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Mars of Jet Propulsion Laboratory (JPL) and Arizona from 2007
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Depth-to-Ice Map of a Southe
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| title |
Depth-to-Ice Map of a Southern Mars Site Near Melea Planum |
| Description |
Color coding in this map of a far-southern site on Mars indicates the change in nighttime ground-surface temperature between summer and fall. This site, like most of high-latitude Mars, has water ice mixed with soil near the surface. The ice is probably in a rock-hard frozen layer beneath a few centimeters or inches of looser, dry soil. The amount of temperature change at the surface likely corresponds to how close to the surface the icy material lies. The dense, icy layer retains heat better than the looser soil above it, so where the icy layer is closer to the surface, the surface temperature changes more slowly than where the icy layer is buried deeper. On the map, areas of the surface that cooled more slowly between summer and autumn (interpreted as having the ice closer to the surface) are coded blue and green. Areas that cooled more quickly (interpreted as having more distance to the ice) are coded red and yellow. The depth to the top of the icy layer estimated from these observations suggests that in some areas, but not others, water is being exchanged by diffusion between atmospheric water vapor and subsurface water ice. Differences in what type of material lies above the ice appear to affect the depth to the ice. The area in this image with the greatest seasonal change in surface temperature corresponds to an area of sand dunes. This map and its interpretation are in a May 3, 2007, report in the journal Nature by Joshua Bandfield of Arizona State University, Tempe. The Thermal Emission Imaging System camera on NASA's Mars Odyssey orbiter collected the data presented in the map. The site is centered near 67 degrees south latitude, 36.5 degrees east longitude, near a plain named Melea Planum. This site is within the portion of the planet where, in 2002, the Gamma Ray Spectrometer suite of instruments on Mars Odyssey found evidence for water ice lying just below the surface. The information from the Gamma Ray Spectrometer is averaged over patches of ground hundreds of kilometers or miles wide. The information from the Thermal Emission Imaging System allows more than 100-fold higher resolution in mapping variations in the depth to ice. The Thermal Emission Imaging System observed the site in infrared wavelengths during night time, providing surface-temperature information. It did so once on Dec. 27, 2005, during late summer in Mars' southern hemisphere, and again on Jan. 22, 2006, the first day of autumn there. The colors on this map signify relative differences in how much the surface temperature changed between those two observations. Blue indicates the locations with the least change. Red indicates areas with most change. Modeling provides estimates that the range of temperature changes shown in this map corresponds to a range in depth-to-ice of less than 1 centimeter (0.4 inch) to more than 19 centimeters (more than 7.5 inches). The sensitivity of this method for estimating the depth is not good for depths greater than about 20, centimeters (8 inches). The temperature-change data are overlaid on a mosaic of black-and-white, daytime images taken in infrared wavelengths by the same camera, providing information about shapes in the landscape. The 20-kilometer scale bar is 12.4 miles long. Credit: NASA/JPL/ASU |
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Depth-to-Ice Map of an Arcti
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| title |
Depth-to-Ice Map of an Arctic Site on Mars |
| Description |
Color coding in this map of a far-northern site on Mars indicates the change in nighttime ground-surface temperature between summer and fall. This site, like most of high-latitude Mars, has water ice mixed with soil near the surface. The ice is probably in a rock-hard frozen layer beneath a few centimeters or inches of looser, dry soil. The amount of temperature change at the surface likely corresponds to how close to the surface the icy material lies. The dense, icy layer retains heat better than the looser soil above it, so where the icy layer is closer to the surface, the surface temperature changes more slowly than where the icy layer is buried deeper. On the map, areas of the surface that cooled more slowly between summer and autumn (interpreted as having the ice closer to the surface) are coded blue and green. Areas that cooled more quickly (interpreted as having more distance to the ice) are coded red and yellow. The depth to the top of the icy layer estimated from these observations, as little as 5 centimeters (2 inches), matches modeling of where it would be if Mars has an active cycle of water being exchanged by diffusion between atmospheric water vapor and subsurface water ice. This map and its interpretation are in a May 3, 2007, report in the journal Nature by Joshua Bandfield of Arizona State University, Tempe. The Thermal Emission Imaging System camera on NASA's Mars Odyssey orbiter collected the data presented in the map. The site is centered near 67.5 degrees north latitude, 132 degrees east longitude, in the Martian arctic plains called Vastitas Borealis. It was formerly a candidate landing site for NASA's Phoenix Mars Lander mission. This site is within the portion of the planet where, in 2002, the Gamma Ray Spectrometer suite of instruments on Mars Odyssey found evidence for water ice lying just below the surface. The information from the Gamma Ray Spectrometer is averaged over patches of ground hundreds of kilometers or miles wide. The information from the Thermal Emission Imaging System allows more than 100-fold higher resolution in mapping variations in the depth to ice. The Thermal Emission Imaging System observed the site in infrared wavelengths during night time, providing surface-temperature information, once on March 13, 2005, during summer in Mars' northern hemisphere, and again on April 8, 2005, during autumn there. The colors on this map signify relative differences in how much the surface temperature changed between those two observations. Blue indicates the locations with the least change. Red indicates areas with most change. Modeling provides estimates that the range of temperature changes shown in this map corresponds to a range in depth-to-ice of 5 centimeters (2 inches) to more than 18 centimeters (more than 7 inches). The sensitivity of this method for estimating the depth is not good for depths greater than about 20 centimeters (8 inches). The temperature-change data are overlaid on a mosaic of, black-and-white, daytime images taken in visible-light wavelengths by the same camera, providing information about shapes in the landscape. The 10-kilometer scale bar is 6.2 miles long. Credit: NASA/JPL/ASU |
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2001 Mars Odyssey Turns 5
| title |
2001 Mars Odyssey Turns 5 |
| Description |
Five years after leaving Florida for Mars, NASA's Mars Odyssey spacecraft is still orbiting the red planet, collecting scientific data and relaying communications from NASA's two Mars rovers to Earth. Images such as this spectacular, color view of sun-bathed, layered escarpments and wind-scalloped, basalt dunes in the solar system's largest canyon continue to beckon space explorers and guide the way for future missions. Basaltic dunes are common on Mars but rare on Earth. Rounded knobs and mesas on the canyon floor are reminiscent of desert geology in the southwestern U.S. A team led by Phil Christensen, principal investigator for Odyssey's cameras at Arizona State University, Jim Bell at Cornell University, and space artist Don Davis created this panorama. They added color to radiance files from the Thermal Emission Imaging System (THEMIS), a camera on Odyssey that takes images in both the visible and infrared parts of the spectrum. They correlated the radiance - intensity of reflected sunlight - with that of other color images from Mars and mimimized the effects of residual scattered light in the images. In addition to producing images such as this, Mars Odyssey has made global observations of Martian climate, geology, and mineralogy. The spacecraft's Gamma Ray Spectrometer has allowed scientists to make maps of the elemental distribution of hydrogen, silicon, iron, potassium, thorium, and chlorine on the Martian surface. A global map of minerals associated with water, essential to life as we know it, guided NASA in its selection of Meridiani Planum, the landing site for NASA's Opportunity rover, an area rich in hematite. Odyssey is currently supporting landing site selection for the Phoenix Scout Mission, to be launched in 2007, using data showing that surface areas near the poles of Mars consist of more than 50 percent water ice by volume. Other Odyssey accomplishments include measurement of radiation, a prerequisite for future human exploration because of its potential health effects, and a groundbreaking program in education outreach that has allowed students to take pictures of Mars and conduct scientific investigations with cameras on Odyssey. Mars Odyssey was launched April 7, 2001 on a Delta II rocket from Cape Canaveral, Florida, and reached Mars on October 24, 2001. Odyssey employed a technique called "aerobraking" that used the atmosphere of Mars to slow down and gradually bring the spacecraft closer to Mars with each orbit. Odyssey's science mapping mission began in February 2002. The primary science mission continued through August 2004. Odyssey is currently in its extended mission. Credit: NASA/JPL-Caltech/ASU/Cornell/Don Davis |
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Rocky Mesas of Nilosyrtis Me
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PIA10071
Sol (our sun)
HiRISE
| Title |
Rocky Mesas of Nilosyrtis Mensae Region, in Color |
| Original Caption Released with Image |
