.1391 Longitude: 205.186 Instrument: VIS Captured: 2014-09-08 01:16 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.
https://photojournal.jpl.nasa.gov/catalog/PIA22183	/content/Nasa_Mars_Images/PIA22183_modest.jpg	Ladon Basin was a large impact structure that was filled in by the deposits from Ladon Valles, a major ancient river on Mars as seen in this image from NASA's Mars Reconnaissance Orbiter (MRO).	Map Projected Browse ImageClick on the image for larger versionLadon Basin was a large impact structure that was filled in by the deposits from Ladon Valles, a major ancient river on Mars as seen in this image from NASA's Mars Reconnaissance Orbiter (MRO).These wet sediments were altered into minerals such as various clay minerals. Clays imply chemistry that may have been favorable for life on ancient Mars, if anything lived there, so this could be a good spot for future exploration by rovers and perhaps return of samples to Earth.The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 52.1 centimeters (20.5 inches) per pixel (with 2 x 2 binning); objects on the order of 156 centimeters (61.4 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.
https://photojournal.jpl.nasa.gov/catalog/PIA03917	/content/Nasa_Mars_Images/PIA03917_modest.jpg	NASA's Mars Global Surveyor shows a dust devil that seen climbing the wall of a crater at 4.1°S, 9.5°W on May 21, 2002. This crater is in western Terra Meridiani on Mars.	MGS MOC Release No. MOC2-318, 8 August 2002One of the key elements of the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) Extended Mission is to look for and monitor changes taking place on the planet over the course of a second--and, eventually, a third--martian year. MGS is now well into its second Mars year, which will draw to a close in December 2002. Among the changes the MOC has observed are streaks believed to be caused by the passage of dust devils. Thousands of MOC images show these streaks, dozens show that they change over time, but far fewer images have actually captured a dust devil in the act of creating a streak. At the center right of this image (above left) is a dust devil that, on May 21, 2002, was seen climbing the wall of a crater at 4.1°S, 9.5°W. This crater (above right) is in western Terra Meridiani. The dust devil was moving toward the northeast (upper right), leaving behind a dark trail where a thin coating of surficial dust was removed or disrupted as the dust devil advanced. Dust devils most commonly form after noon on days when the martian air is still (that is, when there isn't even a faint breeze). On such days, the ground is better able to heat up the air immediately above the surface. As the warmed near-surface air begins to rise, it also begins to spin, creating a vortex. The spinning column then moves across the surface and picks up loose dust (if any is present). The dust makes the vortex visible and gives it a tornado-like appearance. The dust devil in this image has a very short, dark shadow cast to the right of the bright column; this shadow is short because the sun was nearly overhead.
https://photojournal.jpl.nasa.gov/catalog/PIA11790	/content/Nasa_Mars_Images/PIA11790_modest.jpg	This polar projection image from NASA's Mars Exploration Rover Opportunity shows tracks from the drive extend northward across dark-toned sand ripples and light-toned patches of exposed bedrock in the Meridiani Planum region of Mars.	NASA's Mars Exploration Rover Opportunity used its navigation camera to take the images combined into this full-circle view of the rover's surroundings just after driving 104 meters (341 feet) on the 1,770th Martian day, or sol, of Opportunity's surface mission (January 15, 2009). This view is presented as a polar projection with geometric seam correction. North is at the top.Tracks from the drive extend northward across dark-toned sand ripples and light-toned patches of exposed bedrock in the Meridiani Planum region of Mars. For scale, the distance between the parallel wheel tracks is about 1 meter (about 40 inches).Prior to the Sol 1770 drive, Opportunity had driven less than a meter since Sol 1713 (November 17, 2008), while it used the tools on its robotic arm first to examine a meteorite called "Santorini" during weeks of restricted communication while the sun was nearly in line between Mars and Earth, then to examine bedrock and soil targets near Santorini.The rover's position after the Sol 1770 drive was about 1.1 kilometer (two-thirds of a mile) south southwest of Victoria Crater. Cumulative odometry was 13.72 kilometers (8.53 miles) since landing in January 2004, including 1.94 kilometers (1.21 miles) since climbing out of Victoria Crater on the west side of the crater on Sol 1634 (August 28, 2008).
https://photojournal.jpl.nasa.gov/catalog/PIA05639	/content/Nasa_Mars_Images/PIA05639_modest.jpg	This map shows NASA's Mars Exploration Rover Spirit's past and future routes across the Gusev Crater floor. The solid red line shows where the rover has traveled so far, from lander to the rim of the large crater dubbed 'Bonneville.'	This map shows the Mars Exploration Rover Spirit's past and future routes across the Gusev Crater floor. The solid red line shows where the rover has traveled so far, from lander to the rim of the large crater dubbed "Bonneville." The dotted red line indicates proposed future paths to the Columbia Hills. Rover team members have not yet decided which direction Spirit will travel across Bonneville's ejecta (the blanket of material expelled from it during formation) and toward the hills, as illustrated by the two diverging dotted lines. Along the way, Spirit will stop to investigate interesting targets, including craters and plain deposits. The journey to the hills is estimated to about two months, or 60 sols. The underlying image in this map was taken by the camera on NASA's Mars Global Surveyor orbiter.
