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Iapetus' Equatorial Region -
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| Description |
Iapetus' Equatorial Region -- Labeled |
| Full Description |
Cassini made a close flyby of Saturn's moon Iapetus on Sept. 10, 2007, and the visual and infrared mapping spectrometer obtained these images during that event. These two images show a higher resolution version of the equatorial region shown in Tiny Grains on Iapetus. The equatorial region includes the equatorial bulge which shows no differences in these compositions compared to surrounding regions. The color image on the right shows the results of mapping for three components of Iapetus' surface: carbon dioxide that is trapped or adsorbed in the surface (red), water in the form of ice (green), and a newly-discovered effect due to trace amount of dark particles in the ice creating what scientists call Rayleigh scattering (blue). The Rayleigh scattering effect is the main reason why the Earth's sky appears blue. There is a complex transition zone from the dark region, on the right, which is high in carbon dioxide, to the more ice-rich region on the left. Some crater floors are filled with carbon dioxide-rich dark material. As the ice becomes cleaner to the left, the small dark particles become more scattered and increase the Rayleigh scattering effect, again indicative of less than 2 percent dark sub-0.5-micron particles. The visual and infrared mapping spectrometer is like a digital camera, but instead of using three colors, it makes images in 352 colors, or wavelengths, from the ultraviolet to the near-infrared. The many wavelengths produce a continuous spectrum in each pixel, and these spectra measure how light is absorbed by different materials. By analyzing the absorptions expressed in each pixel, a map of the composition at each location on the moon can be constructed. 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 was designed, developed and assembled at JPL. The Visual and Infrared Mapping Spectrometer team is based at the University of Arizona. For more information about the Cassini-Huygens mission, visit: http://saturn.jpl.nasa.gov/home/index.cfm. The visual and infrared mapping spectrometer team home page is at: http://wwwvims.lpl.arizona.edu. Credit: NASA/JPL/University of Arizona /USGS |
| Date |
October 8, 2007 |
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Hubble Images of Asteroids H
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| Title |
Hubble Images of Asteroids Help Astronomers Prepare for Spacecraft Visit |
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Hubble Images of Asteroids H
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| Title |
Hubble Images of Asteroids Help Astronomers Prepare for Spacecraft Visit |
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Hubble Images of Asteroids H
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| Title |
Hubble Images of Asteroids Help Astronomers Prepare for Spacecraft Visit |
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Layers in Galle Crater
PIA09686
Sol (our sun)
HiRISE
| Title |
Layers in Galle Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image shows part of a large mass of layered rock in Galle Crater, in the southern cratered highlands of Mars. At low resolution, layers appear as bands and swirls which are nearly horizontal. This causes them to interact dramatically with topography, producing the appearance of folds and loops wrapping around small hills much like lines on a contour map. Zooming in at higher resolution, some long cracks (hundreds of meters long) are cutting across the layers, generally trending northeast-southwest. At full resolution (PSP_002655_1280 [ http://hirise.lpl.arizona.edu/PSP_002655_1280 ]), details of the layers are often obscured by ripples of wind-blown dust or textured patterns of erosion now eroding the rock. In the best exposures, such as that in the cutout section, the layers are fractured into blocks. Some of the layers are relatively resistant, and appear as ridges or fins in the cutout, often with little material supporting them from below. Although this seems to indicate relatively strong, coherent material, few boulders are visible. The ridge-forming layers may be weak, but separated by material with virtually no cohesion. Polygonal fracture patterns in the dark regolith between distinct layers could be due to ground ice, or regional tectonic stresses. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:54 PM Degrees latitude (centered): -51.8° Degrees longitude (East): 330.0° Range to target site: 256.3 km (160.2 miles) Original image scale range: 25.6 cm/pixel (with 1 x 1 binning) so objects ~77 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.8° Phase angle: 71.5° Solar incidence angle: 69°, with the Sun about 21° above the horizon Solar longitude: 186.6°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
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Layers in Galle Crater
PIA09686
Sol (our sun)
HiRISE
| Title |
