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Images of Jet Propulsion Laboratory (JPL) and California from 2007 and February 2007
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Titan 'T28' Mosaic
| Description |
Titan 'T28' Mosaic |
| Full Description |
Bright and dark terrains on Titan's trailing hemisphere are revealed by Cassini's Imaging Science Subsystem in this mosaic of images taken during the T28 flyby in April 2007. The region shown in this image, centered on the northern part of Titan's trailing hemisphere (near 31.2 degrees North, 220.7 degrees West), had only been seen at very low resolution until February 2007, when Cassini flew over this area for the first time. This mosaic consists of images taken during one of a series of flybys in early 2007 designed to study this long unavailable part of Titan (5,150 kilometers, or 3,200 miles across). Several intriguing surface features can be seen in this mosaic that warrant further study. Along the top of the mosaic is a series of dark lineaments, or linear features, that stand out against the blandness of the northern, mid-latitude terrain. These features were also observed by the RADAR instrument in December 2006 and represent an area of potential future co-analysis for the RADAR and camera teams. Another such region is the large bright area known as Adiri at bottom center, also imaged by RADAR in October 2005. The mosaic shows a number of dark areas within Adiri that line up with small dune fields observed by RADAR. A portion of the dark terrain surrounding Adiri was also observed in 2005 by RADAR, and likewise was found to consist of large stretches of longitudinal dune fields --further supporting the correlation between equatorial dark regions and dune "seas." To the east of Adiri is a dark spot surrounded by a ring of bright material, which may be associated with an impact crater similar to Sinlap, discovered earlier in the Cassini mission (see Titan Mosaic - East of Xanadu). This mosaic consists of 29 separate frames using a total of 116 images. Each frame consists of three images, taken using a filter sensitive to near-infrared light centered at 938 nanometers, allowing for observations of Titan's surface and lower atmosphere, added together. An image taken using a filter sensitive to visible light centered at 619 nanometers was then subtracted from the product, effectively removing the lower atmosphere contribution to the brightness values in the image, increasing image contrast and improving the visibility of surface features. This process is also intended to reduce noise, but some camera artifacts still remain, such as a dark ring caused by dust in the camera system near the bottom right of each frame. For a wide angle view taken during this Titan encounter, see Titan 'T28' View. The images used for this mosaic were taken on April 11, 2007 from distances ranging from 106,000 to 180,000 kilometers (66,000 to 112,000 miles). This mosaic is in an orthographic projection with a pixel scale of 1.5 kilometers (0.9 miles) per pixel, although the size of resolvable features is likely several times larger, due to atmospheric scattering. An orthographic view is most like the view seen by a distant observer looking through a, telescope. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/Space Science Institute |
| Date |
May 22, 2007 |
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Map of Titan - December 2006
| Description |
Map of Titan - December 2006 |
| Full Description |
This global digital map of Titan was created using data taken by the Cassini spacecraft Imaging Science Subsystem (ISS). The data here consist of images taken using a filter centered at 938 nanometers, allowing researchers to examine albedo (or inherent brightness) variations across the surface of Titan. Due to the scattering of light by Titan's dense atmosphere, no topographic shading is visible in these images. The map is an equidistant projection and has a scale of 2 kilometers (1.25 miles) per pixel. Equidistant projections preserve distances on a body, with some distortion of area and direction. Actual resolution varies greatly across the map, with the best coverage (close to the map scale) near the center and edges of the map and the worst coverage on the trailing hemisphere (centered around 270 degrees west longitude). Coverage should improve in some of the poorly covered areas starting in February 2007, when northern Belet, Adiri, and Dilmun will be imaged. Imaging coverage in the northern polar region, currently blank on this map, will improve over the next few years, as Titan approaches vernal equinox in August 2009. The mean radius of Titan used for projection of this map is 2,575 kilometers (1,600 miles). Until a control network is created for Titan, the satellite is assumed to be spherical. A labeled version of the map is available here. The named features are designated by the International Astronomical Union. (A "facula" on Titan is a bright spot, a "macula" is a dark spot.) This map demonstrates how our knowledge of Titan's surface has been vastly improved since Cassini arrived and began mapping the outsize moon. See Mapping Titan's Surface and Titan's Variety (with Grid) for earlier Cassini maps of Titan. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/Space Science Institute |
