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Images of Jet Propulsion Laboratory (JPL) and California from 2007 and April 2007
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Titan 'T28' Mosaic
| Description |
Titan 'T28' Mosaic |
| Full Description |
Bright and dark terrains on Titan's trailing hemisphere are revealed by Cassini's Imaging Science Subsystem in this mosaic of images taken during the T28 flyby in April 2007. The region shown in this image, centered on the northern part of Titan's trailing hemisphere (near 31.2 degrees North, 220.7 degrees West), had only been seen at very low resolution until February 2007, when Cassini flew over this area for the first time. This mosaic consists of images taken during one of a series of flybys in early 2007 designed to study this long unavailable part of Titan (5,150 kilometers, or 3,200 miles across). Several intriguing surface features can be seen in this mosaic that warrant further study. Along the top of the mosaic is a series of dark lineaments, or linear features, that stand out against the blandness of the northern, mid-latitude terrain. These features were also observed by the RADAR instrument in December 2006 and represent an area of potential future co-analysis for the RADAR and camera teams. Another such region is the large bright area known as Adiri at bottom center, also imaged by RADAR in October 2005. The mosaic shows a number of dark areas within Adiri that line up with small dune fields observed by RADAR. A portion of the dark terrain surrounding Adiri was also observed in 2005 by RADAR, and likewise was found to consist of large stretches of longitudinal dune fields --further supporting the correlation between equatorial dark regions and dune "seas." To the east of Adiri is a dark spot surrounded by a ring of bright material, which may be associated with an impact crater similar to Sinlap, discovered earlier in the Cassini mission (see Titan Mosaic - East of Xanadu). This mosaic consists of 29 separate frames using a total of 116 images. Each frame consists of three images, taken using a filter sensitive to near-infrared light centered at 938 nanometers, allowing for observations of Titan's surface and lower atmosphere, added together. An image taken using a filter sensitive to visible light centered at 619 nanometers was then subtracted from the product, effectively removing the lower atmosphere contribution to the brightness values in the image, increasing image contrast and improving the visibility of surface features. This process is also intended to reduce noise, but some camera artifacts still remain, such as a dark ring caused by dust in the camera system near the bottom right of each frame. For a wide angle view taken during this Titan encounter, see Titan 'T28' View. The images used for this mosaic were taken on April 11, 2007 from distances ranging from 106,000 to 180,000 kilometers (66,000 to 112,000 miles). This mosaic is in an orthographic projection with a pixel scale of 1.5 kilometers (0.9 miles) per pixel, although the size of resolvable features is likely several times larger, due to atmospheric scattering. An orthographic view is most like the view seen by a distant observer looking through a, telescope. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/Space Science Institute |
| Date |
May 22, 2007 |
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The Crater Gradient
| Description |
The Crater Gradient |
| Full Description |
The Cassini spacecraft investigates the craters and deep valleys on Dione during a close approach in April 2007. Significant variations in the density of impact craters on the surface of Dione can be seen here, with more craters seen on the right side of this mosaic (on Dione's sub-Saturn hemisphere) than on the left (on Dione's anti-Saturn hemisphere). The southern end of the bright Palatine Linea fracture system can be seen near the bottom of the mosaic. Along the terminator, at lower left, part of a large impact basin can be seen. The mosaic is an orthographic projection centered at 33 degrees South, 74 degrees West, over the southern part of Dione's leading hemisphere. An orthographic view is most like the view seen by a distant observer looking through a telescope. North on Dione (1,126 kilometers, or 700 miles across) is up and rotated 6 degrees to the right. The monochrome view uses a combination of images taken with spectral filters sensitive to wavelengths of light centered at 338, 568 and 930 nanometers. The images in this mosaic were taken with the Cassini spacecraft narrow-angle camera on April 24, 2007 at a distance of approximately 121,000 kilometers (75,000 miles) from Dione and at a Sun-Dione-spacecraft, or phase, angle of 55 degrees. Image scale is 723 meters (2,371 feet) per pixel. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/Space Science Institute |
| Date |
June 6, 2007 |
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The Crater Gradient
PIA08956
Saturn
Imaging Science Subsystem -
…
| Title |
The Crater Gradient |
| Original Caption Released with Image |