Layers in Galle Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image shows part of a large mass of layered rock in Galle Crater, in the southern cratered highlands of Mars. At low resolution, layers appear as bands and swirls which are nearly horizontal. This causes them to interact dramatically with topography, producing the appearance of folds and loops wrapping around small hills much like lines on a contour map. Zooming in at higher resolution, some long cracks (hundreds of meters long) are cutting across the layers, generally trending northeast-southwest. At full resolution (PSP_002655_1280 [ http://hirise.lpl.arizona.edu/PSP_002655_1280 ]), details of the layers are often obscured by ripples of wind-blown dust or textured patterns of erosion now eroding the rock. In the best exposures, such as that in the cutout section, the layers are fractured into blocks. Some of the layers are relatively resistant, and appear as ridges or fins in the cutout, often with little material supporting them from below. Although this seems to indicate relatively strong, coherent material, few boulders are visible. The ridge-forming layers may be weak, but separated by material with virtually no cohesion. Polygonal fracture patterns in the dark regolith between distinct layers could be due to ground ice, or regional tectonic stresses. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:54 PM Degrees latitude (centered): -51.8° Degrees longitude (East): 330.0° Range to target site: 256.3 km (160.2 miles) Original image scale range: 25.6 cm/pixel (with 1 x 1 binning) so objects ~77 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.8° Phase angle: 71.5° Solar incidence angle: 69°, with the Sun about 21° above the horizon Solar longitude: 186.6°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
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Evros Vallis and Nearby Crat
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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
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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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Layered Deposits in Ritchey
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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. |
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Layered Deposits in Ritchey
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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. |
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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. |
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Proposed MSL Site in Eberswa
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PIA09678
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Eberswalde Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003231_2095 [ http://hirise.lpl.arizona.edu/PSP_003231_2095 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Eberswalde Crater. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 29.3° Degrees longitude (East): 73.3° Range to target site: 290.3 km (181.4 miles) Original image scale range: 29.0 cm/pixel (with 1 x 1 binning) so objects ~87 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 8.0° Phase angle: 73.5° Solar incidence angle: 66°, with the Sun about 24° above the horizon Solar longitude: 213.3°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
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Proposed MSL Site in Eberswa
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PIA09678
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Eberswalde Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_003231_2095 [ http://hirise.lpl.arizona.edu/PSP_003231_2095 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Eberswalde Crater. Observation Toolbox Acquisition date: 4 April 2007 Local Mars time: 3:28 PM Degrees latitude (centered): 29.3° Degrees longitude (East): 73.3° Range to target site: 290.3 km (181.4 miles) Original image scale range: 29.0 cm/pixel (with 1 x 1 binning) so objects ~87 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 8.0° Phase angle: 73.5° Solar incidence angle: 66°, with the Sun about 24° above the horizon Solar longitude: 213.3°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
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Alluvial Fan Along a Crater
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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. |
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Alluvial Fan Along a Crater
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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. |
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Kaiser Crater Dune Field
PIA09669
Sol (our sun)
HiRISE
| Title |
