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Dissected Terrain Near Paran …
PIA01507
Sol (our sun)
Mars Orbiter Camera
Title Dissected Terrain Near Parana Valles
Original Caption Released with Image Portion of dissected terrain southeast of Parana Valles (MOC 7705). This heavily gullied landscape(25.9°S, 8.3°W) shows the highest "drainage density" yet seen in MOC images. This image is somewhat lower in resolution (downtrack scale = 21.4 m/pixel, crosstrack = 14.3 m/pixel) but in other parameters comparable to Figures 1 and 2 (incidence angle = 27.5°, emission angle = 14.5°). 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.
Layers within the Valles Mar …
PIA01168
Sol (our sun)
Mars Orbiter Camera
Title Layers within the Valles Marineris: Clues to the Ancient Crust of Mars - High Resolution Image
Original Caption Released with Image This high resolution picture of the Martian surface was obtained in the early evening of January 1, 1998 by the Mars Orbiter Camera (MOC), shortly after the Mars Global Surveyor spacecraft began it's 80th orbit. Seen in this view are a plateau and surrounding steep slopes within the Valles Marineris, the large system of canyons that stretches 4000 km (2500 mi) along the equator of Mars. The image covers a tiny fraction of the canyons at very high resolution: it extends only 9.8 km by 17.3 km (6.1 mi by 10.7 mi) but captures features as small as 6 m (20 ft) across. The highest terrain in the image is the relatively smooth plateau near the center. Slopes descend to the north and south (upper and lower part of image, respectively) in broad, debris-filled gullies with intervening rocky spurs. Multiple rock layers, varying from a few to a few tens of meters thick, are visible in the steep slopes on the spurs and gullies. Layered rocks on Earth form from sedimentary processes (such as those that formed the layered rocks now seen in Arizona's Grand Canyon) and volcanic processes (such as layering seen in the Waimea Canyon on the island of Kauai). Both origins are possible for the Martian layered rocks seen in this image. In either case, the total thickness of the layered rocks seen in this image implies a complex and extremely active early history for geologic processes on Mars. Malin Space Science Systems (MSSS) 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.
Layers within the Valles Mar …
PIA01167
Sol (our sun)
Mars Orbiter Camera
Title Layers within the Valles Marineris: Clues to the Ancient Crust of Mars
Original Caption Released with Image This high resolution picture (right) of the Martian surface was obtained in the early evening of January 1, 1998 by the Mars Orbiter Camera (MOC), shortly after the Mars Global Surveyor spacecraft began it's 80th orbit. Seen in this view are a plateau and surrounding steep slopes within the Valles Marineris, the large system of canyons that stretches 4000 km (2500 mi) along the equator of Mars. The image covers a tiny fraction of the canyons at very high resolution: it extends only 9.8 km by 17.3 km (6.1 mi by 10.7 mi) but captures features as small as 6 m (20 ft) across. The highest terrain in the image is the relatively smooth plateau near the center. Slopes descend to the north and south (upper and lower part of image, respectively) in broad, debris-filled gullies with intervening rocky spurs. Multiple rock layers, varying from a few to a few tens of meters thick, are visible in the steep slopes on the spurs and gullies. Layered rocks on Earth form from sedimentary processes (such as those that formed the layered rocks now seen in Arizona's Grand Canyon) and volcanic processes (such as layering seen in the Waimea Canyon on the island of Kauai). Both origins are possible for the Martian layered rocks seen in this image. In either case, the total thickness of the layered rocks seen in this image implies a complex and extremely active early history for geologic processes on Mars. The left and center "context" images are Viking mosaics reproduced at scales of 230 meters/pixel and 80 meters/pixel respectively. Outlines in these two images represent the location of the higher resolution image(s). Malin Space Science Systems (MSSS) 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.
East Tithonium Chasma Wall, …
PIA01696
Sol (our sun)
Mars Orbiter Camera
Title East Tithonium Chasma Wall, Valles Marineris
Original Caption Released with Image Layers of wall rock, windblown drifts, and landslide deposits can be seen in this new view of the wall of Tithonium Chasma in the Valles Marineris trough system. The picture covers an area 3 kilometers (1.9 miles) wide by about 11 kilometers (6.8 miles) long and is illuminated from the lower right. The Mars Orbiter Camera on board the Mars Global Surveyor spacecraft acquired this dramatic picture in early April 1999. 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.
Western Melas and Candor Cha …
PIA01692
Sol (our sun)
Mars Orbiter Camera
Title Western Melas and Candor Chasms, Valles Marineris
Original Caption Released with Image During its March 1999 operations, the Mars Orbiter Camera (MOC) on board the Mars Global Surveyor (MGS) captured this stunning wide-angle camera view of the western portions of Melas and Candor Chasms in the Valles Marineris canyon system. This view covers an area that is about 80 kilometers (50 miles) wide and 220 kilometers (137 miles)long. Melas Chasma is located at the bottom of the image, Candor at the top. Hints of layers in the canyon walls are evident in this image. Color and albedo (brightness)variations on the floors of each chasm indicate the relative distribution of dark sand and brighter sediments and/or rocks. Dark sand on the floor of Melas Chasma was also seen by MOC in March 1999 (see MOC2-104) [ http://www.msss.com/mars/global_surveyor/camera/images/3_25_99_melas/index.html ] and bright layered material was observed in Candor Chasma in April 1998 (see MOC2-59) [ http://www.msss.com/mars/global_surveyor/camera/images/7_20_98_marineris_rel/index.html ]. The colors shown here are not true colors as they would appear to the human eye. The MOC has cameras that obtain images in red and blue portions of the visible spectrum, the green portion is synthesized using the combined average values of the red and blue channels (a relationship understood from Viking Orbiter imaging in the 1970s). Illumination is from the upper left. 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.
Reull Valles in Approximatel …
PIA00322
Sol (our sun)
Visual Imaging Subsystem - C …
Title Reull Valles in Approximately Natural Color
Original Caption Released with Image Reull Valles, conspicuous southeast-trending fretted channel, dissects wall deposits of the large Hellas impact basin. Center of picture is at latitude 42 degrees S. longitude 258 degrees. Fretted channels are wide, flat-floored channels with steep walls, which may be runoff channels that have been modified and enlarged by mass wasting. Many nearby hills and mountains are surrounded by lobate debris aprons, which may have formed by slow creep of rock deposits aided by the presence of near-surface ice. Layering is exposed in the channel and crater walls. The color variations of the surface are very bland in this region, most of the variations seen in the enhanced-color version (PIA00153) are due to atmospheric scattering. Viking Orbiter Picture Numbers 126A08 (violet), 126A16 (green), and 126A24 (red) at 157 m/pixel resolution. Picture width is 161 km. North is 112 degrees clockwise from top.
Tharsis Volcanoes and Valles …
PIA02005
Sol (our sun)
Mars Orbiter Camera
Title Tharsis Volcanoes and Valles Marineris, Mars
Original Caption Released with Image It is northern summer on Mars and clouds are very common over the famous Tharsis volcanoes during the afternoon. At the far left, a white patchy cloud denotes the location of Olympus Mons. Ascraeus Mons is under the brightest cloud toward the center left, but the volcanoes Pavonis Mons and Arsia Mons (toward lower left below Ascraeus Mons) have much less cloud cover. The patch of clouds toward the upper left mark the location of the Alba Patera volcano. The Valles Marineris trough system--so long that it would stretch across North America--is seen in the lower third of this picture. This is a color composite of 9 red and 9 blue image strips taken by the Mars Global Surveyor Mars Orbiter Camera on 9 successive orbits from pole-to-pole during the calibration phase of the mission in March 1999. The color is computer-enhanced and is not shown as it would actually appear to the human eye. 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.
May 1999 Dust Storm in Valle …
PIA02045
Sol (our sun)
Mars Orbiter Camera
Title May 1999 Dust Storm in Valles Marineris
Original Caption Released with Image Mars Global Surveyor's (MGS) Mars Orbiter Camera (MOC) captured this view of a dust storm within the Ius and Melas Chasms of the Valles Marineris trough system on May 16, 1999. The dust storm is seen in the lower 1/3 of the image. It occurs at the junction between eastern Ius Chasma and western Melas Chasma. The apparent motion of the storm is approximately from the south (bottom of image) toward the north. The dust cloud forms a sharp front along its northern margin, which is seen along the north wall of Ius and Melas Chasms--in fact, at the time the image was taken, the dust had advanced up over the north wall of Melas Chasma (upper portion of lower right third of image) and was advancing across the upland that separates this chasm from western Candor Chasma. For a clear-atmosphere view of western Candor and Melas Chasms, see "Western Melas and Candor Chasms, Valles Marineris, MOC2-105, 25 March 1999" [ http://www.msss.com/mars/global_surveyor/camera/images/3_25_99_vmcolor/index.html ]. For scale, note that the large crater south of Hebes Chasma, Perrotin, is about 95 kilometers (59 miles) across. Bluish-white clouds in the image are interpreted to consist of water ice. The pink/red clouds of the dust storm occur closer to the ground, at a lower altitude than the water ice clouds. One of the most interesting aspects of this dust storm is that Valles Marineris was observed to have a dust storm at exactly the same time of year, one Martian year ago. During its approach to Mars, MOC obtained a picture of the planet on July 2,1997, just prior to the Mars Pathfinder landing. At the time, it was winter in the southern hemisphere, and dust clouds were observed within Valles Marineris. The picture is seen in "Mars Orbiter Camera Views Mars Pathfinder Landing Site,MOC2-1, 3 July 1997" [ http://www.msss.com/mars/global_surveyor/camera/images/c9/index.html ]. It will be interesting to see if similar storms occur within the Valles Marineris 1 and 2 Mars years hence. The next times will be in early April 2001 and mid-February 2003. 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.
Candor Chasm in Valles Marin …
PIA00199
Sol (our sun)
Visual Imaging Subsystem - C …
Title Candor Chasm in Valles Marineris
Original Caption Released with Image Part of Candor Chasm in Valles Marineris, Mars, from about latitude -9 degrees to -3 degrees and longitude 69 degrees to 75 degrees. Layered terrain is visible in the scene, perhaps due to a huge ancient lake. The geomorphology is complex, shaped by tectonics, mass wasting, and wind, and perhaps by water and volcanism.