Mesas in the Nilosyrtis Mensae region of Mars appear in enhanced color in this image from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. The image was taken on April 5, 2007, as part of a campaign to examine more than two dozen candidate landing sites for the NASA Mars Science Laboratory rover, which is scheduled for launch in 2009. This image shows a region of science interest to which the Mars Science Laboratory rover might drive. It would need to first land in a nearby area that is flatter and less rocky. Clay minerals have been detected in this region by imaging spectrometers on the European Space Agency's Mars Express orbiter and on the Mars Reconnaissance Orbiter. These minerals are of great interest in the search for evidence of life on ancient Mars. Someday the capability may exist for precision landing and hazard avoidance, so a rover could be set down right next to such rugged outcrops of interest for study and perhaps for collection of rock samples for return to Earth. The area covered by this image is about one kilometer (six-tenths of a mile) across, at 29.3 degrees north latitude, 73.3 degrees east longitude. North is up. The view is a composite of exposures that HiRISE took in the infrared, red and blue portions of the spectrum. Color is enhanced, a technique useful for analyzing landscapes. This is a portion of the full-frame color image catalogued as PSP_003231_2095 [ http://hirise.lpl.arizona.edu/PSP_003231_2095 ] in the HiRISE collection. It was taken at a local Mars time of 3:28 p.m. The scene is illuminated from the west with a solar incidence angle of 66 degrees, thus the sun was about 24 degrees above the horizon. The season on Mars was northern autumn. |
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Color Image of Nili Fossae T
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PIA10070
Sol (our sun)
HiRISE
| Title |
Color Image of Nili Fossae Trough, a Candidate MSL Landing Site |
| Original Caption Released with Image |
A portion of a trough in the Nili Fossae region of Mars is shown in enhanced color in this image from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. The image was taken on March 24, 2007, as part of a campaign to examine more than two dozen candidate landing sites for the NASA Mars Science Laboratory rover, which is scheduled for launch in 2009. The Nili Fossae region has one of the largest exposures of clay minerals discovered by the mapping spectrometer (called OMEGA for its French name's acronym) on the European Space Agency's Mars Express orbiter. These minerals have also been mapped in greater detail by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on the Mars Reconnaissance Orbiter (see http://crism.jhuapl.edu/gallery/featuredImage [ http://crism.jhuapl.edu/gallery/featuredImage ]). This image covers an area nearly one kilometer (six-tenths of a mile) wide, at 21.1 degrees north latitude, 74.2 degrees east longitude. North is up. It is a composite of exposures that HiRISE took in the infrared, red and blue portions of the spectrum. Color is enhanced beyond the standard enhancement in HiRISE color images, as this view is excerpted from a special video treatment of the full-frame image. The purple areas are basaltic in composition, including sand-sized material that bounces around in the wind to form dunes. Basalt in the most common type of volcanic rock on the Earth and other terrestrial planets. Orange areas are rich in clays. Clay minerals contain water in their mineral structure and may also preserve organic materials, so there is great interest in studying these deposits to understand past environments that could have supported life. The blue-green patches are outcrops of unaltered rocks rich in the mineral pyroxene. This is a portion of the full-frame color image catalogued as PSP_003086_2015 [ http://hirise.lpl.arizona.edu/PSP_003086_2015 ] in the HiRISE collection. The image was taken at a local Mars time of 3:38 p.m. The scene is illuminated from the west with a solar incidence angle of 62 degrees, thus the sun was about 28 degrees above the horizon. The season on Mars was northern autumn. |
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Preparing the Phoenix Lander
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PIA07246
| Title |
Preparing the Phoenix Lander for Mars |
| Original Caption Released with Image |
The Phoenix Mission, slated for launch in August 2007, is the first project in NASA's openly competed program of Mars Scout missions. The Phoenix lander is currently housed in a 100,000-class clean room at Lockheed Martin Space Systems' facilities near Denver, Colo. Shown here, the lander is contained inside the backshell portion of the aeroshell (with the heat shield removed). The lander is sitting in an inverted or upside-down position, with the underside of the lander facing up. The lander's "legs" are not yet attached. Work on the lander will continue in late 2005, when the Phoenix team will make specific modifications and prepare for assembly, test and launch operations to get underway in spring 2006. |
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Phoenix Mission Lander on Ma
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PIA07247
| Title |
Phoenix Mission Lander on Mars, Artist's Concept |
| Original Caption Released with Image |
The Phoenix Mission, slated for launch in August 2007, is the first project in NASA's openly competed program of Mars Scout missions. The mission's plan is to land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. The spacecraft and its instruments are designed to analyze samples collected from up to a half-meter (20 inches) deep by a robotic arm. The arm extends forward in this artist's concept of the lander on Mars. |
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Ares Vallis Cataract
PIA09683
Sol (our sun)
HiRISE
| Title |
Ares Vallis Cataract |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003538_1885 [ http://hirise.lpl.arizona.edu/PSP_003538_1885 ]) shows a dry cataract within Ares Vallis. A cataract is a large waterfall where there is a high, steep drop. The presence of this large cataract in Ares Vallis confirms that this channel was carved by water, probably in one or many large catastrophic flooding events. This feature has many of the same characteristics as the cataracts on Earth associated with the flood that carved the Channelled Scablands in Washington state, including horseshoe-shaped headcuts and longitudinal grooves. These grooves in the lower portion of the image lead up to the cataract, with the water flowing from the south to the north in this image. It then flowed down the cataract into the smaller incised channel. The horseshoe-shaped headcut here is only part of a larger cataract system, and probably formed during the last stage of flooding. The inner channels are now filled with dunes formed by wind blowing along the channel floor. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PMDegrees latitude (centered): 8.4° Degrees longitude (East): 335.6° Range to target site: 276.0 km (172.5 miles) Original image scale range: 27.6 cm/pixel (with 1 x 1 binning) so objects ~83 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.3° Phase angle: 56.9° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 228.1°, Northern Autumn 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. |
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Ares Vallis Cataract
PIA09683
Sol (our sun)
HiRISE
| Title |
Ares Vallis Cataract |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003538_1885 [ http://hirise.lpl.arizona.edu/PSP_003538_1885 ]) shows a dry cataract within Ares Vallis. A cataract is a large waterfall where there is a high, steep drop. The presence of this large cataract in Ares Vallis confirms that this channel was carved by water, probably in one or many large catastrophic flooding events. This feature has many of the same characteristics as the cataracts on Earth associated with the flood that carved the Channelled Scablands in Washington state, including horseshoe-shaped headcuts and longitudinal grooves. These grooves in the lower portion of the image lead up to the cataract, with the water flowing from the south to the north in this image. It then flowed down the cataract into the smaller incised channel. The horseshoe-shaped headcut here is only part of a larger cataract system, and probably formed during the last stage of flooding. The inner channels are now filled with dunes formed by wind blowing along the channel floor. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PMDegrees latitude (centered): 8.4° Degrees longitude (East): 335.6° Range to target site: 276.0 km (172.5 miles) Original image scale range: 27.6 cm/pixel (with 1 x 1 binning) so objects ~83 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.3° Phase angle: 56.9° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 228.1°, Northern Autumn 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. |
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Slope Streak South of Olympu
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PIA09685
Sol (our sun)
HiRISE
| Title |
Slope Streak South of Olympus Mons |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003239_1870 [ http://hirise.lpl.arizona.edu/PSP_003239_1870 ]) reveals slope streaks in an area south of Olympus Mons in the northern hemisphere of Mars. These features are found along the slopes of impact craters, buttes, knobs, ridges, and troughs on Mars. Streaks generally start at a point source and widen downslope, traveling over and sometimes around various obstacles. The subimage [ http://photojournal.jpl.nasa.gov/figures/PIA09685_fig2.jpg ], shows a very wide dark slope that has developed small fingers at its terminus. The dark slope streak does not appear to have relief and does not disturb the pre-existing surface leaving the underlying topography intact beneath its dark trail. This can be seen particularly well near the streak termination. There are also no observable deposits of displaced materials along the terminus. Surrounding the dark slope streak are multiple ~1 meter deep, triangular faceted scars left behind from avalanched slope materials. The high standing remnant surfaces on either side of the lower scarred surface are clearly visible. Avalanche scars are sometimes found in areas where slope streaks have formed but they are believed to be unrelated. The trail of the dark slope streak appears to cross over the avalanche scars suggesting that the slope streak formed more recently. Slope streak formation is among the few known processes currently active on Mars. While their mechanism of formation and triggering is debated, they are most commonly believed to form by downslope movement of extremely dry sand or very fine-grained dust in an almost fluidlike manner (analogous to a terrestrial snow avalanche) exposing darker underlying material. Other ideas include the triggering of slope streak formation by possible concentrations of near-surface ice or scouring of the surface by running water from aquifers intercepting slope faces, briny liquid flows, dry granular flow, mixed water-dust flows, and/or hydrothermal activity. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:35 PM Degrees latitude (centered): 7.1° Degrees longitude (East): 218.2° Range to target site: 274.5 km (171.6 miles) Original image scale range: 54.9 cm/pixel (with 2 x 2 binning) so objects ~165 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 4.2° Phase angle: 61.3° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 213.6°, Northern Autumn 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. |