Kaiser Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003141_1330 [ http://hirise.lpl.arizona.edu/PSP_003141_1330 ]) shows a sand dune field in Kaiser Crater, a 210 km (130 miles) wide impact basin in the Hellespontus region of Mars. Winds have trapped massive quantities of sand on the floors of broad craters in this region. The steepest slopes on each dune, the slip faces, point to the east indicating that the dominant wind direction in this part of the dune field is from west to east. Patches of seasonal frost can be seen in the low areas between the dunes. The subimage reveals smaller secondary dunes superimposed on the surface of the large dunes and even smaller ripples that appear between and perpendicular to the secondary dunes. Avalanching or mass movement of sand has left deep scars on the slip face of the large dune in the upper left portion of the subimage. This may indicate that the sand is not loose but is weakly cemented. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -46.6° Degrees longitude (East): 19.3° Range to target site: 263.9 km (164.9 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 17.5° Phase angle: 74.6° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 209.0°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
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Kaiser Crater Dune Field
PIA09669
Sol (our sun)
HiRISE
| Title |
Kaiser Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003141_1330 [ http://hirise.lpl.arizona.edu/PSP_003141_1330 ]) shows a sand dune field in Kaiser Crater, a 210 km (130 miles) wide impact basin in the Hellespontus region of Mars. Winds have trapped massive quantities of sand on the floors of broad craters in this region. The steepest slopes on each dune, the slip faces, point to the east indicating that the dominant wind direction in this part of the dune field is from west to east. Patches of seasonal frost can be seen in the low areas between the dunes. The subimage reveals smaller secondary dunes superimposed on the surface of the large dunes and even smaller ripples that appear between and perpendicular to the secondary dunes. Avalanching or mass movement of sand has left deep scars on the slip face of the large dune in the upper left portion of the subimage. This may indicate that the sand is not loose but is weakly cemented. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -46.6° Degrees longitude (East): 19.3° Range to target site: 263.9 km (164.9 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 17.5° Phase angle: 74.6° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 209.0°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
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Kaiser Crater Dune Field
PIA09669
Sol (our sun)
HiRISE
| Title |
Kaiser Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_003141_1330 [ http://hirise.lpl.arizona.edu/PSP_003141_1330 ]) shows a sand dune field in Kaiser Crater, a 210 km (130 miles) wide impact basin in the Hellespontus region of Mars. Winds have trapped massive quantities of sand on the floors of broad craters in this region. The steepest slopes on each dune, the slip faces, point to the east indicating that the dominant wind direction in this part of the dune field is from west to east. Patches of seasonal frost can be seen in the low areas between the dunes. The subimage reveals smaller secondary dunes superimposed on the surface of the large dunes and even smaller ripples that appear between and perpendicular to the secondary dunes. Avalanching or mass movement of sand has left deep scars on the slip face of the large dune in the upper left portion of the subimage. This may indicate that the sand is not loose but is weakly cemented. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -46.6° Degrees longitude (East): 19.3° Range to target site: 263.9 km (164.9 miles) Original image scale range: 26.4 cm/pixel (with 1 x 1 binning) so objects ~79 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 17.5° Phase angle: 74.6° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 209.0°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
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. |
|
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. |
|
Surveying the Scene Above Op
…
PIA09687
Sol (our sun)
HiRISE, Panoramic Camera
| Title |
Surveying the Scene Above Opportunity (Simulation) |
| Original Caption Released with Image |
"" Click on the image to view the animation""Lower resolution animation This animation shows a hypothetical flyover above Victoria Crater, where NASA's Mars Exploration Rover Opportunity is perched on a rim. The rover is expected to begin rolling down into the crater in early July 2007. The first part of the movie is based on data taken by the Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment camera. A simulated rover is shown at the site where Opportunity will enter the crater, an alcove nicknamed "Duck Bay." The movie then transitions to a panoramic view of Victoria Crater taken from the top of Duck Bay by Opportunity's panoramic camera. |
|
Surveying the Scene Above Op
…
PIA09687
Sol (our sun)
HiRISE, Panoramic Camera
| Title |
Surveying the Scene Above Opportunity (Simulation) |
| Original Caption Released with Image |