Groovy Terrain in Mangala Va …
PIA02813
Sol (our sun)
Mars Orbiter Camera
Title Groovy Terrain in Mangala Valles
Original Caption Released with Image When it was proposed to NASA in 1985, one of the goals of the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) experiment was to take pictures with high enough resolution to be able to see large boulders on the planet's surface. For large martian outflow channels--believed by some to have been carved by giant floods several billion years ago--seeing boulders and measuring their size and distribution in the channels can tell geologists something about the nature of the flood--for example, how fast the water was moving, and, in some cases, how deep it was. But Mars doesn't always cooperate. The white box in the context image on the right shows the location of the high resolution MOC image on the left. The white box in the context frame is located among buttes and mesas within Mangala Valles, one of the large martian channels thought to have been carved by floods long ago. The high resolution view, however, offers no insight into the processes that formed Mangala Valles. Instead, the entire surface--mesa tops, buttes, and channel floor--are all covered-up with a thick blanket of wind-eroded, ridged and grooved material. Some of the buttes and mesas have boulders on their surfaces, and wind has hollowed-out circular depressions around these boulders. But the boulders in this case probably have nothing to do with the floods that might have formed Mangala Valles--they are boulders exposed in the bedrock contained beneath the ridged and grooved mantle that covers each butte and mesa. The dark streaks on slopes in this image are places where dry accumulations of dust have slid downhill, much like a snow avalanche. Similar streaks have been seen elsewhere on the dusty surfaces of Mars, and some have been found to change over time. For example, see Recent Movements: New Landslides in Less than 1 Martian year [ http://photojournal.jpl.nasa.gov/catalog/PIA02379 ]. This picture is located near 8.7°S, 151.2°W, it covers an area 3 km (1.9 mi) by 11.7 km (7.3 mi). North is toward the upper right, and illumination is from the upper left. This is a subframe of MOC image M11-01809, acquired January 13, 2000. To see what the raw MOC image data look like, visit the newest data releases (for Mission Subphases M07 - M12, covering September 1999 through February 2000) in the MOC GALLERY [ http://www.msss.com/moc_gallery ].
Groovy Terrain in Mangala Va …
PIA02813
Sol (our sun)
Mars Orbiter Camera
Title Groovy Terrain in Mangala Valles
Original Caption Released with Image When it was proposed to NASA in 1985, one of the goals of the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) experiment was to take pictures with high enough resolution to be able to see large boulders on the planet's surface. For large martian outflow channels--believed by some to have been carved by giant floods several billion years ago--seeing boulders and measuring their size and distribution in the channels can tell geologists something about the nature of the flood--for example, how fast the water was moving, and, in some cases, how deep it was. But Mars doesn't always cooperate. The white box in the context image on the right shows the location of the high resolution MOC image on the left. The white box in the context frame is located among buttes and mesas within Mangala Valles, one of the large martian channels thought to have been carved by floods long ago. The high resolution view, however, offers no insight into the processes that formed Mangala Valles. Instead, the entire surface--mesa tops, buttes, and channel floor--are all covered-up with a thick blanket of wind-eroded, ridged and grooved material. Some of the buttes and mesas have boulders on their surfaces, and wind has hollowed-out circular depressions around these boulders. But the boulders in this case probably have nothing to do with the floods that might have formed Mangala Valles--they are boulders exposed in the bedrock contained beneath the ridged and grooved mantle that covers each butte and mesa. The dark streaks on slopes in this image are places where dry accumulations of dust have slid downhill, much like a snow avalanche. Similar streaks have been seen elsewhere on the dusty surfaces of Mars, and some have been found to change over time. For example, see Recent Movements: New Landslides in Less than 1 Martian year [ http://photojournal.jpl.nasa.gov/catalog/PIA02379 ]. This picture is located near 8.7°S, 151.2°W, it covers an area 3 km (1.9 mi) by 11.7 km (7.3 mi). North is toward the upper right, and illumination is from the upper left. This is a subframe of MOC image M11-01809, acquired January 13, 2000. To see what the raw MOC image data look like, visit the newest data releases (for Mission Subphases M07 - M12, covering September 1999 through February 2000) in the MOC GALLERY [ http://www.msss.com/moc_gallery ].
Groovy Terrain in Mangala Va …
PIA02813
Sol (our sun)
Mars Orbiter Camera
Title Groovy Terrain in Mangala Valles
Original Caption Released with Image When it was proposed to NASA in 1985, one of the goals of the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) experiment was to take pictures with high enough resolution to be able to see large boulders on the planet's surface. For large martian outflow channels--believed by some to have been carved by giant floods several billion years ago--seeing boulders and measuring their size and distribution in the channels can tell geologists something about the nature of the flood--for example, how fast the water was moving, and, in some cases, how deep it was. But Mars doesn't always cooperate. The white box in the context image on the right shows the location of the high resolution MOC image on the left. The white box in the context frame is located among buttes and mesas within Mangala Valles, one of the large martian channels thought to have been carved by floods long ago. The high resolution view, however, offers no insight into the processes that formed Mangala Valles. Instead, the entire surface--mesa tops, buttes, and channel floor--are all covered-up with a thick blanket of wind-eroded, ridged and grooved material. Some of the buttes and mesas have boulders on their surfaces, and wind has hollowed-out circular depressions around these boulders. But the boulders in this case probably have nothing to do with the floods that might have formed Mangala Valles--they are boulders exposed in the bedrock contained beneath the ridged and grooved mantle that covers each butte and mesa. The dark streaks on slopes in this image are places where dry accumulations of dust have slid downhill, much like a snow avalanche. Similar streaks have been seen elsewhere on the dusty surfaces of Mars, and some have been found to change over time. For example, see Recent Movements: New Landslides in Less than 1 Martian year [ http://photojournal.jpl.nasa.gov/catalog/PIA02379 ]. This picture is located near 8.7°S, 151.2°W, it covers an area 3 km (1.9 mi) by 11.7 km (7.3 mi). North is toward the upper right, and illumination is from the upper left. This is a subframe of MOC image M11-01809, acquired January 13, 2000. To see what the raw MOC image data look like, visit the newest data releases (for Mission Subphases M07 - M12, covering September 1999 through February 2000) in the MOC GALLERY [ http://www.msss.com/moc_gallery ].
Groovy Terrain in Mangala Va …
PIA02813
Sol (our sun)
Mars Orbiter Camera
Title Groovy Terrain in Mangala Valles
Original Caption Released with Image When it was proposed to NASA in 1985, one of the goals of the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) experiment was to take pictures with high enough resolution to be able to see large boulders on the planet's surface. For large martian outflow channels--believed by some to have been carved by giant floods several billion years ago--seeing boulders and measuring their size and distribution in the channels can tell geologists something about the nature of the flood--for example, how fast the water was moving, and, in some cases, how deep it was. But Mars doesn't always cooperate. The white box in the context image on the right shows the location of the high resolution MOC image on the left. The white box in the context frame is located among buttes and mesas within Mangala Valles, one of the large martian channels thought to have been carved by floods long ago. The high resolution view, however, offers no insight into the processes that formed Mangala Valles. Instead, the entire surface--mesa tops, buttes, and channel floor--are all covered-up with a thick blanket of wind-eroded, ridged and grooved material. Some of the buttes and mesas have boulders on their surfaces, and wind has hollowed-out circular depressions around these boulders. But the boulders in this case probably have nothing to do with the floods that might have formed Mangala Valles--they are boulders exposed in the bedrock contained beneath the ridged and grooved mantle that covers each butte and mesa. The dark streaks on slopes in this image are places where dry accumulations of dust have slid downhill, much like a snow avalanche. Similar streaks have been seen elsewhere on the dusty surfaces of Mars, and some have been found to change over time. For example, see Recent Movements: New Landslides in Less than 1 Martian year [ http://photojournal.jpl.nasa.gov/catalog/PIA02379 ]. This picture is located near 8.7°S, 151.2°W, it covers an area 3 km (1.9 mi) by 11.7 km (7.3 mi). North is toward the upper right, and illumination is from the upper left. This is a subframe of MOC image M11-01809, acquired January 13, 2000. To see what the raw MOC image data look like, visit the newest data releases (for Mission Subphases M07 - M12, covering September 1999 through February 2000) in the MOC GALLERY [ http://www.msss.com/moc_gallery ].
Groovy Terrain in Mangala Va …
PIA02813
Sol (our sun)
Mars Orbiter Camera
Title Groovy Terrain in Mangala Valles
Original Caption Released with Image When it was proposed to NASA in 1985, one of the goals of the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) experiment was to take pictures with high enough resolution to be able to see large boulders on the planet's surface. For large martian outflow channels--believed by some to have been carved by giant floods several billion years ago--seeing boulders and measuring their size and distribution in the channels can tell geologists something about the nature of the flood--for example, how fast the water was moving, and, in some cases, how deep it was. But Mars doesn't always cooperate. The white box in the context image on the right shows the location of the high resolution MOC image on the left. The white box in the context frame is located among buttes and mesas within Mangala Valles, one of the large martian channels thought to have been carved by floods long ago. The high resolution view, however, offers no insight into the processes that formed Mangala Valles. Instead, the entire surface--mesa tops, buttes, and channel floor--are all covered-up with a thick blanket of wind-eroded, ridged and grooved material. Some of the buttes and mesas have boulders on their surfaces, and wind has hollowed-out circular depressions around these boulders. But the boulders in this case probably have nothing to do with the floods that might have formed Mangala Valles--they are boulders exposed in the bedrock contained beneath the ridged and grooved mantle that covers each butte and mesa. The dark streaks on slopes in this image are places where dry accumulations of dust have slid downhill, much like a snow avalanche. Similar streaks have been seen elsewhere on the dusty surfaces of Mars, and some have been found to change over time. For example, see Recent Movements: New Landslides in Less than 1 Martian year [ http://photojournal.jpl.nasa.gov/catalog/PIA02379 ]. This picture is located near 8.7°S, 151.2°W, it covers an area 3 km (1.9 mi) by 11.7 km (7.3 mi). North is toward the upper right, and illumination is from the upper left. This is a subframe of MOC image M11-01809, acquired January 13, 2000. To see what the raw MOC image data look like, visit the newest data releases (for Mission Subphases M07 - M12, covering September 1999 through February 2000) in the MOC GALLERY [ http://www.msss.com/moc_gallery ].
Looking Out Across Dao, Nige …
PIA02810
Sol (our sun)
Mars Orbiter Camera
Title Looking Out Across Dao, Niger, and Harmakhis Valles
Original Caption Released with Image The Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) opened its fourth year orbiting the red planet with this mid-autumn view of three major valley systems east of the Hellas plains. From left to right, the first major valley, Dao Vallis, runs diagonally from the upper left to just past the lower center of the image. Niger Vallis joins Dao Vallis just above the center of the frame. Harmakhis Vallis extends diagonally across the right half of the picture, toward the lower right. These valleys are believed by some to have been formed--at least in part--by large outbursts of liquid water some time far back in the martian past, though there is no way to know exactly how many hundreds of millions or billions of years ago this might have occurred. In each valley, water would have flowed toward the bottom of the image. Although their dimensions vary along their courses, the valleys are all roughly 1 km (0.6 miles) deep and range in width from about 40 km (25 miles) down to about 8 km (5 mi). Located around 40°S, 270°W, the picture covers an area approximately 800 km across and is illuminated by sunlight from the lower left. North is toward the left, the picture is a composite of red and blue wide angle images obtained by MOC on September 13, 2000.