| Date |
December 29, 2006 |
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Map of Titan with Labels- De
…
| Description |
This global digital map of Titan was created using data taken by the Cassini spacecraft Imaging Science Subsystem (ISS). |
| Full Description |
This global digital map of Titan was created using data taken by the Cassini spacecraft Imaging Science Subsystem (ISS). The data here consist of images taken using a filter centered at 938 nanometers, allowing researchers to examine albedo (or inherent brightness) variations across the surface of Titan. Due to the scattering of light by Titan's dense atmosphere, no topographic shading is visible in these images. The map is an equidistant projection and has a scale of 2 kilometers (1.25 miles) per pixel. Equidistant projections preserve distances on a body, with some distortion of area and direction. Actual resolution varies greatly across the map, with the best coverage (close to the map scale) near the center and edges of the map and the worst coverage on the trailing hemisphere (centered around 270 degrees west longitude). Coverage should improve in some of the poorly covered areas starting in February 2007, when northern Belet, Adiri, and Dilmun will be imaged. Imaging coverage in the northern polar region, currently blank on this map, will improve over the next few years, as Titan approaches vernal equinox in August 2009. The mean radius of Titan used for projection of this map is 2,575 kilometers (1,600 miles). Until a control network is created for Titan, the satellite is assumed to be spherical. A clean version of the map, as well as a link to higher resolution versions, is available here. The named features are designated by the International Astronomical Union. (A "facula" on Titan is a bright spot, a "macula" is a dark spot.) This map demonstrates how our knowledge of Titan's surface has been vastly improved since Cassini arrived and began mapping the outsize moon. See Mapping Titan's Surface and Titan's Variety (with Grid) for earlier Cassini maps of Titan. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . *Credit:* NASA/JPL/Space Science Institute |
| Date |
December 29, 2006 |
|
Titan "T28" Mosaic
PIA08945
Saturn
Imaging Science Subsystem
| Title |
Titan "T28" Mosaic |
| Original Caption Released with Image |
. The images used for this mosaic were taken on April 11, 2007 from distances ranging from 106,000 to 180,000 kilometers (66,000 to 112,000 miles). This mosaic is in an orthographic projection with a pixel scale of 1.5 kilometers (0.9 miles) per pixel, although the size of resolvable features is likely several times larger, due to atmospheric scattering. An orthographic view is most like the view seen by a distant observer looking through a telescope. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov/home/index.cfm [ http://saturn.jpl.nasa.gov ]. The Cassini imaging team homepage is at http://ciclops.org [ http://ciclops.org ]., Bright and dark terrains on Titan's trailing hemisphere are revealed by Cassini's Imaging Science Subsystem in this mosaic of images taken during the T28 flyby in April 2007. The region shown in this image, centered on the northern part of Titan's trailing hemisphere (near 31.2 degrees North, 220.7 degrees West), had only been seen at very low resolution until February 2007, when Cassini flew over this area for the first time. This mosaic consists of images taken during one of a series of flybys in early 2007 designed to study this long unavailable part of Titan (5,150 kilometers, or 3,200 miles across). Several intriguing surface features can be seen in this mosaic that warrant further study. Along the top of the mosaic is a series of dark lineaments, or linear features, that stand out against the blandness of the northern, mid-latitude terrain. These features were also observed by the RADAR instrument in December 2006 and represent an area of potential future co-analysis for the RADAR and camera teams. Another such region is the large bright area known as Adiri at bottom center, also imaged by RADAR in October 2005. The mosaic shows a number of dark areas within Adiri that line up with small dune fields observed by RADAR. A portion of the dark terrain surrounding Adiri was also observed in 2005 by RADAR, and likewise was found to consist of large stretches of longitudinal dune fields -- further supporting the correlation between equatorial dark regions and dune "seas." To the east of Adiri is a dark spot surrounded by a ring of bright material, which may be associated with an impact crater similar to Sinlap, discovered earlier in the Cassini mission (see PIA6222 [ http://photojournal.jpl.nasa.gov/catalog/PIA06222 ]). This mosaic consists of 29 separate frames using a total of 116 images. Each frame consists of three images, taken using a filter sensitive to near-infrared light centered at 938 nanometers, allowing for observations of Titan's surface and lower atmosphere, added together. An image taken using a filter sensitive to visible light centered at 619 nanometers was then subtracted from the product, effectively removing the lower atmosphere contribution to the brightness values in the image, increasing image contrast and improving the visibility of surface features.This process is also intended to reduce noise, but some camera artifacts still remain, such as a dark ring caused by dust in the camera system near the bottom right of each frame. For a wide angle view taken during this Titan encounter, see PIA8943 [ http://photojournal.jpl.nasa.gov/catalog/PIA08943 ] |