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Slope Streak South of Olympu
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PIA09685
Sol (our sun)
HiRISE
| Title |
Slope Streak South of Olympus Mons |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003239_1870 [ http://hirise.lpl.arizona.edu/PSP_003239_1870 ]) reveals slope streaks in an area south of Olympus Mons in the northern hemisphere of Mars. These features are found along the slopes of impact craters, buttes, knobs, ridges, and troughs on Mars. Streaks generally start at a point source and widen downslope, traveling over and sometimes around various obstacles. The subimage [ http://photojournal.jpl.nasa.gov/figures/PIA09685_fig2.jpg ], shows a very wide dark slope that has developed small fingers at its terminus. The dark slope streak does not appear to have relief and does not disturb the pre-existing surface leaving the underlying topography intact beneath its dark trail. This can be seen particularly well near the streak termination. There are also no observable deposits of displaced materials along the terminus. Surrounding the dark slope streak are multiple ~1 meter deep, triangular faceted scars left behind from avalanched slope materials. The high standing remnant surfaces on either side of the lower scarred surface are clearly visible. Avalanche scars are sometimes found in areas where slope streaks have formed but they are believed to be unrelated. The trail of the dark slope streak appears to cross over the avalanche scars suggesting that the slope streak formed more recently. Slope streak formation is among the few known processes currently active on Mars. While their mechanism of formation and triggering is debated, they are most commonly believed to form by downslope movement of extremely dry sand or very fine-grained dust in an almost fluidlike manner (analogous to a terrestrial snow avalanche) exposing darker underlying material. Other ideas include the triggering of slope streak formation by possible concentrations of near-surface ice or scouring of the surface by running water from aquifers intercepting slope faces, briny liquid flows, dry granular flow, mixed water-dust flows, and/or hydrothermal activity. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:35 PM Degrees latitude (centered): 7.1° Degrees longitude (East): 218.2° Range to target site: 274.5 km (171.6 miles) Original image scale range: 54.9 cm/pixel (with 2 x 2 binning) so objects ~165 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 4.2° Phase angle: 61.3° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 213.6°, Northern Autumn 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. |
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Faults and Folds in Western
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PIA09682
Sol (our sun)
HiRISE
| Title |
Faults and Folds in Western Candor Chasma |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003540_1735 [ http://hirise.lpl.arizona.edu/PSP_003540_1735 ]) shows various interesting structures along the floor of Candor Chasma, a major canyon of Valles Marineris. The rocks along the floor of the chasma consist of multiple layers of light-toned material, possibly windblown or water-lain sediment. These layers have been shifted along faults and also folded, giving the layers an apparent wavy appearance as they are exposed at the surface through erosion. Some waviness in the layers may also have formed as these sediments were laid down, for example, in dunes or large ripples. Detailed mapping of these faults and folds may help reveal the origin of these layered deposits and if water played any role in their formation. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:33 PM Degrees latitude (centered): -6.4° Degrees longitude (East): 283.2° Range to target site: 263.6 km (164.7 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 7.3° Phase angle: 46.0° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 228.2°, Northern Autumn 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. |
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Faults and Folds in Western
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PIA09682
Sol (our sun)
HiRISE
| Title |
Faults and Folds in Western Candor Chasma |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003540_1735 [ http://hirise.lpl.arizona.edu/PSP_003540_1735 ]) shows various interesting structures along the floor of Candor Chasma, a major canyon of Valles Marineris. The rocks along the floor of the chasma consist of multiple layers of light-toned material, possibly windblown or water-lain sediment. These layers have been shifted along faults and also folded, giving the layers an apparent wavy appearance as they are exposed at the surface through erosion. Some waviness in the layers may also have formed as these sediments were laid down, for example, in dunes or large ripples. Detailed mapping of these faults and folds may help reveal the origin of these layered deposits and if water played any role in their formation. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:33 PM Degrees latitude (centered): -6.4° Degrees longitude (East): 283.2° Range to target site: 263.6 km (164.7 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 7.3° Phase angle: 46.0° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 228.2°, Northern Autumn 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. |
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Layers in Galle Crater
PIA09686
Sol (our sun)
HiRISE
| Title |
Layers in Galle Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image shows part of a large mass of layered rock in Galle Crater, in the southern cratered highlands of Mars. At low resolution, layers appear as bands and swirls which are nearly horizontal. This causes them to interact dramatically with topography, producing the appearance of folds and loops wrapping around small hills much like lines on a contour map. Zooming in at higher resolution, some long cracks (hundreds of meters long) are cutting across the layers, generally trending northeast-southwest. At full resolution (PSP_002655_1280 [ http://hirise.lpl.arizona.edu/PSP_002655_1280 ]), details of the layers are often obscured by ripples of wind-blown dust or textured patterns of erosion now eroding the rock. In the best exposures, such as that in the cutout section, the layers are fractured into blocks. Some of the layers are relatively resistant, and appear as ridges or fins in the cutout, often with little material supporting them from below. Although this seems to indicate relatively strong, coherent material, few boulders are visible. The ridge-forming layers may be weak, but separated by material with virtually no cohesion. Polygonal fracture patterns in the dark regolith between distinct layers could be due to ground ice, or regional tectonic stresses. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:54 PM Degrees latitude (centered): -51.8° Degrees longitude (East): 330.0° Range to target site: 256.3 km (160.2 miles) Original image scale range: 25.6 cm/pixel (with 1 x 1 binning) so objects ~77 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.8° Phase angle: 71.5° Solar incidence angle: 69°, with the Sun about 21° above the horizon Solar longitude: 186.6°, Northern Autumn 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. |
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Layers in Galle Crater
PIA09686
Sol (our sun)
HiRISE
| Title |
Layers in Galle Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image shows part of a large mass of layered rock in Galle Crater, in the southern cratered highlands of Mars. At low resolution, layers appear as bands and swirls which are nearly horizontal. This causes them to interact dramatically with topography, producing the appearance of folds and loops wrapping around small hills much like lines on a contour map. Zooming in at higher resolution, some long cracks (hundreds of meters long) are cutting across the layers, generally trending northeast-southwest. At full resolution (PSP_002655_1280 [ http://hirise.lpl.arizona.edu/PSP_002655_1280 ]), details of the layers are often obscured by ripples of wind-blown dust or textured patterns of erosion now eroding the rock. In the best exposures, such as that in the cutout section, the layers are fractured into blocks. Some of the layers are relatively resistant, and appear as ridges or fins in the cutout, often with little material supporting them from below. Although this seems to indicate relatively strong, coherent material, few boulders are visible. The ridge-forming layers may be weak, but separated by material with virtually no cohesion. Polygonal fracture patterns in the dark regolith between distinct layers could be due to ground ice, or regional tectonic stresses. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:54 PM Degrees latitude (centered): -51.8° Degrees longitude (East): 330.0° Range to target site: 256.3 km (160.2 miles) Original image scale range: 25.6 cm/pixel (with 1 x 1 binning) so objects ~77 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.8° Phase angle: 71.5° Solar incidence angle: 69°, with the Sun about 21° above the horizon Solar longitude: 186.6°, Northern Autumn 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. |
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Evros Vallis and Nearby Crat
…
PIA09684
Sol (our sun)
HiRISE
| Title |