Light-toned Layered Outcrops …
PIA02847
Sol (our sun)
Mars Orbiter Camera
Title Light-toned Layered Outcrops in Valles Marineris Walls
Original Caption Released with Image Valles Marineris a system of troughs, chasms, and pit chains that stretches more than 4,000 km (2,500 miles) across the martian western hemisphere. Outcrops of layered material found in mounds and mesas within the chasms of the Valles Marineris were known from the pictures taken by Mariner 9 in 1972 and the Viking orbiters of 1976-1980. One example of the those known previously is the mesa labeled "Candor Mensa" in the context image (above), another example is the mound in the center of Ganges Chasma. For several decades, it has been widely speculated among Mars scientists that the light- and dark-toned layered materials in the Valles Marineris might have formed in lakes that had once filled the chasms during the most recent epoch of martian history, others thought they might result from volcanic ash deposited in the chasms. Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) images have confirmed the presence of light- and dark-toned layered sedimentary rock outcrops in the Valles Marineris, but they have also revealed many more than were previously known and they have shown several good examples that these materials are coming out of the walls of the Valles Marineris chasms. The fact that these materials come out of the chasm walls means that the layers do not represent lakes (or volcanic debris) that formed in the Valles Marineris. Instead, they represent materials deposited and buried long before there ever was a Valles Marineris. They are seen now because of the faulting and erosion that opened up and widened the Valles Marineris troughs. The context image is a mosaic of Viking 1 orbiter images taken in 1976 showing a portion of the wall that separates western Ophir Chasma from western Candor Chasma in the Valles Marineris. This area is located around 5°S, 74°W. The white box labeled "M17-00467" shows the location of a subframe of MOC image M17-00467 that was acquired in July 2000 to allow scientists to examine one of the many bright patches (indicated by small arrows) seen on the walls of Valles Marineris. The release image is a subframe of MOC image M17-00467, showing a high-resolution view of one of the bright patches on the walls of Candor Chasma. The MOC image reveals that the bright material indeed consists of light-toned layered rock similar to other outcrops thought to be sedimentary in origin found throughout the Valles Marineris. The dark ridge running from top center to center-left in this view is mantled by a smooth, dark material that covers additional light-toned layered rock. The observation that these kinds of bright layered rock occur within the walls of the Valles Marineris indicate that the materials are very, very old. They have been buried under several kilometers (i.e., more than a mile) of additional layered rock, all of which is beneath plains thought to be more than 2.5 to 3.5 billion years old. These relationships suggest that all of the layered sedimentary rocks observed on Mars by MGS MOC may date back to the, earliest parts of martian history, between 3.5 and 4.5 billion years ago. In both pictures, north is toward the top. Sunlight illuminates the context image from the top/right, the MOC image (top left) is illuminated from the upper left.
Light-toned Layered Outcrops …
PIA02847
Sol (our sun)
Mars Orbiter Camera
Title Light-toned Layered Outcrops in Valles Marineris Walls
Original Caption Released with Image Valles Marineris a system of troughs, chasms, and pit chains that stretches more than 4,000 km (2,500 miles) across the martian western hemisphere. Outcrops of layered material found in mounds and mesas within the chasms of the Valles Marineris were known from the pictures taken by Mariner 9 in 1972 and the Viking orbiters of 1976-1980. One example of the those known previously is the mesa labeled "Candor Mensa" in the context image (above), another example is the mound in the center of Ganges Chasma. For several decades, it has been widely speculated among Mars scientists that the light- and dark-toned layered materials in the Valles Marineris might have formed in lakes that had once filled the chasms during the most recent epoch of martian history, others thought they might result from volcanic ash deposited in the chasms. Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) images have confirmed the presence of light- and dark-toned layered sedimentary rock outcrops in the Valles Marineris, but they have also revealed many more than were previously known and they have shown several good examples that these materials are coming out of the walls of the Valles Marineris chasms. The fact that these materials come out of the chasm walls means that the layers do not represent lakes (or volcanic debris) that formed in the Valles Marineris. Instead, they represent materials deposited and buried long before there ever was a Valles Marineris. They are seen now because of the faulting and erosion that opened up and widened the Valles Marineris troughs. The context image is a mosaic of Viking 1 orbiter images taken in 1976 showing a portion of the wall that separates western Ophir Chasma from western Candor Chasma in the Valles Marineris. This area is located around 5°S, 74°W. The white box labeled "M17-00467" shows the location of a subframe of MOC image M17-00467 that was acquired in July 2000 to allow scientists to examine one of the many bright patches (indicated by small arrows) seen on the walls of Valles Marineris. The release image is a subframe of MOC image M17-00467, showing a high-resolution view of one of the bright patches on the walls of Candor Chasma. The MOC image reveals that the bright material indeed consists of light-toned layered rock similar to other outcrops thought to be sedimentary in origin found throughout the Valles Marineris. The dark ridge running from top center to center-left in this view is mantled by a smooth, dark material that covers additional light-toned layered rock. The observation that these kinds of bright layered rock occur within the walls of the Valles Marineris indicate that the materials are very, very old. They have been buried under several kilometers (i.e., more than a mile) of additional layered rock, all of which is beneath plains thought to be more than 2.5 to 3.5 billion years old. These relationships suggest that all of the layered sedimentary rocks observed on Mars by MGS MOC may date back to the, earliest parts of martian history, between 3.5 and 4.5 billion years ago. In both pictures, north is toward the top. Sunlight illuminates the context image from the top/right, the MOC image (top left) is illuminated from the upper left.
Light-toned Layered Outcrops …
PIA02847
Sol (our sun)
Mars Orbiter Camera
Title Light-toned Layered Outcrops in Valles Marineris Walls
Original Caption Released with Image Valles Marineris a system of troughs, chasms, and pit chains that stretches more than 4,000 km (2,500 miles) across the martian western hemisphere. Outcrops of layered material found in mounds and mesas within the chasms of the Valles Marineris were known from the pictures taken by Mariner 9 in 1972 and the Viking orbiters of 1976-1980. One example of the those known previously is the mesa labeled "Candor Mensa" in the context image (above), another example is the mound in the center of Ganges Chasma. For several decades, it has been widely speculated among Mars scientists that the light- and dark-toned layered materials in the Valles Marineris might have formed in lakes that had once filled the chasms during the most recent epoch of martian history, others thought they might result from volcanic ash deposited in the chasms. Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) images have confirmed the presence of light- and dark-toned layered sedimentary rock outcrops in the Valles Marineris, but they have also revealed many more than were previously known and they have shown several good examples that these materials are coming out of the walls of the Valles Marineris chasms. The fact that these materials come out of the chasm walls means that the layers do not represent lakes (or volcanic debris) that formed in the Valles Marineris. Instead, they represent materials deposited and buried long before there ever was a Valles Marineris. They are seen now because of the faulting and erosion that opened up and widened the Valles Marineris troughs. The context image is a mosaic of Viking 1 orbiter images taken in 1976 showing a portion of the wall that separates western Ophir Chasma from western Candor Chasma in the Valles Marineris. This area is located around 5°S, 74°W. The white box labeled "M17-00467" shows the location of a subframe of MOC image M17-00467 that was acquired in July 2000 to allow scientists to examine one of the many bright patches (indicated by small arrows) seen on the walls of Valles Marineris. The release image is a subframe of MOC image M17-00467, showing a high-resolution view of one of the bright patches on the walls of Candor Chasma. The MOC image reveals that the bright material indeed consists of light-toned layered rock similar to other outcrops thought to be sedimentary in origin found throughout the Valles Marineris. The dark ridge running from top center to center-left in this view is mantled by a smooth, dark material that covers additional light-toned layered rock. The observation that these kinds of bright layered rock occur within the walls of the Valles Marineris indicate that the materials are very, very old. They have been buried under several kilometers (i.e., more than a mile) of additional layered rock, all of which is beneath plains thought to be more than 2.5 to 3.5 billion years old. These relationships suggest that all of the layered sedimentary rocks observed on Mars by MGS MOC may date back to the, earliest parts of martian history, between 3.5 and 4.5 billion years ago. In both pictures, north is toward the top. Sunlight illuminates the context image from the top/right, the MOC image (top left) is illuminated from the upper left.
Reull Valles (Enhanced Color …
PIA00153
Sol (our sun)
Visual Imaging Subsystem - C …
Title Reull Valles (Enhanced Color)
Original Caption Released with Image A conspicuous fretted channel, Reull Valles, which dissects wall deposits of the large Hellas impact basin, trends southeast towards the basin floor. Center of picture is at latitude 42 degrees S., longitude 258 degrees W. Fretted channels are wide, flat-floored channels with steep walls, which may be runoff channels that have been modified and enlarged by masswasting. Many nearby hills and mountains are surrounded by lobate debris aprons, which may have formed by slow creep of rock deposits aided by the presence of near-surface ice. Layering is exposed in the channel and crater walls. The color variations of the surface are very bland in this region, most of the variations seen are due to atmospheric scattering. Viking Orbiter Picture Numbers 126A08 (violet), 126A16 (green), and 126A24 (red) at 157 m/pixel resolution. Picture width is 161 km. North is 112 degrees clockwise from top.
Mamers Valles
PIA04098
Sol (our sun)
Thermal Emission Imaging Sys …
Title Mamers Valles
Original Caption Released with Image A broad channel in the Deuteronilus Mensae region displays the strange landforms common to the northern mid-latitudes where ground ice likely plays a role in their formation. A tongue-shaped feature at the bottom of this image looks surprisingly glacier-like in its morphology. 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 37.1, Longitude 15.3 East (344.7 West). 19 meter/pixel resolution.
Mamers Valles
PIA04098
Sol (our sun)
Thermal Emission Imaging Sys …
Title Mamers Valles
Original Caption Released with Image A broad channel in the Deuteronilus Mensae region displays the strange landforms common to the northern mid-latitudes where ground ice likely plays a role in their formation. A tongue-shaped feature at the bottom of this image looks surprisingly glacier-like in its morphology. 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 37.1, Longitude 15.3 East (344.7 West). 19 meter/pixel resolution.
Landslide in Kasei Valles
PIA04269
Sol (our sun)
Mars Orbiter Camera
Title Landslide in Kasei Valles
Original Caption Released with Image The Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) continues in 2003 to return excellent, high resolution images of the red planet's surface. This nearly 1.5 meters (5 ft.) per pixel view of a landslide on a 200 meter-high (219 yards-high) slope in Kasei Valles was specifically targeted for scientific investigation by rotating the MGS spacecraft about 7.8° off-nadir in January 2003. The scar left by the landslide reveals layers in the bedrock at the top the slope and shows a plethora of dark-toned, house-sized boulders that rolled down the slope and collected at the base of the landslide scar. A few meteor impact craters have formed on the landslide deposit and within the scar, indicating that this landslide occurred a very long time ago. Sunlight illuminates this scene from the left/lower left, the landslide is located near 28.3°N, 71.9°W.