"" Click on the image to view the animation""Lower resolution animation This animation shows a hypothetical flyover above Victoria Crater, where NASA's Mars Exploration Rover Opportunity is perched on a rim. The rover is expected to begin rolling down into the crater in early July 2007. The first part of the movie is based on data taken by the Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment camera. A simulated rover is shown at the site where Opportunity will enter the crater, an alcove nicknamed "Duck Bay." The movie then transitions to a panoramic view of Victoria Crater taken from the top of Duck Bay by Opportunity's panoramic camera. |
|
Opportunity's Long Road to V
…
PIA09689
Sol (our sun)
HiRISE, Mars Orbiter Camera
| Title |
Opportunity's Long Road to Victoria (Animation) |
| Original Caption Released with Image |
"" Click on the image to view the animation""Lower resolution animation This movie maps out the travels of NASA's Mars Exploration Rover Opportunity, from is landing site at Eagle Crater to the rim of Victoria Crater about six miles (9.7 kilometers) away. The rover, which landed on the red planet more than three years ago, spent 21 months trekking across the plains of Meridiani Planum from Endurance Crater to reach Victoria Crater on sol 951 (Sept. 26, 2006). Victoria is the largest crater encountered by Opportunity yet, at 800 meters (half a mile) across. Once there, the rover began to explore the rim of the crater, working around its sharp cliffs and gentle bays in a clockwise direction. It examined the cliffs' rock layers visible from rim viewpoints and it assessed the bays for a possible entry route. Opportunity then headed back to its original arrival point at Victoria, an alcove informally named "Duck Bay," where it is expected to roll into the crater in early July 2007. The images making up the first map in this movie are from the Mars Observer Camera on NASA's Mars Global Surveyor, while the second map uses an image from the High Resolution Imaging Science Experiment on NASA's Mars Reconnaissance Orbiter. |
|
Opportunity's Long Road to V
…
PIA09689
Sol (our sun)
HiRISE, Mars Orbiter Camera
| Title |
Opportunity's Long Road to Victoria (Animation) |
| Original Caption Released with Image |
"" Click on the image to view the animation""Lower resolution animation This movie maps out the travels of NASA's Mars Exploration Rover Opportunity, from is landing site at Eagle Crater to the rim of Victoria Crater about six miles (9.7 kilometers) away. The rover, which landed on the red planet more than three years ago, spent 21 months trekking across the plains of Meridiani Planum from Endurance Crater to reach Victoria Crater on sol 951 (Sept. 26, 2006). Victoria is the largest crater encountered by Opportunity yet, at 800 meters (half a mile) across. Once there, the rover began to explore the rim of the crater, working around its sharp cliffs and gentle bays in a clockwise direction. It examined the cliffs' rock layers visible from rim viewpoints and it assessed the bays for a possible entry route. Opportunity then headed back to its original arrival point at Victoria, an alcove informally named "Duck Bay," where it is expected to roll into the crater in early July 2007. The images making up the first map in this movie are from the Mars Observer Camera on NASA's Mars Global Surveyor, while the second map uses an image from the High Resolution Imaging Science Experiment on NASA's Mars Reconnaissance Orbiter. |
|
Another Apollinaris
PIA09986
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Another Apollinaris |
| Original Caption Released with Image |
Context image for PIA09986 Another Apollinaris The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Today's image shows the southwestern flank of the volcano. Image information: VIS instrument. Latitude -9.2N, Longitude 173.5E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Another Apollinaris
PIA09986
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Another Apollinaris |
| Original Caption Released with Image |
Context image for PIA09986 Another Apollinaris The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Today's image shows the southwestern flank of the volcano. Image information: VIS instrument. Latitude -9.2N, Longitude 173.5E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Final Apollinaris
PIA09987
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Final Apollinaris |
| Original Caption Released with Image |
Context image for PIA09987 Final Apollinaris The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Today's image shows the northwestern edge of the summit caldera. Image information: VIS instrument. Latitude -8.3N, Longitude 173.6E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Final Apollinaris
PIA09987
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Final Apollinaris |
| Original Caption Released with Image |
Context image for PIA09987 Final Apollinaris The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Today's image shows the northwestern edge of the summit caldera. Image information: VIS instrument. Latitude -8.3N, Longitude 173.6E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Apollinaris Patera