The Cassini spacecraft investigates the craters and deep valleys on Dione during a close approach in April 2007. Significant variations in the density of impact craters on the surface of Dione can be seen here, with more craters seen on the right side of this mosaic (on Dione's sub-Saturn hemisphere) than on the left (on Dione's anti-Saturn hemisphere). The southern end of the bright Palatine Linea fracture system can be seen near the bottom of the mosaic. Along the terminator, at lower left, part of a large impact basin can be seen. The mosaic is an orthographic projection centered at 33 degrees South, 74 degrees West, over the southern part of Dione's leading hemisphere. An orthographic view is most like the view seen by a distant observer looking through a telescope. North on Dione (1,126 kilometers, or 700 miles across) is up and rotated 6 degrees to the right. The monochrome view uses a combination of images taken with spectral filters sensitive to wavelengths of light centered at 338, 568 and 930 nanometers. The images in this mosaic were taken with the Cassini spacecraft narrow-angle camera on April 24, 2007 at a distance of approximately 121,000 kilometers (75,000 miles) from Dione and at a Sun-Dione-spacecraft, or phase, angle of 55 degrees. Image scale is 723 meters (2,371 feet) per pixel. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov/home/index.cfm [ http://saturn.jpl.nasa.gov ]. The Cassini imaging team homepage is at http://ciclops.org [ http://ciclops.org ]. |
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Titan "T28" Mosaic
PIA08945
Saturn
Imaging Science Subsystem
| Title |
Titan "T28" Mosaic |
| Original Caption Released with Image |
. The images used for this mosaic were taken on April 11, 2007 from distances ranging from 106,000 to 180,000 kilometers (66,000 to 112,000 miles). This mosaic is in an orthographic projection with a pixel scale of 1.5 kilometers (0.9 miles) per pixel, although the size of resolvable features is likely several times larger, due to atmospheric scattering. An orthographic view is most like the view seen by a distant observer looking through a telescope. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov/home/index.cfm [ http://saturn.jpl.nasa.gov ]. The Cassini imaging team homepage is at http://ciclops.org [ http://ciclops.org ]., Bright and dark terrains on Titan's trailing hemisphere are revealed by Cassini's Imaging Science Subsystem in this mosaic of images taken during the T28 flyby in April 2007. The region shown in this image, centered on the northern part of Titan's trailing hemisphere (near 31.2 degrees North, 220.7 degrees West), had only been seen at very low resolution until February 2007, when Cassini flew over this area for the first time. This mosaic consists of images taken during one of a series of flybys in early 2007 designed to study this long unavailable part of Titan (5,150 kilometers, or 3,200 miles across). Several intriguing surface features can be seen in this mosaic that warrant further study. Along the top of the mosaic is a series of dark lineaments, or linear features, that stand out against the blandness of the northern, mid-latitude terrain. These features were also observed by the RADAR instrument in December 2006 and represent an area of potential future co-analysis for the RADAR and camera teams. Another such region is the large bright area known as Adiri at bottom center, also imaged by RADAR in October 2005. The mosaic shows a number of dark areas within Adiri that line up with small dune fields observed by RADAR. A portion of the dark terrain surrounding Adiri was also observed in 2005 by RADAR, and likewise was found to consist of large stretches of longitudinal dune fields -- further supporting the correlation between equatorial dark regions and dune "seas." To the east of Adiri is a dark spot surrounded by a ring of bright material, which may be associated with an impact crater similar to Sinlap, discovered earlier in the Cassini mission (see PIA6222 [ http://photojournal.jpl.nasa.gov/catalog/PIA06222 ]). This mosaic consists of 29 separate frames using a total of 116 images. Each frame consists of three images, taken using a filter sensitive to near-infrared light centered at 938 nanometers, allowing for observations of Titan's surface and lower atmosphere, added together. An image taken using a filter sensitive to visible light centered at 619 nanometers was then subtracted from the product, effectively removing the lower atmosphere contribution to the brightness values in the image, increasing image contrast and improving the visibility of surface features.This process is also intended to reduce noise, but some camera artifacts still remain, such as a dark ring caused by dust in the camera system near the bottom right of each frame. For a wide angle view taken during this Titan encounter, see PIA8943 [ http://photojournal.jpl.nasa.gov/catalog/PIA08943 ] |
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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
…
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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Evros Vallis and Nearby Crat
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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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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. |