Hebrus Valles
PIA04451
Sol (our sun)
Thermal Emission Imaging Sys …
Title Hebrus Valles
Original Caption Released with Image About 1000 km west of the massive Elysium volcanic complex, a system of branching troughs shows a continuum of features that provides clues to their origin. Within the scene there are fully formed troughs, some approaching 2 km in depth, as well as shallow, discontinuous pits and troughs. The presence of the latter landforms suggests that a process of collapse is responsible for producing the deep and continuous final form of the troughs. 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 21.1, Longitude 123.3 East (236.7 West). 19 meter/pixel resolution.
Hebrus Valles
PIA04451
Sol (our sun)
Thermal Emission Imaging Sys …
Title Hebrus Valles
Original Caption Released with Image About 1000 km west of the massive Elysium volcanic complex, a system of branching troughs shows a continuum of features that provides clues to their origin. Within the scene there are fully formed troughs, some approaching 2 km in depth, as well as shallow, discontinuous pits and troughs. The presence of the latter landforms suggests that a process of collapse is responsible for producing the deep and continuous final form of the troughs. 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 21.1, Longitude 123.3 East (236.7 West). 19 meter/pixel resolution.
The Layer Cake Walls of Vall …
PIA10074
Sol (our sun)
CRISM
Title The Layer Cake Walls of Valles Marineris
Original Caption Released with Image This image of the northern wall of Coprates Chasma, in Valles Marineris, was taken by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) at 1227 UTC (8:27 a.m. EDT) on June 16, 2007, near 13.99 degrees south latitude, 303.09 degrees east longitude. CRISM's image was taken in 544 colors covering 0.36-3.92 micrometers, and shows features as small as 20 meters (66 feet) across. The region covered is just over 10 kilometers (6.2 miles) wide at its narrowest point. Valles Marineris is a large canyon system straddling Mars' equator, with a total size approximating the Mediterranean Sea emptied of water. It is subdivided into several interconnected "chasmata" each hundreds of kilometers wide and, in some cases, thousands of kilometers long. The walls of several of the chasmata, including Coprates Chasma, expose a section of Mars' upper crust about 5 kilometers (3 miles) in depth. Exposures like these show the layers of rock that record the formation of Mars' crust over geologic time, much as the walls of the Grand Canyon on Earth show part of our planet's history. The upper panel of this montage shows the location of the CRISM image on a mosaic from the Mars Odyssey spacecraft's Thermal Emission Imaging System (THEMIS), taken in longer infrared wavelengths than measured by CRISM. The CRISM image samples the base of Coprates Chasma's wall, including a conspicuous horizontal band that continues along the wall for tens of kilometers to the east and west, and a topographic shelf just above that. The middle two panels show the CRISM image in visible and infrared light. In the middle left panel, the red, green, and blue image planes show brightness at 0.59, 0.53, and 0.48 microns, similar to what the human eye would see. Color variations are subdued by the presence of dust on all exposed surfaces. In the middle right panel, the red, green, and blue image planes show brightness at 2.53, 1.51, and 1.08 microns. These three infrared wavelengths are the "usual" set that the CRISM team uses to provide an overview of infrared data, because dust has a less obscuring effect, and because they are sensitive to a wide variety of minerals. Layering is clearly evident in the wall rocks. The conspicuous band running along the base of the chasma wall appears slightly yellowish, and the scarp at the edge of the topographic bench appears slightly green. The bottom two panels use combinations of wavelengths to show the strengths of absorptions that provide "fingerprints" of different minerals. In the lower left panel, red shows strength of a 0.53-micron absorption due to oxidized iron in dust, green shows strength of an inflection in the spectrum at 0.6 microns that may be related to rock coatings, and blue shows strength of a 1-micron absorption due to the igneous minerals olivine and pyroxene. The conspicuous horizontal band appears slightly blue, indicating a stronger signature of olivine and/or pyroxene. In the lower right panel, red is a measure of, an absorption particular to olivine, green is a measure of a 2.3-micron absorption due to phyllosilicates (clay-like minerals formed when rock was subjected to liquid water), and blue is a measure of absorptions particular to pyroxene. The conspicuous horizontal band is now resolved into an upper portion richer in pyroxene, underlain by material richer in olivine than the rest of the wall rock. Also, erosion-resistant material forming the topographic bench is underlain by phyllosilicate-containing material exposed on the scarp. Taken together, these data reveal a layer cake-like composition of the crustal material exposed in Coprates Chasma's wall. Most of the rock is rich in pyroxene, which is expected because much of Mars' crust consists of volcanic basaltic rock. However discrete layers are richer in olivine, and in some layers the presence of phyllosilicates indicates interaction of rock with liquid water. Because the phyllosilicate-containing layer is low on the walls and deeply buried, it likely represents an early period of Mars' history that was exposed when the canyon system formed. The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) is one of six science instruments on NASA's Mars Reconnaissance Orbiter. Led by The Johns Hopkins University Applied Physics Laboratory, the CRISM team includes expertise from universities, government agencies and small businesses in the United States and abroad.
Valles Marineris and Chryse …
PIA00426
Sol (our sun)
Title Valles Marineris and Chryse Outflow Channels
Original Caption Released with Image A color image of Valles Marineris, the great canyon and the south Chryse basin-Valles Marineris outflow channels of Mars, north toward top. The scene shows the entire Valles Marineris canyon system, over 3,000 km long and averaging 8 km deep, extending from Noctis Labyrinthus, the arcuate system of graben to the west, to the chaotic terrain to the east and related outflow canyons that drain toward the Chryse basin. Eos and Capri Chasmata (south to north) are two canyons connected to Valles Marineris. Ganges Chasma lies directly north. The chaos in the southeast part of the image gives rise to several outflow channels, Shalbatana, Simud, Tiu, and Ares Valles (left to right), that drained north into the Chryse basin. The mouth of Ares Valles is the site of the Mars Pathfinder lander. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color, Mercator projection. The image roughly extends from latitude 20 degrees S. to 20 degrees N. and from longitude 15 degrees to 102.5 degrees. The connected chasma or valleys of Valles Marineris may have formed from a combination of erosional collapse and structural activity. Layers of material in the eastern canyons might consist of carbonates deposited in ancient lakes, eolian deposits, or volcanic materials. Huge ancient river channels began from Valles Marineris and from adjacent canyons and ran north. Many of the channels flowed north into Chryse Basin. The south Chryse outflow channels are cut an average of 1 km into the cratered highland terrain. This terrain is about 9 km above datum near Valles Marineris and steadily decreases in elevation to 1 km below datum in the Chryse basin. Shalbatana is relatively narrow (10 km wide) but can reach 3 km in depth. The channel begins at a 2- to 3-km-deep circular depression within a large impact crater, whose floor is partly covered by chaotic material, and ends in Simud Valles. Tiu and Simud Valles consist of a complex of connected channel floors and chaotic terrain and extend as far south as and connect to eastern Valles Marineris. Ares Vallis originates from discontinuous patches of chaotic terrain within large craters. In the Chryse basin the Ares channel forks, one branch continues northwest into central Chryse Planitia and the other extends north into eastern Chryse Planitia.
Valles Marineris
PIA00422
Sol (our sun)
Title Valles Marineris
Original Caption Released with Image A color image of Valles Marineris, the great canyon of Mars, north toward top. The scene shows the entire canyon system, over 3,000 km long and averaging 8 km deep, extending from Noctis Labyrinthus, the arcuate system of graben to the west, to the chaotic terrain to the east. This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color, Mercator projection. The image extends from latitude 0 degrees to 20 degrees S. and from longitude 45 degrees to 102.5 degrees. The connected chasma or valleys of Valles Marineris may have formed from a combination of erosional collapse and structural activity. Layers of material in the eastern canyons might consist of carbonates deposited in ancient lakes. Huge ancient river channels began from Valles Marineris and from adjacent canyons and ran north. Many of the channels flowed north into Chryse Basin, which contains the site of the Viking 1 Lander and the future site of the Mars Pathfinder Lander.
Pits Near Rhabon Valles
PIA06329
Sol (our sun)
Mars Orbiter Camera
Title Pits Near Rhabon Valles
Original Caption Released with Image 25 June 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a series of pits running down the center of a broad, shallow trough called a "graben". On Mars, many such troughs, and attendant pits, are the result of geologic forces that extended the crust as the Tharsis region of Mars bulged outward to form what is known as, well, the Tharsis Bulge. This graben and pit chain are located near the Rhabon Valles around 23.8°N, 92.3°W. The image covers an area about 3 km (1.9 mi) wide, sunlight illuminates the scene from the lower left.
Bedforms in Maja Valles
PIA06925
Sol (our sun)
Mars Orbiter Camera
Title Bedforms in Maja Valles
Original Caption Released with Image 8 October 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows large, light-toned, ripple-like windblown bedforms in a portion of the giant flood channel complex, Maja Valles. Ripples such as these are very common on Mars but not very well understood. They are larger than most ripples on Earth, and smaller than typical dunes. They are usually old, and probably immobile, features. Sometimes, larger, dark sand dunes are seen riding over them (although that is not the case here). If similarly-sized ripples were to be investigated by a Mars rover, they would probably provide critical information that would help determine the nature of bedforms like these all over Mars. The Maja Valles scene shown here is located near 17.7°N, 54.8°W, and covers an area about 1.4 km (0.9 mi) wide. Sunlight illuminates the scene from the lower left.
Valles Marineris Features
PIA06943
Sol (our sun)
Mars Orbiter Camera
Title Valles Marineris Features
Original Caption Released with Image 17 October 2004 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows light-toned, ripple-like, windblown bedforms and ridges with dark talus accumulations on their slopes in the western portion of the vast Valles Marineris trough system. These features are located near Oudemans Crater around 7.6°S, 91.2°W. The image covers an area about 3 km (1.9 mi) wide and sunlight illuminates the scene from the upper left.