PIA09984
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Apollinaris Patera |
| Original Caption Released with Image |
Context image for PIA09984 Apollinaris Patera The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Today's image is of the eroded southeastern flank of the volcano. Image information: VIS instrument. Latitude -9.7N, Longitude 175.1E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Apollinaris Patera
PIA09984
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Apollinaris Patera |
| Original Caption Released with Image |
Context image for PIA09984 Apollinaris Patera The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Today's image is of the eroded southeastern flank of the volcano. Image information: VIS instrument. Latitude -9.7N, Longitude 175.1E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
More Apollinaris
PIA09985
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
More Apollinaris |
| Original Caption Released with Image |
Context image for PIA09985 More Apollinaris The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Today's image shows the boundary between the base of the volcano and the wind eroded materials located NNW of Apollinaris Patera. Image information: VIS instrument. Latitude -7.6N, Longitude 173.0E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
More Apollinaris
PIA09985
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
More Apollinaris |
| Original Caption Released with Image |
Context image for PIA09985 More Apollinaris The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Today's image shows the boundary between the base of the volcano and the wind eroded materials located NNW of Apollinaris Patera. Image information: VIS instrument. Latitude -7.6N, Longitude 173.0E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Apollinaris Patera
PIA09983
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Apollinaris Patera |
| Original Caption Released with Image |
Context image for PIA09983 Apollinaris Patera The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Part of the summit caldera is shown in this image. Image information: VIS instrument. Latitude -8.6N, Longitude 174.0E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Apollinaris Patera
PIA09983
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Apollinaris Patera |
| Original Caption Released with Image |
Context image for PIA09983 Apollinaris Patera The major Martian dust storm of 2007 filled the sky with dust and produced conditions that prevented the THEMIS VIS camera from being able to image the surface. With no new images being acquired, we've dug into the archive to highlight some interesting areas on Mars. The this week's region is Apollinaris Patera. Apollinaris Patera is an old volcano that has undergone extensive erosion. This volcano is located north of Gusev Crater, the home of the rover called Spirit. Part of the summit caldera is shown in this image. Image information: VIS instrument. Latitude -8.6N, Longitude 174.0E. 18 meter/pixel resolution. Please see the THEMIS Data Citation Note [ http://themis.la.asu.edu/terms ] for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
|
Aram Chaos Sediments
PIA09624
Sol (our sun)
HiRISE
| Title |
Aram Chaos Sediments |
| Original Caption Released with Image |
Click on image for larger version Aram Chaos appears to be a former impact crater. The terrain is disrupted, giving it a chaotic appearance (hence the name "chaos"). Scientists have postulated that a lake may have once existed inside the crater and sediments were laid down within the lake. The mineral hematite (rich in iron) has been detected by orbiting spacecraft within Aram Chaos. Hematite has been identified in several other locations on Mars, including at the Mars Exploration Rover landing site in Meridiani Planum. The hematite at both Meridiani and Aram Chaos most likely formed by precipitation in water. This HiRISE image (PSP_002839_1825 [ http://hirise.lpl.arizona.edu/PSP_002839_1825 ]) shows the light-toned sediments inside Aram Chaos that could have formed in a former lake. Unfortunately, dark debris now obscures much of this sediment, making it difficult to view and interpret the rocks. The light-toned layered deposit in the south (bottom) of the image is higher standing and has a pitted surface. Circular structures with dark centers are likely to be impact craters that have been partly filled with dark debris, including sand. More irregular depressions appear to result from erosion of layered beds within the sediments. Wind could erode materials that are slightly weaker more quickly and produce the irregular topography seen along the surface of the deposit. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:41 PM Degrees latitude (centered): 2.7° Degrees longitude (East): 339.3° Range to target site: 272.3 km (170.2 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: 0.0° Phase angle: 56.1° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 194.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Aram Chaos Sediments