Evros Vallis and Nearby Craters |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003273_1675 [ http://hirise.lpl.arizona.edu/PSP_003273_1675 ]) shows part of Evros Vallis, one of the Martian valley networks. These more ancient valley networks may have been eroded by flowing water during a warmer, wetter period of Martian history. Many dunes are visibile along the valley floor, as well as throughout the scene and in a partially exhumed crater on the valley wall. There are multiple generations and orientations of dunes. Dune orientation reflects the dominant or prevailing wind direction. Multiple dune orientations indicate that this region has experienced different wind regimes. An exhumed crater is one that likely formed a long time ago, was buried, and is now being re-exposed because the materials that originally covered it are being eroded away. The prominent crater on the valley wall as well as several other craters in this scene are thought to be partially exhumed. The subimage [ http://photojournal.jpl.nasa.gov/figures/PIA09684_fig2.jpg ] (approximately 300 m across) shows a couple groups of secondary craters. Secondary craters are craters that form when ejecta from the primary crater hits the surface with enough energy to form another smaller crater. As seen in the subimage, secondary craters often form in clusters spatially, because ejecta thrown out of the primary crater impacts the surface near each other at approximately the same time. Many potential secondary craters have have similar morphologies and have distinct, bright ejecta. This implies that these craters are relatively young and that their ejecta have yet to be covered by dust. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -12.6° Degrees longitude (East): 13.3° Range to target site: 264.3 km (165.2 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 7.6° Phase angle: 46.2° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 215.3°, Northern Autumn 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. |
|
Evros Vallis and Nearby Crat
…
PIA09684
Sol (our sun)
HiRISE
| Title |
Evros Vallis and Nearby Craters |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003273_1675 [ http://hirise.lpl.arizona.edu/PSP_003273_1675 ]) shows part of Evros Vallis, one of the Martian valley networks. These more ancient valley networks may have been eroded by flowing water during a warmer, wetter period of Martian history. Many dunes are visibile along the valley floor, as well as throughout the scene and in a partially exhumed crater on the valley wall. There are multiple generations and orientations of dunes. Dune orientation reflects the dominant or prevailing wind direction. Multiple dune orientations indicate that this region has experienced different wind regimes. An exhumed crater is one that likely formed a long time ago, was buried, and is now being re-exposed because the materials that originally covered it are being eroded away. The prominent crater on the valley wall as well as several other craters in this scene are thought to be partially exhumed. The subimage [ http://photojournal.jpl.nasa.gov/figures/PIA09684_fig2.jpg ] (approximately 300 m across) shows a couple groups of secondary craters. Secondary craters are craters that form when ejecta from the primary crater hits the surface with enough energy to form another smaller crater. As seen in the subimage, secondary craters often form in clusters spatially, because ejecta thrown out of the primary crater impacts the surface near each other at approximately the same time. Many potential secondary craters have have similar morphologies and have distinct, bright ejecta. This implies that these craters are relatively young and that their ejecta have yet to be covered by dust. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -12.6° Degrees longitude (East): 13.3° Range to target site: 264.3 km (165.2 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 7.6° Phase angle: 46.2° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 215.3°, Northern Autumn 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. |
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Dark Slope Streak with Strea
…
PIA09681
Sol (our sun)
HiRISE
| Title |
Dark Slope Streak with Streak-Generated Topography |
| Original Caption Released with Image |
Click on image for larger version This is a portion of HiRISE image PSP_003542_2035 [ http://hirise.lpl.arizona.edu/PSP_003542_2035 ] which shows a dark slope streak north of Olympus Mons, in a region was covered by Mars Orbital Camera image R09/00701. (This portion is rotated with south up so that the direction the streak flowed is towards the bottom of the frame). This image shows that the slope streak forming process altered the pre-existing surface both by excavating material and depositing it. The fine scalloped texture of the surrounding surface is not present within the streak, and there are low linear mounds within the streak that are not seen outside. Their absence outside the streak indicates that the formation of the mounds resulted from the streak formation process. There is a large boulder or knob within the streak near the top of the frame which the dark slope streak appears to have flowed around, leaving a light-toned patch of the surrounding surface material intact downstream of the boulder. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:22 PM Degrees latitude (centered): 23.3° Degrees longitude (East): 223.7° Range to target site: 285.3 km (178.3 miles) Original image scale range: 28.5 cm/pixel (with 1 x 1 binning) so objects ~86 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 7.6° Phase angle: 71.6° Solar incidence angle: 65°, with the Sun about 25° above the horizon Solar longitude: 228.3°, Northern Autumn 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. |
|
Dark Slope Streak with Strea
…
PIA09681
Sol (our sun)
HiRISE
| Title |
Dark Slope Streak with Streak-Generated Topography |
| Original Caption Released with Image |
Click on image for larger version This is a portion of HiRISE image PSP_003542_2035 [ http://hirise.lpl.arizona.edu/PSP_003542_2035 ] which shows a dark slope streak north of Olympus Mons, in a region was covered by Mars Orbital Camera image R09/00701. (This portion is rotated with south up so that the direction the streak flowed is towards the bottom of the frame). This image shows that the slope streak forming process altered the pre-existing surface both by excavating material and depositing it. The fine scalloped texture of the surrounding surface is not present within the streak, and there are low linear mounds within the streak that are not seen outside. Their absence outside the streak indicates that the formation of the mounds resulted from the streak formation process. There is a large boulder or knob within the streak near the top of the frame which the dark slope streak appears to have flowed around, leaving a light-toned patch of the surrounding surface material intact downstream of the boulder. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:22 PM Degrees latitude (centered): 23.3° Degrees longitude (East): 223.7° Range to target site: 285.3 km (178.3 miles) Original image scale range: 28.5 cm/pixel (with 1 x 1 binning) so objects ~86 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 7.6° Phase angle: 71.6° Solar incidence angle: 65°, with the Sun about 25° above the horizon Solar longitude: 228.3°, Northern Autumn 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. |
|
Layered Deposits in Ritchey
…
PIA09667
Sol (our sun)
HiRISE
| Title |
Layered Deposits in Ritchey Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003249_1510 [ http://hirise.lpl.arizona.edu/PSP_003249_1510 ]) shows eroding layered deposits in Ritchey Crater, a large impact crater in the southern highlands. Three general units can be seen: a relatively dark upper layer, a light middle unit, and the floor material, which may be mostly obscured by dust. The dark cap layer appears to be relatively hard and resistant, while the light material is weak. Once the upper layer is removed, the light layer does not last long. The cutout from the top center part of the image shows this stack. The dark unit is thin and breaking into boulders. The light material is actually divided into smaller layers, and is pervasively fractured. However, the boulders falling from the edge are mostly small and rarely remain intact if they move more than a few meters. The cracking of the layer could be due to water loss from the layer, or to regional tectonic effects such as stresses from burial and erosion. The base unit is partially covered by wind-blown ripples. It is unclear how each of these layers formed. Volcanic ash layers, lake or stream deposits, or sandstone deposited by dunes can all produce horizontal layers. Unraveling the origin would provide important clues to Mars' past. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -28.5° Degrees longitude (East): 309.4° Range to target site: 259.1 km (161.9 miles) Original image scale range: 25.9 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: 7.4° Phase angle: 60.4° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 214.1°, Northern Autumn 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. |
|
Layered Deposits in Ritchey
…
PIA09667
Sol (our sun)
HiRISE
| Title |
Layered Deposits in Ritchey Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003249_1510 [ http://hirise.lpl.arizona.edu/PSP_003249_1510 ]) shows eroding layered deposits in Ritchey Crater, a large impact crater in the southern highlands. Three general units can be seen: a relatively dark upper layer, a light middle unit, and the floor material, which may be mostly obscured by dust. The dark cap layer appears to be relatively hard and resistant, while the light material is weak. Once the upper layer is removed, the light layer does not last long. The cutout from the top center part of the image shows this stack. The dark unit is thin and breaking into boulders. The light material is actually divided into smaller layers, and is pervasively fractured. However, the boulders falling from the edge are mostly small and rarely remain intact if they move more than a few meters. The cracking of the layer could be due to water loss from the layer, or to regional tectonic effects such as stresses from burial and erosion. The base unit is partially covered by wind-blown ripples. It is unclear how each of these layers formed. Volcanic ash layers, lake or stream deposits, or sandstone deposited by dunes can all produce horizontal layers. Unraveling the origin would provide important clues to Mars' past. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -28.5° Degrees longitude (East): 309.4° Range to target site: 259.1 km (161.9 miles) Original image scale range: 25.9 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: 7.4° Phase angle: 60.4° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 214.1°, Northern Autumn 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. |
|
Layered Deposits in Ritchey
…
PIA09667
Sol (our sun)
HiRISE
| Title |