https://photojournal.jpl.nasa.gov/catalog/PIA17967	/content/Nasa_Mars_Images/PIA17967_modest.jpg	This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of the huge dune field located at the north polar cap. As spring continues to deepen, the dunes are becoming darker and darker as they lose their winter frost cover.	Context imageThis VIS image shows a portion of the huge dune field located at the north polar cap. As spring continues to deepen, the dunes are becoming darker and darker as they lose their winter frost cover.Orbit Number: 53424 Latitude: 81.615 Longitude: 208.313 Instrument: VIS Captured: 2013-12-29 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.
https://photojournal.jpl.nasa.gov/catalog/PIA04998	/content/Nasa_Mars_Images/PIA04998_modest.jpg	The smooth surfaces of angular and rounded rocks seen in this image of the martian terrain may be the result of wind-polishing debris. The picture was taken by the panoramic camera onboard NASA's Mars Exploration Rover Spirit.	The smooth surfaces of angular and rounded rocks seen in this image of the martian terrain may be the result of wind-polishing debris. The picture was taken by the panoramic camera on the Mars Exploration Rover Spirit.
https://photojournal.jpl.nasa.gov/catalog/PIA07185	/content/Nasa_Mars_Images/PIA07185_modest.jpg	This image from NASA's Mars Odyssey shows a portion of the flank of Olympus Mons on Mars. Lava flows are easily identifiable in this image.	This is a daytime IR image of the same location as yesterday's nighttime IR image (PIA07182). Lava flows are much easier to identify in this image. The warming of the surface by the sun has increased the signal emitted to the camera.Image information: IR instrument. Latitude 14, Longitude 229.8 East (130.2 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.
https://photojournal.jpl.nasa.gov/catalog/PIA04822	/content/Nasa_Mars_Images/PIA04822_modest.jpg	Mars Exploration Rover (MER) spacecraft. This image shows the aeroshell, which includes the backshell as well as the heatshield.	December 5, 2002Mars Exploration Rover (MER) spacecraft. This image shows the aeroshell, which includes the backshell as well as the heatshield.
https://photojournal.jpl.nasa.gov/catalog/PIA01431	/content/Nasa_Mars_Images/PIA01431_modest.jpg	This image from NASA's Mars Global Surveyor acquired on April 28, 1998, shows some of the lava flows near the summit of Ascraeus Mons.	Ascraeus Mons Volcano: Like Earth, Mars has many volcanoes and volcanic features. This high-resolution view shows some of the lava flows near the summit of Ascraeus Mons, one of the three giant shield volcanoes known as the "Tharsis Montes." Volcanoes form when magma (molten rock) erupts out onto the surface of a planet. Based on Viking-era observations, Ascraeus Mons is considered to be one of the tallest volcanoes on Mars... its summit is more than 11 km (6.8 miles) above the surrounding plain. The summit is more than 23 km (14 miles) higher in elevation than the place where Mars Pathfinder landed in July 1997.Description of MOC Image: This picture shows an area that is about 20 km (12 miles) higher in elevation than the Mars Pathfinder landing site. The picture shows three main features: (1) a crater at the center-right, (2) a sinuous, discontinuous channel across the upper half, and (3) a rough and pitted, elevated surface across the lower half of the image.(1) Crater at center right. Distinguishing meteor craters from volcanic craters can sometimes be a challenge on Mars. This particular crater was most likely formed by meteor impact because it has a raised rim and a faint radial ejecta pattern around the outside of it. This crater is 600 m (2000 feet) across, about 3/4 the size of the famous "Meteor Crater" near Winslow, Arizona.(2) Sinuous channel. The type of discontinuous channel running across the upper half of the image is sometimes referred to as a "sinuous rille." These are common on the volcanic plains of the Moon and among volcanoes and volcanic plains on Earth. Such a channel was once a lava tube. It is running down the middle of an old lava flow. The "tube" looks like a "channel" because its roof has collapsed. The discontinuous nature of this channel is the result of the collapse, or "cave-in" of what was once the roof of the lava tube. It is common for certain types of relatively fluid lavas to form lava tubes. As it is being emplaced, the outer margins of the lava flow cool and harden, but the interior remains hot and continues to flow down-hill. Eventually, the eruption stops and the lava inside the tube cools, contracts, and hardens, leaving behind a tube (basically, a long narrow cave).(3) Rough elevated surface. The rough, pitted, and elevated surface across the bottom half of the image is a lava flow. The margins of this feature are somewhat lobate in form, and the entire feature is elevated above its surroundings, indicating that it was the last lava flow to pour through this region.Putting it All Together: Aa and Pahoehoe Lava Flows: Shield volcanoes such as Ascraeus Mons form from relatively fluid lavas. Shield volcanoes on Earth include the well-known Islands of Hawai'i. The kind of lava that is fluid enough to make shield volcanoes is called basalt. This is an iron- and magnesium-rich silicate lava that, when cooled, is usually black or very dark brown.Basalt lava flows come in two main varieties: Aa and Pahoehoe. These are Hawai'ian names. "Aa" (pronounced "ah-ah") lava flows have very rough, jumbly surfaces, and they usually lack lava tubes. "Aa" lava flow surfaces are very rough to walk on-- thus the term "aa" probably refers to the sound a person might make when walking on a cooled/solidified aa flow in bare feet!"Pahoehoe" (pronounced "pa-hoy-hoy") is a term that means "ropey." The surfaces of pahoehoe lava flows are generally very smooth and billowy. Sometimes they have a ropy texture like melted taffy or caramel. Pahoehoe flows very commonly contain lava tubes.The rough-surfaced flow across the lower half of the MOC image is interpreted to be an "aa" lava flow, and the smoother surface with a sinuous channel running down its center is interpreted to be a "pahoehoe" lava flow. Both would indicate that the lavas on Ascraeus Mons, at least at this location, are probably composed of basalt.More Picture Information: This MOC picture is a subframe of image #26705, centered approximately at 11.5°N latitude, 103.5°W longitude. It was taken on April 28, 1998, at 4:23 AM Universal Time, on Mars Global Surveyor's 267th orbit around Mars. Orbit 267 was the second-to-last orbit on which observations were obtained before Mars and the spacecraft passed behind the Sun for several weeks known as "Solar Conjunction."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.