PIA09624
Sol (our sun)
HiRISE
| Title |
Aram Chaos Sediments |
| Original Caption Released with Image |
Click on image for larger version Aram Chaos appears to be a former impact crater. The terrain is disrupted, giving it a chaotic appearance (hence the name "chaos"). Scientists have postulated that a lake may have once existed inside the crater and sediments were laid down within the lake. The mineral hematite (rich in iron) has been detected by orbiting spacecraft within Aram Chaos. Hematite has been identified in several other locations on Mars, including at the Mars Exploration Rover landing site in Meridiani Planum. The hematite at both Meridiani and Aram Chaos most likely formed by precipitation in water. This HiRISE image (PSP_002839_1825 [ http://hirise.lpl.arizona.edu/PSP_002839_1825 ]) shows the light-toned sediments inside Aram Chaos that could have formed in a former lake. Unfortunately, dark debris now obscures much of this sediment, making it difficult to view and interpret the rocks. The light-toned layered deposit in the south (bottom) of the image is higher standing and has a pitted surface. Circular structures with dark centers are likely to be impact craters that have been partly filled with dark debris, including sand. More irregular depressions appear to result from erosion of layered beds within the sediments. Wind could erode materials that are slightly weaker more quickly and produce the irregular topography seen along the surface of the deposit. Observation Toolbox Acquisition date: 3 March 2007 Local Mars time: 3:41 PM Degrees latitude (centered): 2.7° Degrees longitude (East): 339.3° Range to target site: 272.3 km (170.2 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: 0.0° Phase angle: 56.1° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 194.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Southern Layered Mound and F
…
PIA09616
Sol (our sun)
HiRISE
| Title |
Southern Layered Mound and Floor in Gale Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002464_1745 [ http://hirise.lpl.arizona.edu/PSP_002464_1745 ]) shows the interior of Gale Crater, a region being considered as a landing site for the 2009 Mars Science Laboratory. Gale is distinguished from many other craters on Mars by a large interior layered mound that extends to the height of the crater rim. The top part of this image contains portions of the southeast part of the mound, with the bottom part showing details of the crater floor. The mound material here is exposed as several distinct smaller hills. Close up, the hills show abundant rocks and debris aprons on their flanks, lacking distinct bedrock layers seen elsewhere on Mars. This suggests that the mound material is friable and easily eroded by the wind over time. Other evidence of wind activity includes bright bedforms near the top of the image and dark bedforms and sand sheets at bottom. Between the hills and dark sand are a series of stacked stratigraphic units. Polygons are seen in some of the units, indicating contraction due to water loss, cooling, or some other process. Many of the polygons seem highly fractured. Possible crossbeds are seen in some of the rock exposures near the bottom of the image. This and other images of Gale will be studied over the coming months and years in order to better understand the geology and further assess the potential as a future landing site. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -5.5° Degrees longitude (East): 138.1° Range to target site: 268.3 km (167.7 miles) Original image scale range: 26.8 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: 3.1° Phase angle: 58.9° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 178.1°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Southern Layered Mound and F
…
PIA09616
Sol (our sun)
HiRISE
| Title |
Southern Layered Mound and Floor in Gale Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002464_1745 [ http://hirise.lpl.arizona.edu/PSP_002464_1745 ]) shows the interior of Gale Crater, a region being considered as a landing site for the 2009 Mars Science Laboratory. Gale is distinguished from many other craters on Mars by a large interior layered mound that extends to the height of the crater rim. The top part of this image contains portions of the southeast part of the mound, with the bottom part showing details of the crater floor. The mound material here is exposed as several distinct smaller hills. Close up, the hills show abundant rocks and debris aprons on their flanks, lacking distinct bedrock layers seen elsewhere on Mars. This suggests that the mound material is friable and easily eroded by the wind over time. Other evidence of wind activity includes bright bedforms near the top of the image and dark bedforms and sand sheets at bottom. Between the hills and dark sand are a series of stacked stratigraphic units. Polygons are seen in some of the units, indicating contraction due to water loss, cooling, or some other process. Many of the polygons seem highly fractured. Possible crossbeds are seen in some of the rock exposures near the bottom of the image. This and other images of Gale will be studied over the coming months and years in order to better understand the geology and further assess the potential as a future landing site. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -5.5° Degrees longitude (East): 138.1° Range to target site: 268.3 km (167.7 miles) Original image scale range: 26.8 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: 3.1° Phase angle: 58.9° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 178.1°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Scalloped Topography in Pene