Layered Deposits in Ritchey Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003249_1510 [ http://hirise.lpl.arizona.edu/PSP_003249_1510 ]) shows eroding layered deposits in Ritchey Crater, a large impact crater in the southern highlands. Three general units can be seen: a relatively dark upper layer, a light middle unit, and the floor material, which may be mostly obscured by dust. The dark cap layer appears to be relatively hard and resistant, while the light material is weak. Once the upper layer is removed, the light layer does not last long. The cutout from the top center part of the image shows this stack. The dark unit is thin and breaking into boulders. The light material is actually divided into smaller layers, and is pervasively fractured. However, the boulders falling from the edge are mostly small and rarely remain intact if they move more than a few meters. The cracking of the layer could be due to water loss from the layer, or to regional tectonic effects such as stresses from burial and erosion. The base unit is partially covered by wind-blown ripples. It is unclear how each of these layers formed. Volcanic ash layers, lake or stream deposits, or sandstone deposited by dunes can all produce horizontal layers. Unraveling the origin would provide important clues to Mars' past. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -28.5° Degrees longitude (East): 309.4° Range to target site: 259.1 km (161.9 miles) Original image scale range: 25.9 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: 7.4° Phase angle: 60.4° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 214.1°, Northern Autumn 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. |
|
Proposed MSL Site in Eberswa
…
PIA09678
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Eberswalde Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003231_2095 [ http://hirise.lpl.arizona.edu/PSP_003231_2095 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Eberswalde Crater. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 29.3° Degrees longitude (East): 73.3° Range to target site: 290.3 km (181.4 miles) Original image scale range: 29.0 cm/pixel (with 1 x 1 binning) so objects ~87 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 8.0° Phase angle: 73.5° Solar incidence angle: 66°, with the Sun about 24° above the horizon Solar longitude: 213.3°, Northern Autumn 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. |
|
Proposed MSL Site in Eberswa
…
PIA09678
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Eberswalde Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003231_2095 [ http://hirise.lpl.arizona.edu/PSP_003231_2095 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Eberswalde Crater. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 29.3° Degrees longitude (East): 73.3° Range to target site: 290.3 km (181.4 miles) Original image scale range: 29.0 cm/pixel (with 1 x 1 binning) so objects ~87 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 8.0° Phase angle: 73.5° Solar incidence angle: 66°, with the Sun about 24° above the horizon Solar longitude: 213.3°, Northern Autumn 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. |
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Alluvial Fan Along a Crater
…
PIA09666
Sol (our sun)
HiRISE
| Title |
Alluvial Fan Along a Crater Wall |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003269_1600 [ http://hirise.lpl.arizona.edu/PSP_003269_1600 ]) covers an alluvial fan along the wall of a large crater in the mid latitudes of the southern hemisphere of Mars. The fan was formed when water and sediments drained down the steep wall of the crater creating a cone-shaped pile of debris at the base. As the fan grew with time, the channels carrying water and sediment across the fan surface changed locations, producing a layered deposit capped by channels radiating from the fan apex along the crater wall. Subsequent stripping of the fan surface by the wind has left the coarser channel deposits in relief and exposed the fine scale layering within the fan in many locations. While is it is not known whether the source of the water responsible for creating the fan was related runoff from precipitation or groundwater or perhaps both, alluvial fans of broadly similar form are observed in many locations on Earth and are usually formed by runoff from precipitation. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -19.9° Degrees longitude (East): 123.2° Range to target site: 258.6 km (161.6 miles) Original image scale range: 25.9 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: 4.7° Phase angle: 48.6° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 215.1°, Northern Autumn 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. |
|
Alluvial Fan Along a Crater
…
PIA09666
Sol (our sun)
HiRISE
| Title |
Alluvial Fan Along a Crater Wall |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003269_1600 [ http://hirise.lpl.arizona.edu/PSP_003269_1600 ]) covers an alluvial fan along the wall of a large crater in the mid latitudes of the southern hemisphere of Mars. The fan was formed when water and sediments drained down the steep wall of the crater creating a cone-shaped pile of debris at the base. As the fan grew with time, the channels carrying water and sediment across the fan surface changed locations, producing a layered deposit capped by channels radiating from the fan apex along the crater wall. Subsequent stripping of the fan surface by the wind has left the coarser channel deposits in relief and exposed the fine scale layering within the fan in many locations. While is it is not known whether the source of the water responsible for creating the fan was related runoff from precipitation or groundwater or perhaps both, alluvial fans of broadly similar form are observed in many locations on Earth and are usually formed by runoff from precipitation. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -19.9° Degrees longitude (East): 123.2° Range to target site: 258.6 km (161.6 miles) Original image scale range: 25.9 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: 4.7° Phase angle: 48.6° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 215.1°, Northern Autumn 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. |
|
Craters on South Polar Layer
…
PIA09670
Sol (our sun)
HiRISE
| Title |
Craters on South Polar Layered Deposits |
| Original Caption Released with Image |
Click on image for larger version This subimage, about 2.5 km across, shows the south polar layered deposits exposed in a scarp illuminated from the lower right. This HiRISE image (PSP_002882_0940 [ http://hirise.lpl.arizona.edu/PSP_002882_0940 ]) was taken in the southern spring, when the surface was completely covered by carbon dioxide frost. Therefore, most of the brightness variations in this scene are caused by topography. The polar layered deposits are broken into blocks by fractures in two directions. Neither set of fractures is parallel to the current scarp face, suggesting that they were not formed as the scarp was eroded, but instead are due to pre-existing weaknesses in the polar layered deposits. The four craters at lower left appear to have formed at the same time by an impactor that broke up as it entered the Martian atmosphere. The presence of many craters such as these on the south polar layered deposits indicates that they are not as young as the north polar layered deposits, which have very few craters on them. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 7:06 PM Degrees latitude (centered): -85.9° Degrees longitude (East): 303.4° Range to target site: 246.9 km (154.3 miles) Original image scale range: 24.7 cm/pixel (with 1 x 1 binning) so objects ~74 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 6.7° Phase angle: 78.5° Solar incidence angle: 84°, with the Sun about 6° above the horizon Solar longitude: 196.9°, Northern Autumn 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. |
|
Craters on South Polar Layer
…
PIA09670
Sol (our sun)
HiRISE
| Title |
Craters on South Polar Layered Deposits |
| Original Caption Released with Image |
Click on image for larger version This subimage, about 2.5 km across, shows the south polar layered deposits exposed in a scarp illuminated from the lower right. This HiRISE image (PSP_002882_0940 [ http://hirise.lpl.arizona.edu/PSP_002882_0940 ]) was taken in the southern spring, when the surface was completely covered by carbon dioxide frost. Therefore, most of the brightness variations in this scene are caused by topography. The polar layered deposits are broken into blocks by fractures in two directions. Neither set of fractures is parallel to the current scarp face, suggesting that they were not formed as the scarp was eroded, but instead are due to pre-existing weaknesses in the polar layered deposits. The four craters at lower left appear to have formed at the same time by an impactor that broke up as it entered the Martian atmosphere. The presence of many craters such as these on the south polar layered deposits indicates that they are not as young as the north polar layered deposits, which have very few craters on them. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 7:06 PM Degrees latitude (centered): -85.9° Degrees longitude (East): 303.4° Range to target site: 246.9 km (154.3 miles) Original image scale range: 24.7 cm/pixel (with 1 x 1 binning) so objects ~74 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 6.7° Phase angle: 78.5° Solar incidence angle: 84°, with the Sun about 6° above the horizon Solar longitude: 196.9°, Northern Autumn 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. |
|
Craters on South Polar Layer
…
PIA09670
Sol (our sun)
HiRISE
| Title |
Craters on South Polar Layered Deposits |
| Original Caption Released with Image |
Click on image for larger version This subimage, about 2.5 km across, shows the south polar layered deposits exposed in a scarp illuminated from the lower right. This HiRISE image (PSP_002882_0940 [ http://hirise.lpl.arizona.edu/PSP_002882_0940 ]) was taken in the southern spring, when the surface was completely covered by carbon dioxide frost. Therefore, most of the brightness variations in this scene are caused by topography. The polar layered deposits are broken into blocks by fractures in two directions. Neither set of fractures is parallel to the current scarp face, suggesting that they were not formed as the scarp was eroded, but instead are due to pre-existing weaknesses in the polar layered deposits. The four craters at lower left appear to have formed at the same time by an impactor that broke up as it entered the Martian atmosphere. The presence of many craters such as these on the south polar layered deposits indicates that they are not as young as the north polar layered deposits, which have very few craters on them. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 7:06 PM Degrees latitude (centered): -85.9° Degrees longitude (East): 303.4° Range to target site: 246.9 km (154.3 miles) Original image scale range: 24.7 cm/pixel (with 1 x 1 binning) so objects ~74 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 6.7° Phase angle: 78.5° Solar incidence angle: 84°, with the Sun about 6° above the horizon Solar longitude: 196.9°, Northern Autumn 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. |