Auqakuh Valles
PIA03824
Sol (our sun)
Thermal Emission Imaging Sys …
Title Auqakuh Valles
Original Caption Released with Image (Released 7 June 2002) The Science This ancient sinuous river channel, located near 30° N, 299° W (61° E), was likely carved by water early in Mars history. Auqakuh Valles cuts through a remarkable series of rock layers that were deposited and then subsequently eroded. This change from conditions favoring deposition to those favoring erosion indicates that the environment of this region has changed significantly over time. In addition, the different rock layers seen in this image vary in hardness, with some being relatively soft and easily eroded, whereas others are harder and resistant. These differences imply that these layers vary in their composition, physical properties, and/or degree of cementation, and again suggest that major changes have occurred during the history of this region. Similar differences occur throughout the southwest U.S., where hard rock layers, such as the limestones and sandstones in the Grand Canyon, form resistant cliffs, whereas softer mudstones are easily eroded to form broad slopes. The Martian layers, such as the smooth, dark-toned mesas visible in numerous places to the right (east) of the channel, were once continuous across the region. As these layers have eroded, they have produced a wide array of textures, from smooth surfaces, to knobby terrains, to the unusual lobate patterns seen in the upper right of the image. The most recent activity in the region appears to be the formation of mega-ripples by the wind. These ripples, spaced approximately 75 m apart, form perpendicular to the wind direction, and can be seen following the pattern of the channel floor as it curves through this region. This pattern shows that even this relatively small channel, which varies in width from about 500 to 750 m throughout this image, acts to funnel the wind down the channel. The Story Auqakuh Vallis, an ancient river channel that winds its way down the center of this image, is the "fossil" remains of an earlier, probably more watery time in Martian history. Now, you might think that Auqakuh has something to do with Aqua, the Latin word for water. Instead, Auqakuh is the word for Mars in the Quechuan language of the Incan Empire that once stretched across vast portions of South America. This Inca-honoring river channel cuts through a remarkable series of rock layers that expose a history of climate change in the region. The coarse, rugged, and wildly textured terrain was created as rock layers were first deposited, then eroded over time. Some of the rock layers are soft and easily eroded, while others are clearly harder and more resistant. From these differences, geologists can tell that the layers are made up of different materials, have different physical characteristics, and are either loosely or strongly cemented together. That suggests major environmental changes over time as well, since different kinds of rocks form under different conditions. Similar differences in rock layers occur throughout the Southwest of the, United States. The next time you're visiting the Grand Canyon or hiking in similar terrain, notice where hard rock layers, such as limestones and sandstones, form resistant cliffs, whereas softer mudstones are easily eroded to form broad slopes along the canyon. Just in case the river channel in the above image looks more like a raised vein rather than a hollowed out channel, try looking at the half-circle depression on the left-hand side of the image, about a third of the way up. The bright features on the upper half streak down toward the bottom of the bowl. Once you focus on this for a while, your brain figures out that the channel must be depressed as well. Now that you can see that the channel cuts into the surface, click on the image for a closer look at the bottom of the channel. Mega-ripples about 82 yards apart line the channel floor as it curves through the region. This pattern shows that even this relatively small channel, which varies from about one-third to a half of a mile in width, funnels the wind down its curving length, creating perpendicular piles of waving texture on the channel's floor. East of the channel, smooth, dark-toned mesas are visible, providing a scant reminder that they were once continuous across the region. As these layers have eroded, they've produced a wide array of textures, from smooth surfaces, to knobby terrains, to the unusual curved, lobe-like patterns seen in the upper right of the image.
Auqakuh Valles
PIA03824
Sol (our sun)
Thermal Emission Imaging Sys …
Title Auqakuh Valles
Original Caption Released with Image (Released 7 June 2002) The Science This ancient sinuous river channel, located near 30° N, 299° W (61° E), was likely carved by water early in Mars history. Auqakuh Valles cuts through a remarkable series of rock layers that were deposited and then subsequently eroded. This change from conditions favoring deposition to those favoring erosion indicates that the environment of this region has changed significantly over time. In addition, the different rock layers seen in this image vary in hardness, with some being relatively soft and easily eroded, whereas others are harder and resistant. These differences imply that these layers vary in their composition, physical properties, and/or degree of cementation, and again suggest that major changes have occurred during the history of this region. Similar differences occur throughout the southwest U.S., where hard rock layers, such as the limestones and sandstones in the Grand Canyon, form resistant cliffs, whereas softer mudstones are easily eroded to form broad slopes. The Martian layers, such as the smooth, dark-toned mesas visible in numerous places to the right (east) of the channel, were once continuous across the region. As these layers have eroded, they have produced a wide array of textures, from smooth surfaces, to knobby terrains, to the unusual lobate patterns seen in the upper right of the image. The most recent activity in the region appears to be the formation of mega-ripples by the wind. These ripples, spaced approximately 75 m apart, form perpendicular to the wind direction, and can be seen following the pattern of the channel floor as it curves through this region. This pattern shows that even this relatively small channel, which varies in width from about 500 to 750 m throughout this image, acts to funnel the wind down the channel. The Story Auqakuh Vallis, an ancient river channel that winds its way down the center of this image, is the "fossil" remains of an earlier, probably more watery time in Martian history. Now, you might think that Auqakuh has something to do with Aqua, the Latin word for water. Instead, Auqakuh is the word for Mars in the Quechuan language of the Incan Empire that once stretched across vast portions of South America. This Inca-honoring river channel cuts through a remarkable series of rock layers that expose a history of climate change in the region. The coarse, rugged, and wildly textured terrain was created as rock layers were first deposited, then eroded over time. Some of the rock layers are soft and easily eroded, while others are clearly harder and more resistant. From these differences, geologists can tell that the layers are made up of different materials, have different physical characteristics, and are either loosely or strongly cemented together. That suggests major environmental changes over time as well, since different kinds of rocks form under different conditions. Similar differences in rock layers occur throughout the Southwest of the, United States. The next time you're visiting the Grand Canyon or hiking in similar terrain, notice where hard rock layers, such as limestones and sandstones, form resistant cliffs, whereas softer mudstones are easily eroded to form broad slopes along the canyon. Just in case the river channel in the above image looks more like a raised vein rather than a hollowed out channel, try looking at the half-circle depression on the left-hand side of the image, about a third of the way up. The bright features on the upper half streak down toward the bottom of the bowl. Once you focus on this for a while, your brain figures out that the channel must be depressed as well. Now that you can see that the channel cuts into the surface, click on the image for a closer look at the bottom of the channel. Mega-ripples about 82 yards apart line the channel floor as it curves through the region. This pattern shows that even this relatively small channel, which varies from about one-third to a half of a mile in width, funnels the wind down its curving length, creating perpendicular piles of waving texture on the channel's floor. East of the channel, smooth, dark-toned mesas are visible, providing a scant reminder that they were once continuous across the region. As these layers have eroded, they've produced a wide array of textures, from smooth surfaces, to knobby terrains, to the unusual curved, lobe-like patterns seen in the upper right of the image.
Noctis Labyrinthus/Valles Ma …
PIA03813
Sol (our sun)
Thermal Emission Imaging Sys …
Title Noctis Labyrinthus/Valles Marineris transition
Original Caption Released with Image (Released 27 May 2002) The Science The transition zone between maze-like troughs of Noctis Labyrinthus and the main Valles Marineris canyon system are shown in this THEMIS visible camera image. This huge system of troughs near the equator of Mars was most likely created by tectonic forces which pulled apart the crust. In the top third of the image, on the western side of the northernmost trough, a buildup of relatively bright material on the plateau has led to an overflow into the trough. Most of the bottom of this trough is covered by sediment deposited from the plateau above. On the right-hand side of this same trough, on the southern wall, there is a thin streak of darker material that also seems to originate from the plateau above. This is most likely a gully formation. This feature could also be a dust avalanche, but because no other similar features are seen, this is unlikely. Other dark material deposited by some unknown process can also be seen all around the easternmost ridge in the trough. Near the bottom of the canyon, layers from the center ridges and the canyon wall can be matched, indicating that the ridges are made of the same material as the wall. Near the bottom of the image, there is yet another depression. This trough is filled with sediment deposited from erosion of the trough wall and possibly from the plateau above. All around the walls of this trough a layer of rocky material can be also be seen. It appears that the areas directly below the rocky ledges are "shielded" from landslide material from above. Finally, in the northwestern wall of this trough, there is an irregular pattern of very bright material not seen anywhere else in the image. Identifying similar formations in other THEMIS visible camera images could provide some context for its occurrence and help us understand how it was formed. The Story Tectonic forces wrenched apart the crust on Mars long ago, forming deep troughs at the Martian equator like the ones seen here. They occur in a transition zone between the maze-like region of Noctis Labyrinthus and the deep canyon system of Valles Marineris, the largest and "grandest" canyon in the solar system. These cracks in the crust can give geologists a good idea of what has happened over the course of the planet's history. Find out a little yourself by taking a closer look at the western side of the trough in the top third of the image. Can you see how the bright sediment from the plateau above has been whisked over the side, overflowing and building up on the floor below? Follow the south wall of this same trough, and you'll come across a dark streak running down (toward the right side of the image). One possibility is that it could be a dust avalanche, but if that were so, you'd think it would have occurred much more often, in more places than just that one spot. Since it didn't, scientists believe it probably isn't a dust avalanche, but could be a gully instead. There's also some more dark material deposited, all around the easternmost ridge in the trough as well. No one is quite sure how it formed there or exactly what it's made of. At the least, what geologists can tell is that the ridges in the trough are made of the same material as the canyon walls, since the layers in each of them match. Finding similarities like these can help piece together the story of Martian geology here. When scientists study THEMIS images, however, they are also on the lookout for anything that looks unusual. Try studying the dark depression that carves out the bottom of this image. It too is filled soft-looking sediments, probably deposited from erosion of the trough wall and possibly from the plateau above. Rocky outcrops all around the walls of this trough shield the areas directly below them from landslides from above. But all that seems pretty regular. Do you see anything that stands out? How about the odd pattern of brighter material that seems almost pasted on the northwestern wall of the trough like dried up glue? This material isn't found elsewhere in this image. Sights like this pose a geological mystery, and one of the only ways to solve it is to seek more clues. Do similar formations occur elsewhere on Mars? Stay tuned with THEMIS researchers, because they'll be looking, trying to understand how and how often such features form.