…
PIA09611
Sol (our sun)
HiRISE
| Title |
Scalloped Topography in Peneus Patera Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002296_1215 [ http://hirise.lpl.arizona.edu/PSP_002296_1215 ]), near the southeast rim of Peneus Patera crater, is marked by depressions in the mantle with scalloped edges. Several of the depressions have apparently coalesced together. These features are most commonly found at approximately 55 degrees north and south latitude. Their presence has led to hypotheses of the removal of subsurface material, possibly interstitial ice by sublimation (evaporation). Steep scarps consistently face the south pole while more gentle slopes face in the direction of the equator. This is most likely due to differences in solar heating. A polygonal pattern of fractures, commonly associated with "scalloped terrain," can be found on the surface surrounding and within the depressions. The fractures indicate that the surface has undergone stress that may have been caused by subsidence, desiccation, or thermal contraction. Scallop formation is believed to be an ongoing process at the present time. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 4:01 PM Degrees latitude (centered): ):-58.0° Degrees longitude (East): 53.7° Range to target site: 250.7 km (156.7 miles) Original image scale range: 50.2 cm/pixel (with 2 x 2 binning) so objects ~150 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.7° Phase angle: 73.8° Solar incidence angle: 78°, with the Sun about 12° above the horizon Solar longitude: 170.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Scalloped Topography in Pene
…
PIA09611
Sol (our sun)
HiRISE
| Title |
Scalloped Topography in Peneus Patera Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002296_1215 [ http://hirise.lpl.arizona.edu/PSP_002296_1215 ]), near the southeast rim of Peneus Patera crater, is marked by depressions in the mantle with scalloped edges. Several of the depressions have apparently coalesced together. These features are most commonly found at approximately 55 degrees north and south latitude. Their presence has led to hypotheses of the removal of subsurface material, possibly interstitial ice by sublimation (evaporation). Steep scarps consistently face the south pole while more gentle slopes face in the direction of the equator. This is most likely due to differences in solar heating. A polygonal pattern of fractures, commonly associated with "scalloped terrain," can be found on the surface surrounding and within the depressions. The fractures indicate that the surface has undergone stress that may have been caused by subsidence, desiccation, or thermal contraction. Scallop formation is believed to be an ongoing process at the present time. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 4:01 PM Degrees latitude (centered): ):-58.0° Degrees longitude (East): 53.7° Range to target site: 250.7 km (156.7 miles) Original image scale range: 50.2 cm/pixel (with 2 x 2 binning) so objects ~150 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 5.7° Phase angle: 73.8° Solar incidence angle: 78°, with the Sun about 12° above the horizon Solar longitude: 170.9°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
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Eroding Crater Fill
PIA09615
Sol (our sun)
HiRISE
| Title |
Eroding Crater Fill |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002478_1770) shows the edge of a mound of sediments in the center of a large impact crater near Amenthes Planum. The mound probably once filled much more of the crater, but it is now eroding away. HiRISE shows a variety of layers. A broad view shows several small plateaus which have likely been preserved by a relatively resistant cap layer, while other levels are exposed elsewhere. The subsection highlighted here shows several types of layers exposed in a pit. These variations point to a relatively complex geologic history at this site. Some layers appear to be fracturing into boulders which roll downslope, while others appear relatively smooth. There are also variations in tone, from light to dark. This diversity may be due to different types of rock, as well as varying strength. Images such as this one indicate that rocks formed on Mars in a variety of ways, and by careful analysis it may be possible to deduce some of the history that has produced the geology at this site. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -3.0° Degrees longitude (East): 115.9° Range to target site: 266.1 km (166.3 miles) Original image scale range: 26.6 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: 0.0° Phase angle: 55.7° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 178.7°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Eroding Crater Fill