|
Proposed MSL Site in Nilo Sy
…
PIA09677
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Nilo Syrtis |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003231_2095 [ http://hirise.lpl.arizona.edu/PSP_003231_2095 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Nilo Syrtis. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 29.3° Degrees longitude (East): 73.3° Range to target site: 290.3 km (181.4 miles) Original image scale range: 29.0 cm/pixel (with 1 x 1 binning) so objects ~87 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 8.0° Phase angle: 73.5° Solar incidence angle: 66°, with the Sun about 24° above the horizon Solar longitude: 213.3°, Northern Autumn 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. |
|
Proposed MSL Site in Nilo Sy
…
PIA09677
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Nilo Syrtis |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003231_2095 [ http://hirise.lpl.arizona.edu/PSP_003231_2095 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Nilo Syrtis. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 29.3° Degrees longitude (East): 73.3° Range to target site: 290.3 km (181.4 miles) Original image scale range: 29.0 cm/pixel (with 1 x 1 binning) so objects ~87 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 8.0° Phase angle: 73.5° Solar incidence angle: 66°, with the Sun about 24° above the horizon Solar longitude: 213.3°, Northern Autumn 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. |
|
Kaiser Crater Dune Field
PIA09669
Sol (our sun)
HiRISE
| Title |
Kaiser Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003141_1330 [ http://hirise.lpl.arizona.edu/PSP_003141_1330 ]) shows a sand dune field in Kaiser Crater, a 210 km (130 miles) wide impact basin in the Hellespontus region of Mars. Winds have trapped massive quantities of sand on the floors of broad craters in this region. The steepest slopes on each dune, the slip faces, point to the east indicating that the dominant wind direction in this part of the dune field is from west to east. Patches of seasonal frost can be seen in the low areas between the dunes. The subimage reveals smaller secondary dunes superimposed on the surface of the large dunes and even smaller ripples that appear between and perpendicular to the secondary dunes. Avalanching or mass movement of sand has left deep scars on the slip face of the large dune in the upper left portion of the subimage. This may indicate that the sand is not loose but is weakly cemented. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -46.6° Degrees longitude (East): 19.3° Range to target site: 263.9 km (164.9 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 17.5° Phase angle: 74.6° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 209.0°, Northern Autumn 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. |
|
Kaiser Crater Dune Field
PIA09669
Sol (our sun)
HiRISE
| Title |
Kaiser Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003141_1330 [ http://hirise.lpl.arizona.edu/PSP_003141_1330 ]) shows a sand dune field in Kaiser Crater, a 210 km (130 miles) wide impact basin in the Hellespontus region of Mars. Winds have trapped massive quantities of sand on the floors of broad craters in this region. The steepest slopes on each dune, the slip faces, point to the east indicating that the dominant wind direction in this part of the dune field is from west to east. Patches of seasonal frost can be seen in the low areas between the dunes. The subimage reveals smaller secondary dunes superimposed on the surface of the large dunes and even smaller ripples that appear between and perpendicular to the secondary dunes. Avalanching or mass movement of sand has left deep scars on the slip face of the large dune in the upper left portion of the subimage. This may indicate that the sand is not loose but is weakly cemented. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -46.6° Degrees longitude (East): 19.3° Range to target site: 263.9 km (164.9 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 17.5° Phase angle: 74.6° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 209.0°, Northern Autumn 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. |
|
Kaiser Crater Dune Field
PIA09669
Sol (our sun)
HiRISE
| Title |
Kaiser Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003141_1330 [ http://hirise.lpl.arizona.edu/PSP_003141_1330 ]) shows a sand dune field in Kaiser Crater, a 210 km (130 miles) wide impact basin in the Hellespontus region of Mars. Winds have trapped massive quantities of sand on the floors of broad craters in this region. The steepest slopes on each dune, the slip faces, point to the east indicating that the dominant wind direction in this part of the dune field is from west to east. Patches of seasonal frost can be seen in the low areas between the dunes. The subimage reveals smaller secondary dunes superimposed on the surface of the large dunes and even smaller ripples that appear between and perpendicular to the secondary dunes. Avalanching or mass movement of sand has left deep scars on the slip face of the large dune in the upper left portion of the subimage. This may indicate that the sand is not loose but is weakly cemented. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -46.6° Degrees longitude (East): 19.3° Range to target site: 263.9 km (164.9 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 17.5° Phase angle: 74.6° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 209.0°, Northern Autumn 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. |
|
Proposed MSL Site in Juventa
…
PIA09674
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Juventae Chasma |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003368_1755 [ http://hirise.lpl.arizona.edu/PSP_003368_1755 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Juventae Chasma. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:34 PM Degrees latitude (centered): -4.5° Degrees longitude (East): 297.9° Range to target site: 268.1 km (167.6 miles) Original image scale range: 26.8 cm/pixel (with 1 x 1 binning) so objects ~80 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.5° Phase angle: 59.1° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 219.8°, Northern Autumn 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. |
|
Proposed MSL Site in Juventa
…
PIA09674
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Juventae Chasma |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003368_1755 [ http://hirise.lpl.arizona.edu/PSP_003368_1755 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Juventae Chasma. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:34 PM Degrees latitude (centered): -4.5° Degrees longitude (East): 297.9° Range to target site: 268.1 km (167.6 miles) Original image scale range: 26.8 cm/pixel (with 1 x 1 binning) so objects ~80 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.5° Phase angle: 59.1° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 219.8°, Northern Autumn 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. |
|
Valleys on the Ejecta Blanke
…
PIA09675
Sol (our sun)
HiRISE
| Title |
Valleys on the Ejecta Blanket from Cerulli Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003312_2145 [ http://hirise.lpl.arizona.edu/PSP_003312_2145 ]) reveals valleys that cross the ejecta from the large impact crater Cerulli to the south. The valleys appear to have been cut by flowing water and then buried by later deposits of unknown origin, possibly carried in by the wind. While it is clear that the valleys are younger than the ejecta and older than at least some of the mantling materials, the exact time they were formed is uncertain. For example, it is possible that the valleys were carved immediately after Cerulli crater formed, as has been inferred for some other valleys around craters imaged elsewhere on Mars by HiRISE. Alternatively, the valleys may have formed some time after the crater formed, perhaps as a result of water released from an earlier mantling deposit. A second image is planned for this area and will yield three-dimensional information from stereo that may help to resolve the timing and source of water responsible for carving the valleys. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:27 PM Degrees latitude (centered): 34.0° Degrees longitude (East): 21.8° Range to target site: 293.0 km (183.2 miles) Original image scale range: 29.3 cm/pixel (with 1 x 1 binning) so objects ~88 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 3.6° Phase angle: 72.8° Solar incidence angle: 70°, with the Sun about 20° above the horizon Solar longitude: 217.1°, Northern Autumn 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. |
|
Valleys on the Ejecta Blanke
…
PIA09675
Sol (our sun)
HiRISE
| Title |
Valleys on the Ejecta Blanket from Cerulli Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003312_2145 [ http://hirise.lpl.arizona.edu/PSP_003312_2145 ]) reveals valleys that cross the ejecta from the large impact crater Cerulli to the south. The valleys appear to have been cut by flowing water and then buried by later deposits of unknown origin, possibly carried in by the wind. While it is clear that the valleys are younger than the ejecta and older than at least some of the mantling materials, the exact time they were formed is uncertain. For example, it is possible that the valleys were carved immediately after Cerulli crater formed, as has been inferred for some other valleys around craters imaged elsewhere on Mars by HiRISE. Alternatively, the valleys may have formed some time after the crater formed, perhaps as a result of water released from an earlier mantling deposit. A second image is planned for this area and will yield three-dimensional information from stereo that may help to resolve the timing and source of water responsible for carving the valleys. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:27 PM Degrees latitude (centered): 34.0° Degrees longitude (East): 21.8° Range to target site: 293.0 km (183.2 miles) Original image scale range: 29.3 cm/pixel (with 1 x 1 binning) so objects ~88 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 3.6° Phase angle: 72.8° Solar incidence angle: 70°, with the Sun about 20° above the horizon Solar longitude: 217.1°, Northern Autumn 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. |
|
Proposed MSL Site in Gale Cr
…
PIA09679