https://photojournal.jpl.nasa.gov/catalog/PIA02011	/content/Nasa_Mars_Images/PIA02011_modest.jpg	NASA's Mars Global Surveyor shows Warrego Valles, a system of discontinuous valleys located in the martian southern hemisphere south of Valles Marineris between Aonia Terra and Icaria Planum.	After several weeks of hiatus owing to problems with Mars Global Surveyor's High Gain Antenna (e.g., see JPL Release (April 16, 1999) the Mars Orbiter Camera resumed operations during the final days of April 1999. Shown here is one of the first images returned after MOC began taking pictures again.Warrego Valles is a system of discontinuous valleys located in the martian southern hemisphere south of Valles Marineris between Aonia Terra and Icaria Planum. This picture shows one of the small valleys in this system. The planet's surface both inside and outside the valley appears to be extremely rough. A person would find this terrain challenging to walk around in. The picture is illuminated from the upper left and covers an area 3 kilometers (1.9 miles) across.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.
https://photojournal.jpl.nasa.gov/catalog/PIA00935	/content/Nasa_Mars_Images/PIA00935_modest.jpg	This image of Mars from NASA's Mars Global Surveyor Orbiter shows an area centered near the Pathfinder landing site. The dark area north of the center of the image along the sunrise terminator is Acidalia Planitia.	This image of Mars shows an area centered near the Pathfinder landing site. The dark area north of the center of the image along the sunrise terminator is Acidalia Planitia--the Pathfinder landing site is about a third of the way down from this dark area across the light Chryse plains. The bright area near the edge of the planet is Arabia. The lower 40% of the image contains the Xanthe, Margaritifer, and Meridiani highlands, heavily-cratered, ancient areas of the most intense erosion seen on Mars. These will be among the more important targets of the MOC when it begins detailed studies in March 1998.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 operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO.
https://photojournal.jpl.nasa.gov/catalog/PIA22536	/content/Nasa_Mars_Images/PIA22536_modest.jpg	This image from NASA's Mars Reconnaissance Orbiter shows Ganges Chasma in the northeast portion of Valles Marineris. Scattered hills on the canyon floor may be remnants of chaos terrain that formed from collapse of the canyon.	Map Projected Browse ImageClick on image for larger versionNASA's Mars Reconnaissance Orbiter (MRO) observed this image of Ganges Chasma in the northeast portion of Valles Marineris, and opens into outflow channels that flowed to the north.Scattered hills on the canyon floor may be remnants of chaos terrain that formed from collapse of the canyon. Some of the bedrock has diverse colors as we see in the enhanced-color (false color) cutout. The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 53.5 centimeters (21.1 inches) per pixel (with 2 x 2 binning); objects on the order of 160 centimeters (62.0 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.
https://photojournal.jpl.nasa.gov/catalog/PIA12980	/content/Nasa_Mars_Images/PIA12980_modest.jpg	NASA's Mars Exploration Rover used its panoramic camera to record this view of the rim of a crater about 65 kilometers (40 miles) in the distance, on the southwestern horizon. This crater, Bopolu, is about 19 kilometers (12 miles) in diameter.	NASA's Mars Exploration Rover used its panoramic camera to record this view of the rim of a crater about 65 kilometers (40 miles) in the distance, on the southwestern horizon. This crater, Bopolu, is about 19 kilometers (12 miles) in diameter. The image was taken during the 2,179th Martian day, or sol, of Opportunity's mission on Mars (March 11, 2010), two days after the rover drove southward away from Concepcion crater, site of several weeks of investigation.Opportunity's long-term destination is Endeavour Crater, to the southeast and closer than Bopolu. The intended route heads south before turning east in order to bypass potentially hazardous sand ripples to the east, larger than the ripples in the foreground of this image. This approximately true-color view combines three exposures taken through filters admitting wavelengths of 750 nanometers, 530 nanometers and 480 nanometers.