Noctis Labyrinthus/Valles Ma …
PIA03813
Sol (our sun)
Thermal Emission Imaging Sys …
Title Noctis Labyrinthus/Valles Marineris transition
Original Caption Released with Image (Released 27 May 2002) The Science The transition zone between maze-like troughs of Noctis Labyrinthus and the main Valles Marineris canyon system are shown in this THEMIS visible camera image. This huge system of troughs near the equator of Mars was most likely created by tectonic forces which pulled apart the crust. In the top third of the image, on the western side of the northernmost trough, a buildup of relatively bright material on the plateau has led to an overflow into the trough. Most of the bottom of this trough is covered by sediment deposited from the plateau above. On the right-hand side of this same trough, on the southern wall, there is a thin streak of darker material that also seems to originate from the plateau above. This is most likely a gully formation. This feature could also be a dust avalanche, but because no other similar features are seen, this is unlikely. Other dark material deposited by some unknown process can also be seen all around the easternmost ridge in the trough. Near the bottom of the canyon, layers from the center ridges and the canyon wall can be matched, indicating that the ridges are made of the same material as the wall. Near the bottom of the image, there is yet another depression. This trough is filled with sediment deposited from erosion of the trough wall and possibly from the plateau above. All around the walls of this trough a layer of rocky material can be also be seen. It appears that the areas directly below the rocky ledges are "shielded" from landslide material from above. Finally, in the northwestern wall of this trough, there is an irregular pattern of very bright material not seen anywhere else in the image. Identifying similar formations in other THEMIS visible camera images could provide some context for its occurrence and help us understand how it was formed. The Story Tectonic forces wrenched apart the crust on Mars long ago, forming deep troughs at the Martian equator like the ones seen here. They occur in a transition zone between the maze-like region of Noctis Labyrinthus and the deep canyon system of Valles Marineris, the largest and "grandest" canyon in the solar system. These cracks in the crust can give geologists a good idea of what has happened over the course of the planet's history. Find out a little yourself by taking a closer look at the western side of the trough in the top third of the image. Can you see how the bright sediment from the plateau above has been whisked over the side, overflowing and building up on the floor below? Follow the south wall of this same trough, and you'll come across a dark streak running down (toward the right side of the image). One possibility is that it could be a dust avalanche, but if that were so, you'd think it would have occurred much more often, in more places than just that one spot. Since it didn't, scientists believe it probably isn't a dust avalanche, but could be a gully instead. There's also some more dark material deposited, all around the easternmost ridge in the trough as well. No one is quite sure how it formed there or exactly what it's made of. At the least, what geologists can tell is that the ridges in the trough are made of the same material as the canyon walls, since the layers in each of them match. Finding similarities like these can help piece together the story of Martian geology here. When scientists study THEMIS images, however, they are also on the lookout for anything that looks unusual. Try studying the dark depression that carves out the bottom of this image. It too is filled soft-looking sediments, probably deposited from erosion of the trough wall and possibly from the plateau above. Rocky outcrops all around the walls of this trough shield the areas directly below them from landslides from above. But all that seems pretty regular. Do you see anything that stands out? How about the odd pattern of brighter material that seems almost pasted on the northwestern wall of the trough like dried up glue? This material isn't found elsewhere in this image. Sights like this pose a geological mystery, and one of the only ways to solve it is to seek more clues. Do similar formations occur elsewhere on Mars? Stay tuned with THEMIS researchers, because they'll be looking, trying to understand how and how often such features form.
Streamlined Islands in Ares …
PIA03825
Sol (our sun)
Thermal Emission Imaging Sys …
Title Streamlined Islands in Ares Valles
Original Caption Released with Image (Released 10 June 2002) The Science Although liquid water is not stable on the surface of Mars today, there is substantial geologic evidence that large quantities of water once flowed across the surface in the distant past. Streamlined islands, shown here, are one piece of evidence for this ancient water. The tremendous force of moving water, possibly from a catastrophic flood, carved these teardrop-shaped islands within a much larger channel called Ares Valles. The orientation of the islands can be used as an indicator of the direction the water flowed. The islands have a blunt end that is usually associated with an obstacle, commonly an impact crater. The crater is resistant to erosion and creates a geologic barrier around which the water must flow. As the water flows past the obstacle, its erosive power is directed outward, leaving the area in the lee of the obstacle relatively uneroded. However, some scientists have also argued that the area in the lee of the obstacle might be a depositional zone, where material is dropped out of the water as it briefly slows. The ridges observed on the high-standing terrain in the leeward parts of the islands may be benches carved into the rock that mark the height of the water at various times during the flood, or they might be indicative of layering in the leeward rock. As the water makes its way downstream, the interference of the water flow by the obstacle is reduced, and the water that was diverted around the obstacle rejoins itself at the narrow end of the island. Therefore, the direction of the water flow is parallel to the orientation of the island, and the narrow end of the island points downstream. In addition to the streamlined islands, the channel floor exhibits fluting that is also suggestive of flowing water. The flutes (also known as longitudinal grooves) are also parallel to the direction of flow, indicating that the water flow was turbulent and probably quite fast, which is consistent with the hypothesized catastrophic floods that came through Ares Valles. The Story In symbolism only, these guppy-shaped islands and current-like flutes of land beside them may conjure up a mental image of a flowing Martian river. This picture would only be half-right. Scientifically, no fish ever swam this channel, but these landforms do reveal that catastrophic floods of rushing water probably patterned the land in just this way. Geologists who study flood areas believe that a tremendous force of moving water probably carved both the islands and the small, parallel, "current-like" ridges around them. The blunt end of the islands (the "heads" of the "fish") are probably ancient impact craters that posed obstacles to the water as it rushed down the channel in torrents. Because a crater is resistant to erosion, it creates a geologic barrier around which the water must flow. As the water makes its way downstream, the crater's interference with the water flow is reduced, so the water that was diverted around, the obstacle rejoins at the narrow end of the island (the "tail" of the "fish"). Therefore, from this information, you can tell that the water flowed from the southeast to the northwest. As a rule of thumb for the future, you can say that the narrow end of the island points downstream. The result may be the island behind the crater, but geologists disagree about the exact process by which the island forms. Some scientists argue that the erosive power of the water is directed outward, leaving the area behind, or in the lee of, the obstacle relatively untouched. Other scientists argue that the water slows when it encounters the crater obstacle, and small particles of sand and "dirt" drop out of the water and are deposited in the lee. There's another small associated uncertainty too. Look closely at the edges of the islands and notice how the land is terraced. These ledges might mark the height of the water at various times during the flood . . . or they might be an indication that layering occurred. It all depends on your hypothesis. Like the streamlined islands, the current-like flutes are parallel to the direction of flow, indicating that the water flow was turbulent and probably quite fast, which is consistent with the hypothesis that catastrophic floods broke forth in this region, known as Ares Vallis. Ares Vallis is the region where Pathfinder landed to help understand the possible history of water on Mars. Geologists want to understand not only if there was a catastrophic flood, but why it happened. Both orbiters and landers can add to the information on hand, but some Earth examples might provide clues as well. On our planet, some glacial valleys have had major catastrophic floods that were caused by the sudden outburst and drainage of glacial lakes. The Channeled Scabland in Washington state is great Earthly example of a place where the sudden failure of a glacier ice dam spewed out water, leaving a system of large, dry channels with flutes similar to the ones seen in this image. Did something similar happen to cause this outburst on Mars? Hopefully, future studies of THEMIS and other images will help us understand the answer.
Streamlined Islands in Ares …
PIA03825
Sol (our sun)
Thermal Emission Imaging Sys …
Title Streamlined Islands in Ares Valles
Original Caption Released with Image (Released 10 June 2002) The Science Although liquid water is not stable on the surface of Mars today, there is substantial geologic evidence that large quantities of water once flowed across the surface in the distant past. Streamlined islands, shown here, are one piece of evidence for this ancient water. The tremendous force of moving water, possibly from a catastrophic flood, carved these teardrop-shaped islands within a much larger channel called Ares Valles. The orientation of the islands can be used as an indicator of the direction the water flowed. The islands have a blunt end that is usually associated with an obstacle, commonly an impact crater. The crater is resistant to erosion and creates a geologic barrier around which the water must flow. As the water flows past the obstacle, its erosive power is directed outward, leaving the area in the lee of the obstacle relatively uneroded. However, some scientists have also argued that the area in the lee of the obstacle might be a depositional zone, where material is dropped out of the water as it briefly slows. The ridges observed on the high-standing terrain in the leeward parts of the islands may be benches carved into the rock that mark the height of the water at various times during the flood, or they might be indicative of layering in the leeward rock. As the water makes its way downstream, the interference of the water flow by the obstacle is reduced, and the water that was diverted around the obstacle rejoins itself at the narrow end of the island. Therefore, the direction of the water flow is parallel to the orientation of the island, and the narrow end of the island points downstream. In addition to the streamlined islands, the channel floor exhibits fluting that is also suggestive of flowing water. The flutes (also known as longitudinal grooves) are also parallel to the direction of flow, indicating that the water flow was turbulent and probably quite fast, which is consistent with the hypothesized catastrophic floods that came through Ares Valles. The Story In symbolism only, these guppy-shaped islands and current-like flutes of land beside them may conjure up a mental image of a flowing Martian river. This picture would only be half-right. Scientifically, no fish ever swam this channel, but these landforms do reveal that catastrophic floods of rushing water probably patterned the land in just this way. Geologists who study flood areas believe that a tremendous force of moving water probably carved both the islands and the small, parallel, "current-like" ridges around them. The blunt end of the islands (the "heads" of the "fish") are probably ancient impact craters that posed obstacles to the water as it rushed down the channel in torrents. Because a crater is resistant to erosion, it creates a geologic barrier around which the water must flow. As the water makes its way downstream, the crater's interference with the water flow is reduced, so the water that was diverted around, the obstacle rejoins at the narrow end of the island (the "tail" of the "fish"). Therefore, from this information, you can tell that the water flowed from the southeast to the northwest. As a rule of thumb for the future, you can say that the narrow end of the island points downstream. The result may be the island behind the crater, but geologists disagree about the exact process by which the island forms. Some scientists argue that the erosive power of the water is directed outward, leaving the area behind, or in the lee of, the obstacle relatively untouched. Other scientists argue that the water slows when it encounters the crater obstacle, and small particles of sand and "dirt" drop out of the water and are deposited in the lee. There's another small associated uncertainty too. Look closely at the edges of the islands and notice how the land is terraced. These ledges might mark the height of the water at various times during the flood . . . or they might be an indication that layering occurred. It all depends on your hypothesis. Like the streamlined islands, the current-like flutes are parallel to the direction of flow, indicating that the water flow was turbulent and probably quite fast, which is consistent with the hypothesis that catastrophic floods broke forth in this region, known as Ares Vallis. Ares Vallis is the region where Pathfinder landed to help understand the possible history of water on Mars. Geologists want to understand not only if there was a catastrophic flood, but why it happened. Both orbiters and landers can add to the information on hand, but some Earth examples might provide clues as well. On our planet, some glacial valleys have had major catastrophic floods that were caused by the sudden outburst and drainage of glacial lakes. The Channeled Scabland in Washington state is great Earthly example of a place where the sudden failure of a glacier ice dam spewed out water, leaving a system of large, dry channels with flutes similar to the ones seen in this image. Did something similar happen to cause this outburst on Mars? Hopefully, future studies of THEMIS and other images will help us understand the answer.
Kasei Valles
PIA03792
Sol (our sun)
Thermal Emission Imaging Sys …
Title Kasei Valles
Original Caption Released with Image (Released 9 May 2002) Kasei Valles (Kasei is the Japanese word for Mars) is one of the largest outflow channels on Mars. Kasei Valles stretches some 2,000 km across the face of Mars and empties into the Chryse basin. This THEMIS image is of the northern branch of Kasei Valles and shows the channel floor and northern channel wall. The plateau surface located at the top of this image is more heavily cratered than the channel floor which indicates that the plateau is older than the channel floor. The wall of the plateau has spur and gully topography present. The floor of the channel has evidence of fluvial scour including a smaller inner channel. These features were probably carved out during waning stage flow. The probable causes of Martian floods are massive releases of subsurface water/ice due to possible subsurface volcanic activity. Martian outflow channels begin at point sources (chaotic terrain and box canyons) and then flow unconfined into a basin region.