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Gale Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003453_1750 [ http://hirise.lpl.arizona.edu/PSP_003453_1750 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Gale Crater. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:22 PM Degrees latitude (centered): -4.6° Degrees longitude (East): 137.4° Range to target site: 270.4 km (169.0 miles) Original image scale range: 27.1 cm/pixel (with 1 x 1 binning) so objects ~81 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 4.2° Phase angle: 57.5° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 223.9°, Northern Autumn 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. |
|
Proposed MSL Site in Gale Cr
…
PIA09679
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Gale Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003453_1750 [ http://hirise.lpl.arizona.edu/PSP_003453_1750 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Gale Crater. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:22 PM Degrees latitude (centered): -4.6° Degrees longitude (East): 137.4° Range to target site: 270.4 km (169.0 miles) Original image scale range: 27.1 cm/pixel (with 1 x 1 binning) so objects ~81 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 4.2° Phase angle: 57.5° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 223.9°, Northern Autumn 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. |
|
Southern Spring
PIA09668
Sol (our sun)
HiRISE
| Title |
Southern Spring |
| Original Caption Released with Image |
Click on image for larger version Southern spring sunshine is causing the seasonal carbon dioxide cap at the south pole to evaporate. This process happens fitfully, as small and large spots expose bare ground, which warms up, causing small spots to grow. The defrosting areas are controlled by small scale differences in topography, which cause some areas of frost to be sheltered longer than others. Once dust has accessed the surface it is blown in directions controlled by the local winds, making a distinctive fan. When the wind changes direction the fans broaden or may show multiple orientations. It has also been proposed that dust is carried to the top of translucent seasonal carbon dioxide ice by release of gas held under pressure by the ice cap. When the pressure is released, like pulling the cork out of a champagne bottle, the gas escapes, carrying dust with it. This is HiRISE image PSP_003193_0850 [ http://hirise.lpl.arizona.edu/PSP_003193_0850 ]. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 12:49 AM Degrees latitude (centered): -85.2° Degrees longitude (East): 180.0° Range to target site: 248.1 km (155.0 miles) Original image scale range: 49.6 cm/pixel (with 2 x 2 binning) so objects ~149 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 8.7° Phase angle: 74.8° Solar incidence angle: 82°, with the Sun about 8° above the horizon Solar longitude: 211.4°, Northern Autumn 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. |
|
Southern Spring
PIA09668
Sol (our sun)
HiRISE
| Title |
Southern Spring |
| Original Caption Released with Image |
Click on image for larger version Southern spring sunshine is causing the seasonal carbon dioxide cap at the south pole to evaporate. This process happens fitfully, as small and large spots expose bare ground, which warms up, causing small spots to grow. The defrosting areas are controlled by small scale differences in topography, which cause some areas of frost to be sheltered longer than others. Once dust has accessed the surface it is blown in directions controlled by the local winds, making a distinctive fan. When the wind changes direction the fans broaden or may show multiple orientations. It has also been proposed that dust is carried to the top of translucent seasonal carbon dioxide ice by release of gas held under pressure by the ice cap. When the pressure is released, like pulling the cork out of a champagne bottle, the gas escapes, carrying dust with it. This is HiRISE image PSP_003193_0850 [ http://hirise.lpl.arizona.edu/PSP_003193_0850 ]. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 12:49 AM Degrees latitude (centered): -85.2° Degrees longitude (East): 180.0° Range to target site: 248.1 km (155.0 miles) Original image scale range: 49.6 cm/pixel (with 2 x 2 binning) so objects ~149 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 8.7° Phase angle: 74.8° Solar incidence angle: 82°, with the Sun about 8° above the horizon Solar longitude: 211.4°, Northern Autumn 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. |
|
Southern Spring
PIA09668
Sol (our sun)
HiRISE
| Title |
Southern Spring |
| Original Caption Released with Image |
Click on image for larger version Southern spring sunshine is causing the seasonal carbon dioxide cap at the south pole to evaporate. This process happens fitfully, as small and large spots expose bare ground, which warms up, causing small spots to grow. The defrosting areas are controlled by small scale differences in topography, which cause some areas of frost to be sheltered longer than others. Once dust has accessed the surface it is blown in directions controlled by the local winds, making a distinctive fan. When the wind changes direction the fans broaden or may show multiple orientations. It has also been proposed that dust is carried to the top of translucent seasonal carbon dioxide ice by release of gas held under pressure by the ice cap. When the pressure is released, like pulling the cork out of a champagne bottle, the gas escapes, carrying dust with it. This is HiRISE image PSP_003193_0850 [ http://hirise.lpl.arizona.edu/PSP_003193_0850 ]. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 12:49 AM Degrees latitude (centered): -85.2° Degrees longitude (East): 180.0° Range to target site: 248.1 km (155.0 miles) Original image scale range: 49.6 cm/pixel (with 2 x 2 binning) so objects ~149 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 8.7° Phase angle: 74.8° Solar incidence angle: 82°, with the Sun about 8° above the horizon Solar longitude: 211.4°, Northern Autumn 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. |
|
Dark-Toned Ridges in Meridia
…
PIA09673
Sol (our sun)
HiRISE
| Title |
Dark-Toned Ridges in Meridiani |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003379_1835 [ http://hirise.lpl.arizona.edu/PSP_003379_1835 ]) is along the rim of an impact crater in Meridiani and shows a lighter-toned base unit with more resistant dark-toned ridges on top. Both units exhibit complex fracture patterns. Also evident are old dune fields that have been solidified and then fractured, as well as younger, non-solidified dune fields. More recently, the entire area has been deeply eroded by the wind. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:34 PM Degrees latitude (centered): 3.3° Degrees longitude (East): 357.1° Range to target site: 271.6 km (169.7 miles) Original image scale range: 27.2 cm/pixel (with 1 x 1 binning) so objects ~82 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.1° Phase angle: 56.3° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 220.3°, Northern Autumn 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. |
|
Dark-Toned Ridges in Meridia
…
PIA09673
Sol (our sun)
HiRISE
| Title |
Dark-Toned Ridges in Meridiani |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003379_1835 [ http://hirise.lpl.arizona.edu/PSP_003379_1835 ]) is along the rim of an impact crater in Meridiani and shows a lighter-toned base unit with more resistant dark-toned ridges on top. Both units exhibit complex fracture patterns. Also evident are old dune fields that have been solidified and then fractured, as well as younger, non-solidified dune fields. More recently, the entire area has been deeply eroded by the wind. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:34 PM Degrees latitude (centered): 3.3° Degrees longitude (East): 357.1° Range to target site: 271.6 km (169.7 miles) Original image scale range: 27.2 cm/pixel (with 1 x 1 binning) so objects ~82 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.1° Phase angle: 56.3° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 220.3°, Northern Autumn 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. |
|
Pedestal Crater in the Medus
…
PIA09676
Sol (our sun)
HiRISE
| Title |
Pedestal Crater in the Medusa Fossae Formation |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003253_1880 [ http://hirise.lpl.arizona.edu/PSP_003253_1880 ]) shows a pedestal crater located in a geologic unit on Mars called the Medusa Fossae Formation. Pedestal craters are produced by differential erosion around impact craters. If the ejecta (material thrown out of the crater) is more resistant to erosion, then the crater and surrounding ejecta will be preserved while the surface is eroded nearby. This causes the ejecta blanket surrounding the crater to form a "pedestal," standing out in relief rather than gradually merging into its surroundings. There appear to be at least two resistant layers in the material around this pedestal crater, as there are two "steps" in the topography of the pedestal. The cutout, from the long ridge near the top center of the image, shows these steps as well as possible smaller-scale layering. Despite the detail resolved by HiRISE, it is not clear why the step-forming layers are more resistant. Much of the scene is coated with a mantle of dust which obscures details. Dark slope streaks, likely produced by small avalanches in the dust, are common here. Dust deposition and erosion are also likely the reason for the scalloped texture of mantling material in the crater. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:35 PM Degrees latitude (centered): 7.7° Degrees longitude (East): 196.2° Range to target site: 276.8 km (173.0 miles) Original image scale range: 55.4 cm/pixel (with 2 x 2 binning) so objects ~166 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.1° Phase angle: 58.8° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 214.3°, Northern Autumn 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. |
|
Pedestal Crater in the Medus
…
PIA09676
Sol (our sun)
HiRISE
| Title |