https://photojournal.jpl.nasa.gov/catalog/PIA03661	/content/Nasa_Mars_Images/PIA03661_modest.jpg	This image from NASA's Mars Global Surveyor shows a group of tapered ridges, known as yardangs, which formed by wind erosion of a relatively easily-eroded material, most likely sedimentary rock or volcanic ash deposits.	12 January 2006This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a group of tapered ridges, known as yardangs, which formed by wind erosion of a relatively easily-eroded material, most likely sedimentary rock or volcanic ash deposits containing some fraction of sand-sized grains.Location near: 6.1°S, 210.8°W Image width: ~2 km (~1.2 mi) Illumination from: lower left Season: Southern Summer
https://photojournal.jpl.nasa.gov/catalog/PIA02332	/content/Nasa_Mars_Images/PIA02332_modest.jpg	NASA's Mars Global Surveyor shows the mapping of Mars' polar cap recession, surface and atmospheric temperatures, and albedo features found within the seasonal cap itself.	The early part of the Mars Global Surveyor mission provided good TES coverage of the Mars south polar region. These data allow mapping of the polar cap recession, surface and atmospheric temperatures, and albedo features found within the seasonal cap itself (Kieffer et al., 1998, Titus et al., 1998).During the period observed, the seasonal south polar cap retreated continuously and asymmetrically around the geographic pole, much the way Viking observed in 1976-1977 (Kieffer et al., 1977). One of the most dominant albedo features on the seasonal cap is a region that appears almost as dark as bare ground, but yet remains cold. We refer to this region, generally located between latitudes 85°S and 75°S and longitudes 150°W and 310°W, as the Cryptic region.A re-examination of the IRTM data revealed that the Cryptic region was not unique to the TES era, but also was quite apparent during the Viking era. Interesting enough, Antoniadi (Blunck, 1977) observed dark regions forming on the season cap that loosely correlates to the Cryptic region: Depressio Magna (1909) and Depressio Parva (1929). These depressios were located at 270° W, 78°S and 166° W, 76°S, respectively.Analysis of both the TES and IRTM data indicate that the Cryptic region is unique in its thermophysical properties relative to the rest of the cap. The region is a repeatable event that occupies the same general area from year to year. It is darker and slightly warmer than the rest of the south polar cap. Even though the Cryptic region is slightly warmer, it must still be CO2 buffered since it remains "cold" for several days.Spectral analysis of the TES longward of the 15 micron atmospheric band shows that the Cryptic region shows less spectral than the rest of the polar cap. This suggests that the region may be composed of "ice," as opposed to snow or frost (Hansen, 1998). Further spectral analysis on going.This image is a map of TES data, showing Lambert albedo of the south polar cap. The image is a composite from the first rolls of orbit 43 (Ls =219.2°, Nov 17, 1997) and orbit 45 (Ls=220.8°, Nov 20, 1997). The Cryptic region is the blue area curving along the 80°S latitude line. The region shows up in the thermal image (PIA02333) as only slightly warmer than the rest of the polar cap, but still too cold to be bare ground.
https://photojournal.jpl.nasa.gov/catalog/PIA18391	/content/Nasa_Mars_Images/PIA18391_modest.jpg	This map shows in red the route driven by NASA's Curiosity Mars rover from the 'Bradbury Landing' location where it landed in August 2012 to nearly the completion of its first Martian year. The white line shows the planned route ahead.	This map shows in red the route driven by NASA's Curiosity Mars rover from the "Bradbury Landing" location where it landed in August 2012 (blue star at upper right) to nearly the completion of its first Martian year. The white line shows the planned route ahead.Curiosity departed a waypoint called "The Kimberley" on the 630th Martian day, or sol, of the rover's work on Mars (May 15, 2014) and drove more than three-fourths of a mile (1.2 kilometers) between then and the Sol 663 (June 18, 2014) position marked on the map by the green star at the western end of the red line. The rover will have completed a mission goal of working for a full Martian year on Sol 669 (June 24, 2014). A Martian year is 687 Earth days.A major destination for the mission remains geological layering exposed on the lower slope of Mount Sharp, with "Murray Buttes" chosen as the entry point because of a gap there in a band of dark-toned dune fields edging the base of the mountain. The white line indicates a planned route to Murray Buttes chosen in spring 2014 as the safest path for the rover's wheels. Embedded, sharp rocks on the route driven between the "Cooperstown" and "Kimberley" waypoints marked on the map caused the pace of wear and tear on the wheels to accelerate unexpectedly in late 2013. The white-line route avoids some stretches of similar terrain on a more northerly route previously planned for getting to Murray Buttes.The base image for this map is from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. North is up. The scale bar at lower right represents one kilometer (0.62 mile). For broader-context images of the area, see PIA16064 and PIA16058. At Yellowknife Bay, the Mars Science Laboratory Project that built and operates Curiosity achieved its main science objective of determining whether Mars ever offered environmental conditions favorable for microbial life. Rock-powder samples drilled from two mudstone rocks there and analyzed onboard yielded evidence for an ancient lakebed with mild water, the chemical elements needed for life and a mineral source of energy used by some Earth microbes. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Science Laboratory Project and Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/.