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Dark Slope Streak with Strea
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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. |
|
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. |
|
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. |
|
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. |
|
Dust Fans on the Seasonal Ca
…
PIA09660
Sol (our sun)
HiRISE
| Title |
Dust Fans on the Seasonal Carbon Dioxide Polar Cap |
| Original Caption Released with Image |
Click on image for larger version During the long dark night of Martian winter at the south pole, carbon dioxide (CO2) in its solid form (also known as "dry ice") accumulates and forms a seasonal polar cap. HiRISE is currently observing southern spring on Mars. As the sun comes up in the spring, the ice evaporates in a complex way. HiRISE image PSP_003180_0945 [ http://hirise.lpl.arizona.edu/PSP_003180_0945 ] shows dark dust being blown across the seasonal south polar cap. The dust comes from the surface beneath the ice: it either starts at spots bare of ice, or it's possible that it's lofted from below the ice in geyser-like plumes. Local winds blow the dust from its source, forming a long fan. When the wind changes direction, a new fan is formed, pointing in the new direction (see subimage 2, full resolution, approx. 800 meters [1/2 mile] across). In this single image we can see that the wind has blown in a number of directions (see subimage 1, not full resolution, approx. 4 km [2.5 miles] across). This data will be used to study weather patterns near the south pole. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 8:08 PM Degrees latitude (centered): -85.4° Degrees longitude (East): 104.1° Range to target site: 264.4 km (165.2 miles) Original image scale range: 52.9 cm/pixel (with 2 x 2 binning) so objects ~159 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 22.5° Phase angle: 61.9° Solar incidence angle: 80°, with the Sun about 10° above the horizon Solar longitude: 210.8°, 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. |
|
Dust Fans on the Seasonal Ca
…
PIA09660
Sol (our sun)
HiRISE
| Title |
Dust Fans on the Seasonal Carbon Dioxide Polar Cap |
| Original Caption Released with Image |
Click on image for larger version During the long dark night of Martian winter at the south pole, carbon dioxide (CO2) in its solid form (also known as "dry ice") accumulates and forms a seasonal polar cap. HiRISE is currently observing southern spring on Mars. As the sun comes up in the spring, the ice evaporates in a complex way. HiRISE image PSP_003180_0945 [ http://hirise.lpl.arizona.edu/PSP_003180_0945 ] shows dark dust being blown across the seasonal south polar cap. The dust comes from the surface beneath the ice: it either starts at spots bare of ice, or it's possible that it's lofted from below the ice in geyser-like plumes. Local winds blow the dust from its source, forming a long fan. When the wind changes direction, a new fan is formed, pointing in the new direction (see subimage 2, full resolution, approx. 800 meters [1/2 mile] across). In this single image we can see that the wind has blown in a number of directions (see subimage 1, not full resolution, approx. 4 km [2.5 miles] across). This data will be used to study weather patterns near the south pole. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 8:08 PM Degrees latitude (centered): -85.4° Degrees longitude (East): 104.1° Range to target site: 264.4 km (165.2 miles) Original image scale range: 52.9 cm/pixel (with 2 x 2 binning) so objects ~159 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 22.5° Phase angle: 61.9° Solar incidence angle: 80°, with the Sun about 10° above the horizon Solar longitude: 210.8°, 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. |
|
Dust Fans on the Seasonal Ca
…
PIA09660
Sol (our sun)
HiRISE
| Title |
Dust Fans on the Seasonal Carbon Dioxide Polar Cap |
| Original Caption Released with Image |
Click on image for larger version During the long dark night of Martian winter at the south pole, carbon dioxide (CO2) in its solid form (also known as "dry ice") accumulates and forms a seasonal polar cap. HiRISE is currently observing southern spring on Mars. As the sun comes up in the spring, the ice evaporates in a complex way. HiRISE image PSP_003180_0945 [ http://hirise.lpl.arizona.edu/PSP_003180_0945 ] shows dark dust being blown across the seasonal south polar cap. The dust comes from the surface beneath the ice: it either starts at spots bare of ice, or it's possible that it's lofted from below the ice in geyser-like plumes. Local winds blow the dust from its source, forming a long fan. When the wind changes direction, a new fan is formed, pointing in the new direction (see subimage 2, full resolution, approx. 800 meters [1/2 mile] across). In this single image we can see that the wind has blown in a number of directions (see subimage 1, not full resolution, approx. 4 km [2.5 miles] across). This data will be used to study weather patterns near the south pole. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 8:08 PM Degrees latitude (centered): -85.4° Degrees longitude (East): 104.1° Range to target site: 264.4 km (165.2 miles) Original image scale range: 52.9 cm/pixel (with 2 x 2 binning) so objects ~159 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 22.5° Phase angle: 61.9° Solar incidence angle: 80°, with the Sun about 10° above the horizon Solar longitude: 210.8°, 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. |