Pedestal Crater in the Medusa Fossae Formation |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003253_1880 [ http://hirise.lpl.arizona.edu/PSP_003253_1880 ]) shows a pedestal crater located in a geologic unit on Mars called the Medusa Fossae Formation. Pedestal craters are produced by differential erosion around impact craters. If the ejecta (material thrown out of the crater) is more resistant to erosion, then the crater and surrounding ejecta will be preserved while the surface is eroded nearby. This causes the ejecta blanket surrounding the crater to form a "pedestal," standing out in relief rather than gradually merging into its surroundings. There appear to be at least two resistant layers in the material around this pedestal crater, as there are two "steps" in the topography of the pedestal. The cutout, from the long ridge near the top center of the image, shows these steps as well as possible smaller-scale layering. Despite the detail resolved by HiRISE, it is not clear why the step-forming layers are more resistant. Much of the scene is coated with a mantle of dust which obscures details. Dark slope streaks, likely produced by small avalanches in the dust, are common here. Dust deposition and erosion are also likely the reason for the scalloped texture of mantling material in the crater. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:35 PM Degrees latitude (centered): 7.7° Degrees longitude (East): 196.2° Range to target site: 276.8 km (173.0 miles) Original image scale range: 55.4 cm/pixel (with 2 x 2 binning) so objects ~166 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 1.1° Phase angle: 58.8° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 214.3°, Northern Autumn 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. |
|
Phoenix Lander on Mars (Ster
…
PIA09345
| Title |
Phoenix Lander on Mars (Stereo) |
| Original Caption Released with Image |
NASA's Phoenix Mars Lander monitors the atmosphere overhead and reaches out to the soil below in this stereo illustration of the spacecraft fully deployed on the surface of Mars. The image appears three-dimensional when viewed through red-green stereo glasses. Phoenix has been assembled and tested for launch in August 2007 from Cape Canaveral Air Force Station, Fla., and for landing in May or June 2008 on an arctic plain of far-northern Mars. The mission responds to evidence returned from NASA's Mars Odyssey orbiter in 2002 indicating that most high-latitude areas on Mars have frozen water mixed with soil within arm's reach of the surface. Phoenix will use a robotic arm to dig down to the expected icy layer. It will analyze scooped-up samples of the soil and ice for factors that will help scientists evaluate whether the subsurface environment at the site ever was, or may still be, a favorable habitat for microbial life. The instruments on Phoenix will also gather information to advance understanding about the history of the water in the icy layer. A weather station on the lander will conduct the first study Martian arctic weather from ground level. The vertical green line in this illustration shows how the weather station on Phoenix will use a laser beam from a lidar instrument to monitor dust and clouds in the atmosphere. The dark "wings" to either side of the lander's main body are solar panels for providing electric power. The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems, Denver. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen (Denmark), the Max Planck Institute (Germany) and the Finnish Meteorological institute. JPL is a division of the California Institute of Technology in Pasadena. |
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Depth-to-Ice Map of an Arcti
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PIA09335
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Depth-to-Ice Map of an Arctic Site on Mars |
| Original Caption Released with Image |
Color coding in this map of a far-northern site on Mars indicates the change in nighttime ground-surface temperature between summer and fall. This site, like most of high-latitude Mars, has water ice mixed with soil near the surface. The ice is probably in a rock-hard frozen layer beneath a few centimeters or inches of looser, dry soil. The amount of temperature change at the surface likely corresponds to how close to the surface the icy material lies. The dense, icy layer retains heat better than the looser soil above it, so where the icy layer is closer to the surface, the surface temperature changes more slowly than where the icy layer is buried deeper. On the map, areas of the surface that cooled more slowly between summer and autumn (interpreted as having the ice closer to the surface) are coded blue and green. Areas that cooled more quickly (interpreted as having more distance to the ice) are coded red and yellow. The depth to the top of the icy layer estimated from these observations, as little as 5 centimeters (2 inches), matches modeling of where it would be if Mars has an active cycle of water being exchanged by diffusion between atmospheric water vapor and subsurface water ice. This map and its interpretation are in a May 3, 2007, report in the journal "Nature", by Joshua Bandfield of Arizona State University, Tempe. The Thermal Emission Imaging System camera on NASA's Mars Odyssey orbiter collected the data presented in the map. The site is centered near 67.5 degrees north latitude, 132 degrees east longitude, in the Martian arctic plains called Vastitas Borealis. It was formerly a candidate landing site for NASA's Phoenix Mars Lander mission. This site is within the portion of the planet where, in 2002, the Gamma Ray Spectrometer suite of instruments on Mars Odyssey found evidence for water ice lying just below the surface. The information from the Gamma Ray Spectrometer is averaged over patches of ground hundreds of kilometers or miles wide. The information from the Thermal Emission Imaging System allows more than 100-fold higher resolution in mapping variations in the depth to ice. The Thermal Emission Imaging System observed the site in infrared wavelengths during night time, providing surface-temperature information, once on March 13, 2005, during summer in Mars' northern hemisphere, and again on April 8, 2005, during autumn there. The colors on this map signify relative differences in how much the surface temperature changed between those two observations. Blue indicates the locations with the least change. Red indicates areas with most change. Modeling provides estimates that the range of temperature changes shown in this map corresponds to a range in depth-to-ice of 5 centimeters (2 inches) to more than 18 centimeters (more than 7 inches). The sensitivity of this method for estimating the depth is not good for depths greater than about 20 centimeters (8 inches). The temperature-change data are overlaid on a mosaic of black-and-white, daytime images taken in visible-light wavelengths by the same camera, providing information about shapes in the landscape. The 10-kilometer scale bar is 6.2 miles long. NASA's Jet Propulsion Laboratory manages the Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System was developed by Arizona State University in collaboration with Raytheon Santa Barbara Remote Sensing. Lockheed Martin Space Systems, 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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Depth-to-Ice Map of a Southe
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PIA09336
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Depth-to-Ice Map of a Southern Mars Site Near Melea Planum |
| Original Caption Released with Image |
Color coding in this map of a far-southern site on Mars indicates the change in nighttime ground-surface temperature between summer and fall. This site, like most of high-latitude Mars, has water ice mixed with soil near the surface. The ice is probably in a rock-hard frozen layer beneath a few centimeters or inches of looser, dry soil. The amount of temperature change at the surface likely corresponds to how close to the surface the icy material lies. The dense, icy layer retains heat better than the looser soil above it, so where the icy layer is closer to the surface, the surface temperature changes more slowly than where the icy layer is buried deeper. On the map, areas of the surface that cooled more slowly between summer and autumn (interpreted as having the ice closer to the surface) are coded blue and green. Areas that cooled more quickly (interpreted as having more distance to the ice) are coded red and yellow. The depth to the top of the icy layer estimated from these observations suggests that in some areas, but not others, water is being exchanged by diffusion between atmospheric water vapor and subsurface water ice. Differences in what type of material lies above the ice appear to affect the depth to the ice. The area in this image with the greatest seasonal change in surface temperature corresponds to an area of sand dunes. This map and its interpretation are in a May 3, 2007, report in the journal "Nature", by Joshua Bandfield of Arizona State University, Tempe. The Thermal Emission Imaging System camera on NASA's Mars Odyssey orbiter collected the data presented in the map. The site is centered near 67 degrees south latitude, 36.5 degrees east longitude, near a plain named Melea Planum. This site is within the portion of the planet where, in 2002, the Gamma Ray Spectrometer suite of instruments on Mars Odyssey found evidence for water ice lying just below the surface. The information from the Gamma Ray Spectrometer is averaged over patches of ground hundreds of kilometers or miles wide. The information from the Thermal Emission Imaging System allows more than 100-fold higher resolution in mapping variations in the depth to ice. The Thermal Emission Imaging System observed the site in infrared wavelengths during night time, providing surface-temperature information. It did so once on Dec. 27, 2005, during late summer in Mars' southern hemisphere, and again on Jan. 22, 2006, the first day of autumn there. The colors on this map signify relative differences in how much the surface temperature changed between those two observations. Blue indicates the locations with the least change. Red indicates areas with most change. Modeling provides estimates that the range of temperature changes shown in this map corresponds to a range in depth-to-ice of less than 1 centimeter (0.4 inch) to more than 19 centimeters (more than 7.5 inches). The sensitivity of this method for estimating the depth is not good for depths greater than about 20 centimeters (8 inches). The temperature-change data are overlaid on a mosaic of black-and-white, daytime images taken in infrared wavelengths by the same camera, providing information about shapes in the landscape. The 20-kilometer scale bar is 12.4 miles long. NASA's Jet Propulsion Laboratory manages the Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University in collaboration with Raytheon Santa Barbara Remote Sensing. Lockheed Martin Space Systems, 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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