Kasei Valles
PIA03792
Sol (our sun)
Thermal Emission Imaging Sys …
Title Kasei Valles
Original Caption Released with Image (Released 9 May 2002) Kasei Valles (Kasei is the Japanese word for Mars) is one of the largest outflow channels on Mars. Kasei Valles stretches some 2,000 km across the face of Mars and empties into the Chryse basin. This THEMIS image is of the northern branch of Kasei Valles and shows the channel floor and northern channel wall. The plateau surface located at the top of this image is more heavily cratered than the channel floor which indicates that the plateau is older than the channel floor. The wall of the plateau has spur and gully topography present. The floor of the channel has evidence of fluvial scour including a smaller inner channel. These features were probably carved out during waning stage flow. The probable causes of Martian floods are massive releases of subsurface water/ice due to possible subsurface volcanic activity. Martian outflow channels begin at point sources (chaotic terrain and box canyons) and then flow unconfined into a basin region.
Hebrus Valles
PIA03820
Sol (our sun)
Thermal Emission Imaging Sys …
Title Hebrus Valles
Original Caption Released with Image (Released 3 June 2002) The Science Hebrus Valles is located in the Elysium Planitia region of the northern lowlands of the planet. This image shows three sinuous tributaries of the channel system which carved up the surrounding plains. These individual tributaries are up to 3 km wide and have up to three terraces visible along their margins. These terraces may indicate separate flood events or may be the result of one flood plucking away at channel wall materials with varying strengths of resistance. It is not clear if these are separate rock layers or just the erosion of one type of material from rising and falling water levels. A streamlined island is visible in the lower third of the image. This feature indicates that flow was from the lower right to upper left in this region (the tail of the island points downstream). In places ripples, interpreted to be dunes, can also be seen along the interface of the channel floor with the walls. Smaller, fainter channels can also be seen scouring the plains, especially in the lower portion of this image. Other features of note in this image are the various inselbergs (isolated hills) located primarily in the upper portion of the image. The inselbergs are surrounded with aprons of material that was probably shed off of the hills by various processes of erosion. The Story Mars was once the scene of some major floods that rushed out upon the land, carving all kinds of channels. These signs of ancient flooding have always been exciting to scientists who want to understand the history of water on the planet. Water is important to understanding the climate and geological history of Mars, as well as whether life could ever have developed there. While we can't tell much about the life question from pictures like this one, it does give some insights into the great flood itself. You can see three tributaries of a channel system that are up to two miles wide or so. The really interesting thing is that you can see terraces of land that step down from the sides of the tributaries. How did they form? Was there one massive flood that swept through, eroding materials with varying strengths of resistance? Or was it several, separate floods? And what could the answer tell us about the types of rocks and materials in this region? No one knows if these are separate rock layers or just one type of material that has eroded from rising and falling water levels. While these questions will continue to intrigue geologists, one thing that they can tell for sure is the direction the water flowed. Can you find the tear-drop shaped island in the now dry channel? On Earth, we see these islands created in rivers all the time. The "tail" of the island (the point on the teardrop) points downstream, so that means the flood rushed down the channel from the lower right to the upper left. Since the flood, there is some rippling evidence on the channel floor that dunes may have formed. Smaller, fainter channels can also be seen, scouring the plains, especially in the lower portion of this image. Other interesting features in this image are the various inselbergs (isolated hills) located primarily in the upper portion of the image. The inselbergs are surrounded with aprons of material that was probably shed off of the hills by various processes of erosion.
Hebrus Valles
PIA03820
Sol (our sun)
Thermal Emission Imaging Sys …
Title Hebrus Valles
Original Caption Released with Image (Released 3 June 2002) The Science Hebrus Valles is located in the Elysium Planitia region of the northern lowlands of the planet. This image shows three sinuous tributaries of the channel system which carved up the surrounding plains. These individual tributaries are up to 3 km wide and have up to three terraces visible along their margins. These terraces may indicate separate flood events or may be the result of one flood plucking away at channel wall materials with varying strengths of resistance. It is not clear if these are separate rock layers or just the erosion of one type of material from rising and falling water levels. A streamlined island is visible in the lower third of the image. This feature indicates that flow was from the lower right to upper left in this region (the tail of the island points downstream). In places ripples, interpreted to be dunes, can also be seen along the interface of the channel floor with the walls. Smaller, fainter channels can also be seen scouring the plains, especially in the lower portion of this image. Other features of note in this image are the various inselbergs (isolated hills) located primarily in the upper portion of the image. The inselbergs are surrounded with aprons of material that was probably shed off of the hills by various processes of erosion. The Story Mars was once the scene of some major floods that rushed out upon the land, carving all kinds of channels. These signs of ancient flooding have always been exciting to scientists who want to understand the history of water on the planet. Water is important to understanding the climate and geological history of Mars, as well as whether life could ever have developed there. While we can't tell much about the life question from pictures like this one, it does give some insights into the great flood itself. You can see three tributaries of a channel system that are up to two miles wide or so. The really interesting thing is that you can see terraces of land that step down from the sides of the tributaries. How did they form? Was there one massive flood that swept through, eroding materials with varying strengths of resistance? Or was it several, separate floods? And what could the answer tell us about the types of rocks and materials in this region? No one knows if these are separate rock layers or just one type of material that has eroded from rising and falling water levels. While these questions will continue to intrigue geologists, one thing that they can tell for sure is the direction the water flowed. Can you find the tear-drop shaped island in the now dry channel? On Earth, we see these islands created in rivers all the time. The "tail" of the island (the point on the teardrop) points downstream, so that means the flood rushed down the channel from the lower right to the upper left. Since the flood, there is some rippling evidence on the channel floor that dunes may have formed. Smaller, fainter channels can also be seen, scouring the plains, especially in the lower portion of this image. Other interesting features in this image are the various inselbergs (isolated hills) located primarily in the upper portion of the image. The inselbergs are surrounded with aprons of material that was probably shed off of the hills by various processes of erosion.
Light Layered Deposits in Va …
PIA09397
Sol (our sun)
HiRISE
Title Light Layered Deposits in Valles Marineris
Original Caption Released with Image This image shows bright layered deposits near the junction of Coprates Chasma and Melas Chasma, part of Valles Marineris. The outcrop shown here is in a wide alcove in the northern wall and forms a broad mound several kilometers wide, dark, wind-blown material covers it in places. Similar light-toned rock occurs in many places in Valles Marineris. An important question is when these materials formed: were they deposited within the troughs after they opened and then eroded, or are they remnants of the wall rock? Analysis of the orientation of the layers using HiRISE images may help scientists answer this question. There are no fresh impact craters preserved on the outcrop surface, suggesting that the layered deposits are being eroded rapidly enough to erase the craters. In many places, the light rocks have regular fractures called joints. Joints are common in rocks on Earth, and HiRISE images show them in many places on Mars as well. These can provide information about the forces which have affected the rock since it formed, which helps unravel the geologic history of this outcrop. Image PSP_001456_1695 [ http://hiroc.lpl.arizona.edu/images/PSP/PSP_001456_1695/ ] was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on November 17, 2006. The complete image is centered at -10.2 degrees latitude, 291.2 degrees East longitude. The range to the target site was 258.4 km (161.5 miles). At this distance the image scale is 25.9 cm/pixel (with 1 x 1 binning) so objects ~78 cm across are resolved. The image shown here has been map-projected to 25 cm/pixel and north is up. The image was taken at a local Mars time of 3:33 PM and the scene is illuminated from the west with a solar incidence angle of 59 degrees, thus, the sun was about 31 degrees above the horizon. At a solar longitude of 136.9 degrees, the season on Mars is Northern Summer. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Flows in Athabasca Valles So …
PIA09400
Sol (our sun)
HiRISE
Title Flows in Athabasca Valles Source Region
Original Caption Released with Image Click on image for larger version Thin flows cover the plains just north of the source region for the Athabasca Valles channel system. The flows are mostly confined by a scarp (cliff) in the northwest corner of the image. The more heavily cratered terrain above the scarp is part of a tectonic ridge known as a wrinkle ridge. A few flows can be seen atop the wrinkle ridge, but they are not as ubiquitous as those on the plains below. The flows on the plains frequently intersect, with younger ones cutting across older ones. The prominent dark swathes along their edges have particularly rough textures. The darker shade is due to thousands of shadows cast by small bumps on the surface, which HiRISE is able to resolve. Dozens of bright, narrow rifts (cracks) zigzag across the flows. They appear bright because they are filled with light-toned, windblown material. Wind-sculpted knobs and ridges of similar light-toned material are scattered throughout the imaged area. The orientations of the ridges indicate that the winds primarily blow from the southeast. Several impact craters are captured in this image, the largest being about 50 meters (160 feet) in diameter. Many bear the distinctive bright rays characteristic of secondary craters associated with the larger impact crater, Zunil. Some craters penetrated the surface of the flows, and the boulders strewn around them suggest that the material they excavated was rocky. Image PSP_001408_1900 [ http://hiroc.lpl.arizona.edu/images/PSP/PSP_001408_1900/ ] was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on November 14, 2006. The complete image is centered at 10.0 degrees latitude, 158.0 degrees East longitude. The range to the target site was 274.3 km (171.4 miles). At this distance the image scale is 27.4 cm/pixel (with 1 x 1 binning) so objects ~82 cm across are resolved. The image shown here [below] has been map-projected to 25 cm/pixel and north is up. The image was taken at a local Mars time of 3:29 PM and the scene is illuminated from the west with a solar incidence angle of 51 degrees, thus the sun was about 39 degrees above the horizon. At a solar longitude of 135.1 degrees, the season on Mars is Northern Summer. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Flows in Athabasca Valles So …
PIA09400
Sol (our sun)
HiRISE
Title Flows in Athabasca Valles Source Region