PIA09615
Sol (our sun)
HiRISE
| Title |
Eroding Crater Fill |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002478_1770) shows the edge of a mound of sediments in the center of a large impact crater near Amenthes Planum. The mound probably once filled much more of the crater, but it is now eroding away. HiRISE shows a variety of layers. A broad view shows several small plateaus which have likely been preserved by a relatively resistant cap layer, while other levels are exposed elsewhere. The subsection highlighted here shows several types of layers exposed in a pit. These variations point to a relatively complex geologic history at this site. Some layers appear to be fracturing into boulders which roll downslope, while others appear relatively smooth. There are also variations in tone, from light to dark. This diversity may be due to different types of rock, as well as varying strength. Images such as this one indicate that rocks formed on Mars in a variety of ways, and by careful analysis it may be possible to deduce some of the history that has produced the geology at this site. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -3.0° Degrees longitude (East): 115.9° Range to target site: 266.1 km (166.3 miles) Original image scale range: 26.6 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: 0.0° Phase angle: 55.7° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 178.7°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Eroding Crater Fill
PIA09615
Sol (our sun)
HiRISE
| Title |
Eroding Crater Fill |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002478_1770) shows the edge of a mound of sediments in the center of a large impact crater near Amenthes Planum. The mound probably once filled much more of the crater, but it is now eroding away. HiRISE shows a variety of layers. A broad view shows several small plateaus which have likely been preserved by a relatively resistant cap layer, while other levels are exposed elsewhere. The subsection highlighted here shows several types of layers exposed in a pit. These variations point to a relatively complex geologic history at this site. Some layers appear to be fracturing into boulders which roll downslope, while others appear relatively smooth. There are also variations in tone, from light to dark. This diversity may be due to different types of rock, as well as varying strength. Images such as this one indicate that rocks formed on Mars in a variety of ways, and by careful analysis it may be possible to deduce some of the history that has produced the geology at this site. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -3.0° Degrees longitude (East): 115.9° Range to target site: 266.1 km (166.3 miles) Original image scale range: 26.6 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: 0.0° Phase angle: 55.7° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 178.7°, Northern Summer NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
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White Rock Landform in Polla
…
PIA09640
Sol (our sun)
HiRISE
| Title |
White Rock Landform in Pollack Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002244_1720 [ http://hirise.lpl.arizona.edu/PSP_002244_1720 ]) shows a portion of a relatively bright landform named "White Rock" on the floor of Pollack crater in the Sinus Sabaeus region of Mars. Data from the Mars Global Surveyor Thermal Emission Spectrometer (TES) [ http://tes.asu.edu/ ] indicates that this landform is not anomalously bright, relative to other bright Martian regions. Further, the apparent brightness seen here is due to contrast with other materials on the crater floor. Dunes and ripples are visible in the dark material between the bright ridges. Their orientations appear to be influenced by wind directionally channeled by the ridges. Material appears to have been shed from the white landform and deposited on the darker bedforms indicating that the light-toned outcrops break down into fine materials. Its high albedo and location in a topographic basin have led to suggestions that White Rock is an erosional remnant of an ancient lacustrine evaporate deposit. Other interpretations include an eroded accumulation of compacted or weakly cemented aeolian sediment. Observation Toolbox Acquisition date: 1 January 2007 Local Mars time: 3:42 PM Degrees latitude (centered): -8.0° Degrees longitude (East): 25.0° Range to target site: 263.1 km (164.4 miles) Original image scale range: 26.3 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: 1.3° Phase angle: 55.7° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 168.7°, 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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