https://photojournal.jpl.nasa.gov/catalog/PIA23976	/content/Nasa_Mars_Images/PIA23976_modest.jpg	This map shows regions in and around Mars' Jezero Crater, the landing site of NASA's Perseverance rover. The green circle represents the rover's landing ellipse, or the area where it will be landing within the crater.	This map shows regions in and around Jezero Crater on Mars, the landing site of NASA's Perseverance rover. The green circle represents the rover's landing ellipse.Jezero held a lake and river delta billions of years ago; scientists want to capture samples of rock in these regions that may contain evidence of ancient microscopic life, which will be returned to Earth by a future mission for extensive study. Each of these regions represents a distinct area that may hold different kinds of evidence. The outermost region, called Midway/Northeast Syrtis, could be considered for exploration after the rover's primary mission.The map was created in a tool called Campaign Analysis Mapping and Planning (CAMP), developed by NASA's Jet Propulsion Laboratory, a division of Caltech in Southern California, which manages the Mars 2020 Perseverance rover mission for NASA's Science Mission Directorate in Washington. Data for the map was provided by the High-Resolution Imaging Science Experiment (HiRISE), one of the cameras aboard NASA's Mars Reconnaissance Orbiter, also managed by JPL. The University of Arizona, in Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., in Boulder, Colorado.
https://photojournal.jpl.nasa.gov/catalog/PIA05622	/content/Nasa_Mars_Images/PIA05622_modest.jpg	A microscopic image shows variability of grain size, medium-sized, well rounded and sorted, within a parallel-stratified portion of the 'Slickrock' area in the martian rock outcrop examined by NASA's Mars Exploration Rover Opportunity.	Figure 1A microscopic image shows variability of grain size within a parallel-stratified portion of the "Slickrock" area in the martian rock outcrop examined by NASA's Opportunity. Opportunity took this picture with its microscopic imager during the rover's 42nd sol on Mars (March 6, 2004), the sol before it took a similar picture PIA05520 at the same location. Most of the grains visible resemble medium-sized sand grains and are well-rounded and well-sorted.The dip from left to right is an artifact of the camera pointing angle. The grains in the rock define the fine layers, or laminae, and the variability in grain size along each lamina is small compared to the variability between laminae. Some of the fine layers have mostly smaller grains; others have mostly larger grains. Red arrows and labels (Figure 1) indicate the sizes of a representative large grain (0.8 millimeter or 0.03 inch) and a representative small grain (0.3 millimeters or 0.01 inch).
https://photojournal.jpl.nasa.gov/catalog/PIA05644	/content/Nasa_Mars_Images/PIA05644_modest.jpg	NASA's Mars Global Surveyor shows gullies and slopes in the walls of a deep pit in the south polar region of Mars.	22 March 2004This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows gullies and slopes in the walls of a deep pit in the south polar region. The full-resolution (1.5 m/pixel; 5 ft./pixel) image is located near 71.1°S, 358.8°W, and covers an area about 3 km (1.9 mi) across. Sunlight illuminates the scene from the lower left.
https://photojournal.jpl.nasa.gov/catalog/PIA25877	/content/Nasa_Mars_Images/PIA25877_modest.jpg	This image from NASA's Mars Odyssey shows the eastern side of Uranius Mons. Uranius Mons is 4.8 kilometers (3 miles) high with shallow slopes.	Context imageToday's VIS image shows the eastern side of Uranius Mons. Uranius Mons is 4.8 kilometers (3 miles) high with shallow slopes. The surrounding volcanic plains are younger than the volcano itself and originated at other volcanic centers in the Tharsis region.Orbit Number: 93779 Latitude: 26.0433 Longitude: 267.938 Instrument: VIS Captured: 2023-02-04 01:46Please 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.
https://photojournal.jpl.nasa.gov/catalog/PIA07416	/content/Nasa_Mars_Images/PIA07416_modest.jpg	This image, part of THEMIS art month, taken by NASA's Mars Odyssey features a portion of Mars' landscape looking like a face staring at the spacecraft.	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!Something is looking at you...but what is it?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.
https://photojournal.jpl.nasa.gov/catalog/PIA21987	/content/Nasa_Mars_Images/PIA21987_modest.jpg	Siton Undae is a large dune field located in the northern plains near Escorial Crater. This image from NASA's 2001 Mars Odyssey spacecraft shows part of a dune field just west of Escorial Crater (just off the top of image).	Context image Siton Undae is a large dune field located in the northern plains near Escorial Crater. Siton Undae is west of the crater and is one of three dune fields near the crater. The nearby north polar cap is dissected by Chasma Boreale, which exposes an ice free surface. This image shows part of dune field just west of Escorial Crater (just off the top of image).The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water and lava, and a variety of other feature, THEMIS has imaged them all. For the next several months the image of the day will focus on the Tharsis volcanoes, the various chasmata of Valles Marineris, and the major dunes fields. We hope you enjoy these images!Orbit Number: 18999 Latitude: 75.5288 Longitude: 299.95 Instrument: VIS Captured: 2006-03-27 17:13Please 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.