|
Dust Fans on the Seasonal Ca
…
PIA09660
Sol (our sun)
HiRISE
| Title |
Dust Fans on the Seasonal Carbon Dioxide Polar Cap |
| Original Caption Released with Image |
Click on image for larger version During the long dark night of Martian winter at the south pole, carbon dioxide (CO2) in its solid form (also known as "dry ice") accumulates and forms a seasonal polar cap. HiRISE is currently observing southern spring on Mars. As the sun comes up in the spring, the ice evaporates in a complex way. HiRISE image PSP_003180_0945 [ http://hirise.lpl.arizona.edu/PSP_003180_0945 ] shows dark dust being blown across the seasonal south polar cap. The dust comes from the surface beneath the ice: it either starts at spots bare of ice, or it's possible that it's lofted from below the ice in geyser-like plumes. Local winds blow the dust from its source, forming a long fan. When the wind changes direction, a new fan is formed, pointing in the new direction (see subimage 2, full resolution, approx. 800 meters [1/2 mile] across). In this single image we can see that the wind has blown in a number of directions (see subimage 1, not full resolution, approx. 4 km [2.5 miles] across). This data will be used to study weather patterns near the south pole. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 8:08 PM Degrees latitude (centered): -85.4° Degrees longitude (East): 104.1° Range to target site: 264.4 km (165.2 miles) Original image scale range: 52.9 cm/pixel (with 2 x 2 binning) so objects ~159 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: POLAR STEREOGRAPHIC Emission angle: 22.5° Phase angle: 61.9° Solar incidence angle: 80°, with the Sun about 10° above the horizon Solar longitude: 210.8°, 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. |
|
Popular Landform in Cydonia
…
PIA09654
Sol (our sun)
HiRISE
| Title |
Popular Landform in Cydonia Region |
| Original Caption Released with Image |
Click on image for larger version HiRISE captured this image (PSP_003234_2210 [ http://hirise.lpl.arizona.edu/PSP_003234_2210 ]) of an eroded mesa made famous by its similarity to a human face in a Viking Orbiter image with much lower spatial resolution and a different lighting geometry. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 40.7° Degrees longitude (East): 350.5° Range to target site: 299.4 km (187.1 miles) Original image scale range: 29.9 cm/pixel (with 1 x 1 binning) so objects ~90 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.3° Phase angle: 72.8° Solar incidence angle: 73°, with the Sun about 17° above the horizon Solar longitude: 213.4°, 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. |
|
Popular Landform in Cydonia
…
PIA09654
Sol (our sun)
HiRISE
| Title |
Popular Landform in Cydonia Region |
| Original Caption Released with Image |
Click on image for larger version HiRISE captured this image (PSP_003234_2210 [ http://hirise.lpl.arizona.edu/PSP_003234_2210 ]) of an eroded mesa made famous by its similarity to a human face in a Viking Orbiter image with much lower spatial resolution and a different lighting geometry. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 40.7° Degrees longitude (East): 350.5° Range to target site: 299.4 km (187.1 miles) Original image scale range: 29.9 cm/pixel (with 1 x 1 binning) so objects ~90 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.3° Phase angle: 72.8° Solar incidence angle: 73°, with the Sun about 17° above the horizon Solar longitude: 213.4°, 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. |
|
Proposed MSL Site in West Ca
…
PIA09708
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in West Candor |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003263_1740 [ http://hirise.lpl.arizona.edu/PSP_003263_1740 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in West Candor. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:35 PM Degrees latitude (centered): -5.8° Degrees longitude (East): 284.2° Range to target site: 265.3 km (165.8 miles) Original image scale range: 26.5 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: 9.5° Phase angle: 63.1° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 214.8°, 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 West Ca
…
PIA09708
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in West Candor |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003263_1740 [ http://hirise.lpl.arizona.edu/PSP_003263_1740 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in West Candor. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:35 PM Degrees latitude (centered): -5.8° Degrees longitude (East): 284.2° Range to target site: 265.3 km (165.8 miles) Original image scale range: 26.5 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: 9.5° Phase angle: 63.1° Solar incidence angle: 54°, with the Sun about 36° above the horizon Solar longitude: 214.8°, 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. |
|
Gullies and Dunes in a Crate