Original Caption Released with Image Click on image for larger version Thin flows cover the plains just north of the source region for the Athabasca Valles channel system. The flows are mostly confined by a scarp (cliff) in the northwest corner of the image. The more heavily cratered terrain above the scarp is part of a tectonic ridge known as a wrinkle ridge. A few flows can be seen atop the wrinkle ridge, but they are not as ubiquitous as those on the plains below. The flows on the plains frequently intersect, with younger ones cutting across older ones. The prominent dark swathes along their edges have particularly rough textures. The darker shade is due to thousands of shadows cast by small bumps on the surface, which HiRISE is able to resolve. Dozens of bright, narrow rifts (cracks) zigzag across the flows. They appear bright because they are filled with light-toned, windblown material. Wind-sculpted knobs and ridges of similar light-toned material are scattered throughout the imaged area. The orientations of the ridges indicate that the winds primarily blow from the southeast. Several impact craters are captured in this image, the largest being about 50 meters (160 feet) in diameter. Many bear the distinctive bright rays characteristic of secondary craters associated with the larger impact crater, Zunil. Some craters penetrated the surface of the flows, and the boulders strewn around them suggest that the material they excavated was rocky. Image PSP_001408_1900 [ http://hiroc.lpl.arizona.edu/images/PSP/PSP_001408_1900/ ] was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on November 14, 2006. The complete image is centered at 10.0 degrees latitude, 158.0 degrees East longitude. The range to the target site was 274.3 km (171.4 miles). At this distance the image scale is 27.4 cm/pixel (with 1 x 1 binning) so objects ~82 cm across are resolved. The image shown here [below] has been map-projected to 25 cm/pixel and north is up. The image was taken at a local Mars time of 3:29 PM and the scene is illuminated from the west with a solar incidence angle of 51 degrees, thus the sun was about 39 degrees above the horizon. At a solar longitude of 135.1 degrees, the season on Mars is Northern Summer. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Valles Marineris Wall Rock
PIA09391
Sol (our sun)
HiRISE
Title Valles Marineris Wall Rock
Original Caption Released with Image This HiRISE image captures a small part of the northern wall of Valles Marineris, the largest canyon in the solar system. The reason this part of Mars' crust was pulled apart is not known with certainty, so observations like this are part of a campaign to understand the tectonics of Mars. In addition, the canyon provides a view deep into the crust of Mars. This HiRISE image captures 9500 meter (31,000 feet) of vertical relief. A sequence of thin layers can be seen in the upper roughly 1000 m (3000 feet) of the valley wall. Since Valles Marineris cuts into the side of the Tharsis Volcanic Rise, it is likely that these layers are lava flows. Below this, layers are not so regular. This lower section probably exposes rocks that have been intensely disrupted by ancient impact craters, but could also include solidified bodies of magma. Image PSP_001337_1675 [ http://hiroc.lpl.arizona.edu/images/PSP/PSP_001337_1675/ ] was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on November 8, 2006. The complete image is centered at -12.2 degrees latitude, 297.6 degrees East longitude. The range to the target site was 257.0 km (160.6 miles). At this distance the image scale ranges from 51.4 cm/pixel (with 2 x 2 binning) to 102.8 cm/pixel (with 4 x 4 binning). The image shown here has been map-projected to 50 cm/pixel and north is up. The image was taken at a local Mars time of 3:32 PM and the scene is illuminated from the west with a solar incidence angle of 61 degrees, thus the sun was about 29 degrees above the horizon. At a solar longitude of 132.4 degrees, the season on Mars is Northern Summer. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Floor of Kasei Valles
PIA09396
Sol (our sun)
HiRISE
Title Floor of Kasei Valles
Original Caption Released with Image This HiRISE image shows a wonderfully complex surface on the floor of this ancient flood-carved canyon. In this area, the water flowed from the west to the east. However, the floor does not show the kinds of landforms scientist expect from flood erosion. Instead, the floor of the valley has been covered, sometime after the flood, by some kind of flow with giant ridged plates. Some of the plates are more than a kilometer (0.6 miles) across. The ridges appear to have formed when the solid crust on the flow was crumpled during flow. The plates are pieces of the crust that had rafted apart. Very large lava flows can produce this kind of surface, but ice and frozen mud are also capable of forming similar features. Image PSP_001456_2010 [ http://hiroc.lpl.arizona.edu/images/PSP/PSP_001456_2010/ ] was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on November 17, 2006. The complete image is centered at 20.7 degrees latitude, 287.2 degrees East longitude. The range to the target site was 280.3 km (175.2 miles). At this distance the image scale ranges from 28.0 cm/pixel (with 1 x 1 binning) to 56.1 cm/pixel (with 2 x 2 binning). The image shown here has been map-projected to 25 cm/pixel and north is up. The image was taken at a local Mars time of 3:27 PM and the scene is illuminated from the west with a solar incidence angle of 49 degrees, thus the sun was about 41 degrees above the horizon. At a solar longitude of 136.9 degrees, the season on Mars is Northern Summer. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Exposed Layers in Central Va …
PIA09964
Sol (our sun)
HiRISE
Title Exposed Layers in Central Valles Marineris
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_004858_1670 [ http://hirise.lpl.arizona.edu/PSP_004858_1670 ]) shows a landslide scarp on the northern wall of central Valles Marineris, a large canyon system equivalent in length from California to New York. The landslide has exposed a fresh wall of the canyon so that individual layers of rock can be seen. The texture of these layers suggests that some of the darker rock layers are more resistant to erosion than the lighter layers. The variation in brightness and friability of the different layers suggests compositional differences. These layers may have a volcanic origin, having been deposited as ash layers, or a sedimentary origin, either being deposited by water or blown by the wind (aeolian). This image is a little hazy because this image was taken in August 2007, when the large dust storm covered the surface of Mars and filled the atmosphere with fine dust particles. The extra dust in the atmosphere reflects more light into the camera. Observation Toolbox Acquisition date: 8 August 2007 Local Mars time: 2:31 PM Degrees latitude (centered): -12.8° Degrees longitude (East): 301.1° Range to target site: 259.8 km (162.4 miles) Original image scale range: 26.0 cm/pixel (with 1 x 1 binning) so objects ~78 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.6° Phase angle: 32.0° Solar incidence angle: 37°, with the Sun about 53 ° above the horizon Solar longitude: 292.6°, Northern Winter NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Exposed Layers in Central Va …
PIA09964
Sol (our sun)
HiRISE
Title Exposed Layers in Central Valles Marineris
Original Caption Released with Image Click on image for larger version This HiRISE image (PSP_004858_1670 [ http://hirise.lpl.arizona.edu/PSP_004858_1670 ]) shows a landslide scarp on the northern wall of central Valles Marineris, a large canyon system equivalent in length from California to New York. The landslide has exposed a fresh wall of the canyon so that individual layers of rock can be seen. The texture of these layers suggests that some of the darker rock layers are more resistant to erosion than the lighter layers. The variation in brightness and friability of the different layers suggests compositional differences. These layers may have a volcanic origin, having been deposited as ash layers, or a sedimentary origin, either being deposited by water or blown by the wind (aeolian). This image is a little hazy because this image was taken in August 2007, when the large dust storm covered the surface of Mars and filled the atmosphere with fine dust particles. The extra dust in the atmosphere reflects more light into the camera. Observation Toolbox Acquisition date: 8 August 2007 Local Mars time: 2:31 PM Degrees latitude (centered): -12.8° Degrees longitude (East): 301.1° Range to target site: 259.8 km (162.4 miles) Original image scale range: 26.0 cm/pixel (with 1 x 1 binning) so objects ~78 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.6° Phase angle: 32.0° Solar incidence angle: 37°, with the Sun about 53 ° above the horizon Solar longitude: 292.6°, Northern Winter NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.
Valles Marineris Mosaic
PIA06926
Sol (our sun)
Thermal Emission Spectromete …
Title Valles Marineris Mosaic
Original Caption Released with Image The Odyssey spacecraft has taken some great pictures of Valles Marineris, the largest canyon in the solar system. If this canyon were on Earth, it would stretch from New York to Los Angeles. For the next several weeks, the Image of the Day will tour some of the canyons that make up this vast system. We will start with Ius Chasma in the west, and end with Coprates Chasma to the east. For more information on Vallis Marineris, please see http://mars.jpl.nasa.gov/mep/science/vm.html [ http://mars.jpl.nasa.gov/mep/science/vm.html ]. This mosaic of infrared images shows the full length of Valles Marineris. For highest resolution TIF image please visit http://themis.la.asu.edu/zoom-20041008A.html [ http://themis.la.asu.edu/zoom-20041008A.html ]. 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.
Western Candor Chasma, Valle …
PIA01458
Sol (our sun)
Mars Orbiter Camera
Title Western Candor Chasma, Valles Marineris
Original Caption Released with Image Astronautics, from facilities in Pasadena, CA and Denver, CO., One of the most striking discoveries of the Mars Global Surveyor mission has been the identification of thousands of meters/feet of layers within the wall rock of the enormous martian canyon system, Valles Marineris. Valles Marineris was first observed in 1972 by the Mariner 9 spacecraft, from which the troughs get their name: Valles--valleys, Marineris--Mariner. Some hints of layering in both the canyon walls and within some deposits on the canyon floors were seen in Mariner 9 and Viking orbiter images from the 1970s. The Mars Orbiter Camera on board Mars Global Surveyor has been examining these layers at much higher resolution than was available previously. MOC images led to the realization that there are layers in the walls that go down to great depths. An example of the wall rock layers can be seen in MOC image 8403, shown above (C). MOC images also reveal amazing layered outcrops on the floors of some of the Valles Marineris canyons. Particularly noteworthy is MOC image 23304 (D, above), which shows extensive, horizontally-bedded layers exposed in buttes and mesas on the floor of western Candor Chasma. These layered rocks might be the same material as is exposed in the chasm walls (as in 8403--C, above), or they might be rocks that formed by deposition (from water, wind, and/or volcanism) long after Candor Chasma opened up. In addition to layered materials in the walls and on the floors of the Valles Marineris system, MOC images are helping to refine our classification of geologic features that occur within the canyons. For example, MOC image 25205 (E, above), shows the southern tip of a massive, tongue-shaped massif (a mountainous ridge) that was previously identified as a layered deposit. However, this MOC image does not show layering. The material has been sculpted by wind and mass-wasting--downslope movement of debris--but no obvious layers were exposed by these processes. Valles Marineris a fascinating region on Mars that holds much potential to reveal information about the early history and evolution of the red planet. The MOC Science Team is continuing to examine the wealth of new data and planning for new Valles Marineris targets once the Mapping Phase of the Mars Global Surveyor mission commences in March 1999. This image: Layers in western Candor Chasma northern wall. MOC image 8403 subframe shown at full resolution of 4.6 meters (15 feet) per pixel. The image shows an area approximately 2.4 by 2.5 kilometers (1.5 x 1.6 miles). North is up, illumination is from the left. Image 8403 was obtained during Mars Global Surveyor's 84th orbit at 10:12 p.m. (PST) on January 6, 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's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin
Multiple Channels in Warrego …
PIA05662
Sol (our sun)
Thermal Emission Imaging Sys …
Title Multiple Channels in Warrego Valles
Original Caption Released with Image Released 26 March 2004 The 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. The image shows an area in the Warrego Valles region. It was collected July 6, 2003 during northern summer season. The local time is 5pm. The image shows multiple channels dissecting the terrain. With this image, the 448th, the THEMIS Image of the Day completes its second (Earth) year. (The first image, of Nirgal Vallis [ http://photojournal.jpl.nasa.gov/catalog/PIA03756 ], was released on 27 March 2002.) On behalf of the THEMIS team, we'd like to thank you for your continued interest and we hope you continue to come back through our third year and beyond. Image information: VIS instrument. Latitude -42.3, Longitude 267.5 East (92.5 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.
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