https://photojournal.jpl.nasa.gov/catalog/PIA12324	/content/Nasa_Mars_Images/PIA12324_modest.jpg	NASA's 2001 Mars Odyssey infrared image shows a group of dunes in Aonia Terra.	Context imageCredit: NASA/JPL/MOLAContinuing our survey of non-crater dune fields brings us to this group of dunes in Aonia Terra. The daytime IR illustrates the warmth of the dune material compared to the surrounding materials.Image information: IR instrument. Latitude -50.1N, Longitude 293.4E. 121 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.
https://photojournal.jpl.nasa.gov/catalog/PIA20098	/content/Nasa_Mars_Images/PIA20098_modest.jpg	This image from NASA's 2001 Mars Odyssey spacecraft shows a portion of Granicus Valles. This channel system is located west of Elysium Mons and likely was created by both lava and water flow related to the Elysium Mons volcanic complex.	Context imageToday's VIS image shows a portion of Granicus Valles. This channel system is located west of Elysium Mons and likely was created by both lava and water flow related to the Elysium Mons volcanic complex.Orbit Number: 61084 Latitude: 28.5697 Longitude: 129.782 Instrument: VIS Captured: 2015-09-21 10:03Please 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.
https://photojournal.jpl.nasa.gov/catalog/PIA26073	/content/Nasa_Mars_Images/PIA26073_modest.jpg	Made with data recorded by NASA's Perseverance during a July 15, 2023 autonomous drive, this animation shows how the rover used AutoNav to maneuver around the 14-inch (35-centimeter) rock at center-left.	Click here for animationThis animation is a playback of data recorded by NASA's Perseverance Mars rover during an autonomous drive on July 15, 2023, the 854th day, or sol, of the mission. During this drive, the rover identified and navigated around the 14-inch (35-centimeter) rock seen at center-left. The self-driving autonomous navigation system, AutoNav, allows the rover to autonomously re-plan its route around rocks or other obstacles on its way to a pre-established destination. Engineers driving the rover at NASA's Jet Propulsion Laboratory in Southern California use visualization software to plan how the rover moves around on Mars and to evaluate its performance. The lines seen emanating from the front of the rover are 20 feet (6 meters) long and indicate the paths the rover is evaluating for safety in real time, while driving. Lines that turn blue show where the rover identified a "wheel drop" hazard – where a wheel could drop more than 14 inches (35 centimeters). Magenta lines indicate where the rover saw a belly pan clearance issue – where a terrain feature could get too close to the belly pan underneath the rover. The surrounding white terrain is a digital elevation model that the rover creates onboard using navigation camera images. The animation has been sped up compared to real time. A key objective for Perseverance's mission on Mars is astrobiology, including the search for signs of ancient microbial life. The rover will characterize the planet's geology and past climate, pave the way for human exploration of the Red Planet, and be the first mission to collect and cache Martian rock and regolith (broken rock and dust).Subsequent NASA missions, in cooperation with ESA (European Space Agency), would send spacecraft to Mars to collect these sealed samples from the surface and return them to Earth for in-depth analysis.The Mars 2020 Perseverance mission is part of NASA's Moon to Mars exploration approach, which includes Artemis missions to the Moon that will help prepare for human exploration of the Red Planet.JPL, which is managed for NASA by Caltech in Pasadena, California, built and manages operations of the Perseverance rover.
https://photojournal.jpl.nasa.gov/catalog/PIA00197	/content/Nasa_Mars_Images/PIA00197_modest.jpg	NASA's Viking Orbiter 1 spies the north polar residual ice cap, which is cut by spiral-patterned troughs and surrounded by the dark lowland plains of Vastitas Borealis, Mars is located at the top.	Center of the orthographic projection is at latitude 30 degrees N., longitude 150 degrees. The north polar residual ice cap, which is cut by spiral-patterned troughs and surrounded by the dark lowland plains of Vastitas Borealis, is located at the top. The right-central part is dominated by the Tharsis Montes volcanoes. The most prominent of the Tharsis Montes volcanoes is the largest known volcano in the solar system, Olympus Mons. The light-colored lowland plains of Amazonis, Elysium, and Arcadia Planitiae lies north and west of Olympus Mons. The heavily cratered highlands dominate the lower one-third.
https://photojournal.jpl.nasa.gov/catalog/PIA21286	/content/Nasa_Mars_Images/PIA21286_modest.jpg	This image captured by NASA's 2001 Mars Odyssey spacecraft shows several channels in and around unnamed craters in Noachis Terra.	Context image This VIS image shows several channels in and around unnamed craters in Noachis Terra.Orbit Number: 66252 Latitude: -38.0339 Longitude: 40.923 Instrument: VIS Captured: 2016-11-20 01:43Please 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.
https://photojournal.jpl.nasa.gov/catalog/PIA11740	/content/Nasa_Mars_Images/PIA11740_modest.jpg	NASA's Mars Exploration Rover Opportunity to this polar projection 360-degree view of the its surroundings on Oct. 22, 2008 southwest of Victoria Crater on Mars.	NASA's Mars Exploration Rover Opportunity used its navigation camera to take the images combined into this 360-degree view of the rover's surroundings on the 1,687th Martian day, or sol, of its surface mission (Oct. 22, 2008). Opportunity had driven 133 meters (436 feet) that sol, crossing sand ripples up to about 10 centimeters (4 inches) tall. The tracks visible in the foreground are in the east-northeast direction.Opportunity's position on Sol 1687 was about 300 meters southwest of Victoria Crater. The rover was beginning a long trek toward a much larger crater, Endeavour, about 12 kilometers (7 miles) to the southeast.This view is presented as a polar projection with geometric seam correction.