…
PIA09706
Sol (our sun)
HiRISE
| Title |
Gullies and Dunes in a Crater in Newton Basin |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003464_1380 [ http://hirise.lpl.arizona.edu/PSP_003464_1380 ]) is a spectacular image showing gullies associated with distinct layers located at multiple elevations along one crater wall as well as multiple generations of dunes that are eroding or covering a more coherent rock structure. The gullies in this crater appear to originate at the layers that cover a large extent of the slope. On the left side of the image, gullies can be seen emanating from layers in two distinct sets, each at a different elevation. Gullies are often, but not always, form near layers. Many of the gullies seen here have sinuous, or wavy, channels. The bends are called meanders, and on Earth, meanders form in streams that have sustained and/or repeated flow. Not all of the gullies seen in this image extend the same distance downslope. This could result from differences in water supply, sediment supply, slope angle, and time of formation, among other factors. Dunes are also visible in this image, they indicate the prevailing wind direction. What is particularly interesting about this dune field is that there is exposed rock in the middle of it. This rock is either being exposed as the wind moves the dunes away from it or it is being covered. The dunes appear to outline the shape of the rock, which suggests that the rock has been uncovered long enough for dunes to form around it. As the dunes shift over time, they will probably expose more of the underlying rock. The subimage (~1 km across) shows several generations of dunes interacting with the protruding rock. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -41.5° Degrees longitude (East): 202.1° Range to target site: 254.3 km (158.9 miles) Original image scale range: 50.9 cm/pixel (with 2 x 2 binning) so objects ~153 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.2° Phase angle: 54.8° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 224.5°, 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. |
|
Gullies and Dunes in a Crate
…
PIA09706
Sol (our sun)
HiRISE
| Title |
Gullies and Dunes in a Crater in Newton Basin |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003464_1380 [ http://hirise.lpl.arizona.edu/PSP_003464_1380 ]) is a spectacular image showing gullies associated with distinct layers located at multiple elevations along one crater wall as well as multiple generations of dunes that are eroding or covering a more coherent rock structure. The gullies in this crater appear to originate at the layers that cover a large extent of the slope. On the left side of the image, gullies can be seen emanating from layers in two distinct sets, each at a different elevation. Gullies are often, but not always, form near layers. Many of the gullies seen here have sinuous, or wavy, channels. The bends are called meanders, and on Earth, meanders form in streams that have sustained and/or repeated flow. Not all of the gullies seen in this image extend the same distance downslope. This could result from differences in water supply, sediment supply, slope angle, and time of formation, among other factors. Dunes are also visible in this image, they indicate the prevailing wind direction. What is particularly interesting about this dune field is that there is exposed rock in the middle of it. This rock is either being exposed as the wind moves the dunes away from it or it is being covered. The dunes appear to outline the shape of the rock, which suggests that the rock has been uncovered long enough for dunes to form around it. As the dunes shift over time, they will probably expose more of the underlying rock. The subimage (~1 km across) shows several generations of dunes interacting with the protruding rock. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -41.5° Degrees longitude (East): 202.1° Range to target site: 254.3 km (158.9 miles) Original image scale range: 50.9 cm/pixel (with 2 x 2 binning) so objects ~153 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.2° Phase angle: 54.8° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 224.5°, 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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Gullies and Dunes in a Crate
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PIA09706
Sol (our sun)
HiRISE
| Title |
Gullies and Dunes in a Crater in Newton Basin |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003464_1380 [ http://hirise.lpl.arizona.edu/PSP_003464_1380 ]) is a spectacular image showing gullies associated with distinct layers located at multiple elevations along one crater wall as well as multiple generations of dunes that are eroding or covering a more coherent rock structure. The gullies in this crater appear to originate at the layers that cover a large extent of the slope. On the left side of the image, gullies can be seen emanating from layers in two distinct sets, each at a different elevation. Gullies are often, but not always, form near layers. Many of the gullies seen here have sinuous, or wavy, channels. The bends are called meanders, and on Earth, meanders form in streams that have sustained