https://photojournal.jpl.nasa.gov/catalog/PIA00813	/content/Nasa_Mars_Images/PIA00813_modest.jpg	Blue-filter image of the 1997 Martian dust storm. Mars Orbiter Camera wide-angle frame from Orbit 50, taken by NASA's Mars Global Surveyor Orbiter.	Blue-filter image of the 1997 Martian dust storm. Mars Orbiter Camera wide-angle frame from Orbit 50.Figure caption from Science Magazine.
https://photojournal.jpl.nasa.gov/catalog/PIA12996	/content/Nasa_Mars_Images/PIA12996_modest.jpg	The terrain in this image from NASA's Mars Reconnaissance Orbiter lies in the Deuteronilus Mensae region along the highland-lowland dichotomy boundary in the northern hemisphere of Mars.	The terrain in this image lies in the Deuteronilus Mensae region along the highland-lowland dichotomy boundary in the northern hemisphere of Mars. The High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter recorded this image on March 9, 2010. The target for this HiRISE observation was a suggestion submitted through the camera team's HiWish public-suggestion program. For more information about how to submit target suggestions, see http://uahirise.org/hiwish/.This region contains many mesas surrounded by lobate debris aprons that are thought to be ice-rich. These aprons have been interpreted as a variety of possible features including rock glaciers, ice-rich mass movements, or debris-covered glacial flows. Recent radar data from the Shallow Radar instrument on the Mars Reconnaissance Orbiter has shown them to be composed of nearly pure ice. This image shows an area at the edge of one of these mesas with a lobate debris apron extending from its base. Both the mesa top and the surface of the debris apron appear covered with ice-rich mantling materials characteristic of the Martian mid-latitudes and thought to have been deposited around 10 million years ago during a period of high obliquity. This image covers a swath of ground about 1 kilometer (about two-thirds of a mile) wide. It is a portion of HiRISE observation ESP_016959_2240, which is centered at 43.62 degrees north latitude, 28.62 degrees east longitude. The season on Mars is northern-hemisphere spring. Other image products from this observation are available at http://hirise.lpl.arizona.edu/ESP_016959_2240.Color images from HiRISE combine information from detectors with three different color filters: red, infrared, and blue-green. Thus they include information from part of the spectrum human eyes cannot see and are not true color as the eye would see. The resulting false color helps to show differences among surface materials. The University of Arizona, Tucson, operates the HiRISE camera, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Reconnaissance Orbiter for the NASA Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, built the spacecraft.
https://photojournal.jpl.nasa.gov/catalog/PIA00420	/content/Nasa_Mars_Images/PIA00420_modest.jpg	Ismenius Lacus region of Mars containing the impact crater Moreux. This scene shows heavily cratered highlands in the south on relatively smooth lowland plains in the north separated by a belt of dissected terrain, as seen by NASA's Viking spacecraft.	Color image of part of the Ismenius Lacus region of Mars (MC-5 quadrangle) containing the impact crater Moreux (right center); north toward top. The scene shows heavily cratered highlands in the south on relatively smooth lowland plains in the north separated by a belt of dissected terrain, containing flat-floored valleys, mesas, and buttes. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 36 degrees N. to 50 degrees N. and from longitude 310 degrees to 340 degrees; Lambert conformal conic projection. The dissected terrain along the highlands/lowlands boundary consists of the flat-floored valleys of Deuteronilus Mensae (on left) and Prontonilus Mensae (on right) and farther north the small, rounded hills of knobby terrain. Flows on the mensae floors contain striae that run parallel to valley walls; where valleys meet, the striae merge, similar to medial moraines on glaciers. Terraces within the valley hills have been interpreted as either layered rocks or wave terraces. The knobby terrain has been interpreted as remnants of the old, densely cratered highland terrain perhaps eroded by mass wasting.
https://photojournal.jpl.nasa.gov/catalog/PIA22041	/content/Nasa_Mars_Images/PIA22041_modest.jpg	This image from NASA's Mars Reconnaissance Orbiter shows a crater is located in Elysium Planitia, Mars, an area dominated by volcanic processes. It is likely that the crater fill material is volcanic in origin.	Map Projected Browse ImageClick on the image for larger versionThis 2.5-kilometer diameter crater observed by NASA's Mars Reconnaissance Orbiter (MRO) has been significantly altered from the usual bowl-shaped appearance we associate with craters. Material has covered significant portions of the ejecta and filled in the crater. This fill material has since been subject to erosion -- like boulders weathering out of the slopes -- and the crater rim is also highly irregular.This crater is located in Elysium Planitia, an area dominated by volcanic processes. It is likely that the crater fill material is volcanic in origin, and possible that the rim was etched by lava, either flowing into the crater or spilling over after the crater filled completely. However, there are also signs of erosion by wind, like the parallel ridges in the rim breaches and between high-standing regions of the crater fill. It is likely that the current appearance of this crater is due to a combination of surface processes.This is a stereo pair with ESP_045319_1830. The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 61.7 centimeters (21 inches) per pixel (with 2 x 2 binning); objects on the order of 185 centimeters (59.8 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.
https://photojournal.jpl.nasa.gov/catalog/PIA18562	/content/Nasa_Mars_Images/PIA18562_modest.jpg	This image from NASA's Mars Reconnaissance Orbiter covers layered sedimentary rocks on the floor of an impact crater north of Eberswalde Crater. There may have been a lake in this crater billions of years ago.	Map Projected Browse ImageClick on the image for larger versionThis image covers layered sedimentary rocks on the floor of an impact crater north of Eberswalde Crater. There may have been a lake in this crater billions of years ago, and the area was once considered a landing spot for the Mars Science Laboratory.There are diverse rock compositions, as we can see in an enhanced-color cutout. This image completes a stereo pair, so be sure to view the stereo anaglyph.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 and Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington.
https://photojournal.jpl.nasa.gov/catalog/PIA00968	/content/Nasa_Mars_Images/PIA00968_modest.jpg	This image shows NASA's Sojourner rover's Alpha Proton X-ray Spectrometer (APXS) deployed against the rock 'Stimpy' on the afternoon of Sol 68 (September 11, 1997).	This image shows the Sojourner rover's Alpha Proton X-ray Spectrometer (APXS) deployed against the rock "Stimpy" on the afternoon of Sol 68 (September 11). The two rocks behind the rover were previously analyzed by the APXS.This image and PIA01563 (right 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 a 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.
https://photojournal.jpl.nasa.gov/catalog/PIA05914	/content/Nasa_Mars_Images/PIA05914_modest.jpg	NASA's Mars Global Surveyor shows	7 May 2004The dark streaks, just left of center, on the steep slope in this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image were formed by a relatively recent rock slide. The streak closest to the center of the image resolves into a series of small depressions, indicating the path of a large, rolling boulder. The rock slide is inferred to have been recent (i.e., within the past several Mars years) because it is so much darker than its surroundings--there has not been sufficient time for the streak surfaces to become mantled by dust. The other talus accumulations on this slope are most likely lighter in tone because they are older and coated with dust. These features are located in Ophir Chasma, part of the Valles Marineris trough system, near 4.2°S, 74.0°W. The picture is illuminated by sunlight from the lower left and covers an area about 3 km (1.9 mi) across.
https://photojournal.jpl.nasa.gov/catalog/PIA21555	/content/Nasa_Mars_Images/PIA21555_modest.jpg	This image from NASA's Mars Reconnaissance Orbiter covers the entrance to Mawrth Vallis.	Map Projected Browse ImageClick on the image for larger versionIn Andy Weir's "The Martian," stranded astronaut Mark Watney drives from the Ares 3 landing site in Acidalia Planitia towards the Ares 4 landing site in Schiaparelli Crater via Mawrth Vallis. This image covers the entrance to Mawrth Vallis. (Have a look at the scene in 3D.)As you can tell, driving over this terrain will be much more difficult than it was depicted in the novel or the movie. The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 58.5 centimeters (19.1 inches) per pixel (with 2 x 2 binning); objects on the order of 176 centimeters (69.2 inches) across are resolved.] North is up.This is a stereo pair with ESP_048595_2060.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.
https://photojournal.jpl.nasa.gov/catalog/PIA00945	/content/Nasa_Mars_Images/PIA00945_modest.jpg	This image taken in 1997 by NASA's Mars Global Surveyor shows the orientation and magnitude of the magnetic field measured by the MGS magnetometer as it sped over the surface of Mars during an early aerobraking pass.	This is MOC frame P005_03, a subset of PIA00941. MOC image P005_03 was acquired at 6:25 AM PDT on September 19, 1997, about 11 minutes after Mars Global Surveyor passed close to the planet for the fifth time. During the imaging period, the spacecraft was canted towards the sunlit hemisphere by 25°, and the MOC was obliquely viewing features about 1600 km (1000 miles) away. The resolution at that distance was about 6 meters (20 feet) per picture element (pixels), but in order to improve the number of gray levels, the pixels were summed in both the cross-track and along-track directions, yielding final resolution of about 12 meters (40 feet) per pixel. The MOC image covers an area about 12 km X 12 km (7.5 X 7.5 miles).Labyrinthus Noctis near the crest of a large (many thousands of kilometers) upcoming of the Martian crust, and the 2000 meter (6500 foot) deep canyons visible in these pictures are bounded by faults. Debris shed from the steep slopes has moved down into after the canyons opened. Small dunes are seen in the lowest area, beneath the high cliffs.Launched on November 7, 1996, Mars Global Surveyor entered Mars orbit on Thursday, September 11, 1997. The spacecraft has been using atmospheric drag to reduce the size of its orbit for the past three weeks, and will achieve a circular orbit only 400 km (248 mi) above the surface early next year. Mapping operations begin in March 1998. At that time, MOC narrow angle images will be 5-10 times higher resolution than these pictures.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.