and/or repeated flow. Not all of the gullies seen in this image extend the same distance downslope. This could result from differences in water supply, sediment supply, slope angle, and time of formation, among other factors. Dunes are also visible in this image, they indicate the prevailing wind direction. What is particularly interesting about this dune field is that there is exposed rock in the middle of it. This rock is either being exposed as the wind moves the dunes away from it or it is being covered. The dunes appear to outline the shape of the rock, which suggests that the rock has been uncovered long enough for dunes to form around it. As the dunes shift over time, they will probably expose more of the underlying rock. The subimage (~1 km across) shows several generations of dunes interacting with the protruding rock. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:40 PM Degrees latitude (centered): -41.5° Degrees longitude (East): 202.1° Range to target site: 254.3 km (158.9 miles) Original image scale range: 50.9 cm/pixel (with 2 x 2 binning) so objects ~153 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.2° Phase angle: 54.8° Solar incidence angle: 53°, with the Sun about 37° above the horizon Solar longitude: 224.5°, 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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Blocks in the Olympus Mons
PIA09713
Sol (our sun)
HiRISE
| Title |
Blocks in the Olympus Mons |
| Original Caption Released with Image |
Click on image for larger version The aureole that surrounds the western and northern sectors of Olympus Mons has puzzled Mars geologists. The most common idea is that these deposits formed as giant land slides as the volcano partially collapsed under its own weight. This HiRISE image (PSP_003450_1975 [ http://hirise.lpl.arizona.edu/PSP_003450_1975 ]) is centered on a dark and relatively dust-free part of the aureole. Where the dust has been stripped off, swirling bands of darker and lighter rocks are visibile. These suggest gently warped layers that have been exposed by erosion. In fact, many of the small pinnacles and mesas in this area are being eroded by the wind in the same way as layered deposits in other parts of Mars. However, there are also blocks that shed dark material, that could be broken up lava rock. The many dunes in the area suggest that much of the debris is sand sized. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 17.4° Degrees longitude (East): 216.7° Range to target site: 280.7 km (175.5 miles) Original image scale range: 28.1 cm/pixel (with 1 x 1 binning) so objects ~84 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.9° Phase angle: 64.6° Solar incidence angle: 62°, with the Sun about 28° above the horizon Solar longitude: 223.8°, 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. |
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Blocks in the Olympus Mons
PIA09713
Sol (our sun)
HiRISE
| Title |
Blocks in the Olympus Mons |
| Original Caption Released with Image |
Click on image for larger version The aureole that surrounds the western and northern sectors of Olympus Mons has puzzled Mars geologists. The most common idea is that these deposits formed as giant land slides as the volcano partially collapsed under its own weight. This HiRISE image (PSP_003450_1975 [ http://hirise.lpl.arizona.edu/PSP_003450_1975 ]) is centered on a dark and relatively dust-free part of the aureole. Where the dust has been stripped off, swirling bands of darker and lighter rocks are visibile. These suggest gently warped layers that have been exposed by erosion. In fact, many of the small pinnacles and mesas in this area are being eroded by the wind in the same way as layered deposits in other parts of Mars. However, there are also blocks that shed dark material, that could be broken up lava rock. The many dunes in the area suggest that much of the debris is sand sized. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 17.4° Degrees longitude (East): 216.7° Range to target site: 280.7 km (175.5 miles) Original image scale range: 28.1 cm/pixel (with 1 x 1 binning) so objects ~84 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.9° Phase angle: 64.6° Solar incidence angle: 62°, with the Sun about 28° above the horizon Solar longitude: 223.8°, 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. |
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Proposed MSL Site in East Me
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PIA09707
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in East Meridiani |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003326_1800 [ http://hirise.lpl.arizona.edu/PSP_003326_1800 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in East Meridiani. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:33 PM Degrees latitude (centered): 0.0° Degrees longitude (East): 3.6° Range to target site: 273.6 km (171.0 miles) Original image scale range: 27.4 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: 9.4° Phase angle: 64.0° Solar incidence angle: 55°, with the Sun about 35° above the horizon Solar longitude: 217.8 °, 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. |
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