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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. |
|
Map of Titan - December 2006
PIA08346
Saturn
Imaging Science Subsystem
| Title |
Map of Titan - December 2006 |
| Original Caption Released with Image |
Annotated Version This global digital map of Titan was created using data taken by the Cassini spacecraft Imaging Science Subsystem (ISS). The data here consist of images taken using a filter centered at 938 nanometers, allowing researchers to examine albedo (or inherent brightness) variations across the surface of Titan. Due to the scattering of light by Titan's dense atmosphere, no topographic shading is visible in these images. The map is an equidistant projection and has a scale of 2 kilometers (1.25 miles) per pixel. Equidistant projections preserve distances on a body, with some distortion of area and direction. Actual resolution varies greatly across the map, with the best coverage (close to the map scale) near the center and edges of the map and the worst coverage on the trailing hemisphere (centered around 270 degrees west longitude). Coverage should improve in some of the poorly covered areas starting in February 2007, when northern Belet, Adiri, and Dilmun will be imaged. Imaging coverage in the northern polar region, currently blank on this map, will improve over the next few years, as Titan approaches vernal equinox in August 2009. The mean radius of Titan used for projection of this map is 2,575 kilometers (1,600 miles). Until a control network is created for Titan, the satellite is assumed to be spherical. The named features are designated by the International Astronomical Union. (A "facula" on Titan is a bright spot, a "macula" is a dark spot.) This map demonstrates how our knowledge of Titan's surface has been vastly improved since Cassini arrived and began mapping the outsize moon. See PIA06086 [ http://photojournal.jpl.nasa.gov/catalog/PIA06086 ] for an earlier Cassini map of Titan. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov/home/index.cfm [ http://saturn.jpl.nasa.gov ]. The Cassini imaging team homepage is at http://ciclops.org [ http://ciclops.org ]. |
|
Map of Titan - December 2006
PIA08346
Saturn
Imaging Science Subsystem
| Title |
Map of Titan - December 2006 |
| Original Caption Released with Image |
Annotated Version This global digital map of Titan was created using data taken by the Cassini spacecraft Imaging Science Subsystem (ISS). The data here consist of images taken using a filter centered at 938 nanometers, allowing researchers to examine albedo (or inherent brightness) variations across the surface of Titan. Due to the scattering of light by Titan's dense atmosphere, no topographic shading is visible in these images. The map is an equidistant projection and has a scale of 2 kilometers (1.25 miles) per pixel. Equidistant projections preserve distances on a body, with some distortion of area and direction. Actual resolution varies greatly across the map, with the best coverage (close to the map scale) near the center and edges of the map and the worst coverage on the trailing hemisphere (centered around 270 degrees west longitude). Coverage should improve in some of the poorly covered areas starting in February 2007, when northern Belet, Adiri, and Dilmun will be imaged. Imaging coverage in the northern polar region, currently blank on this map, will improve over the next few years, as Titan approaches vernal equinox in August 2009. The mean radius of Titan used for projection of this map is 2,575 kilometers (1,600 miles). Until a control network is created for Titan, the satellite is assumed to be spherical. The named features are designated by the International Astronomical Union. (A "facula" on Titan is a bright spot, a "macula" is a dark spot.) This map demonstrates how our knowledge of Titan's surface has been vastly improved since Cassini arrived and began mapping the outsize moon. See PIA06086 [ http://photojournal.jpl.nasa.gov/catalog/PIA06086 ] for an earlier Cassini map of Titan. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov/home/index.cfm [ http://saturn.jpl.nasa.gov ]. The Cassini imaging team homepage is at http://ciclops.org [ http://ciclops.org ]. |
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Joint Observation of the Isi
…
PIA09614
Sol (our sun)
HiRISE
| Title |
Joint Observation of the Isidis Basin with the Rosetta Mission |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002703_1920 [ http://hirise.lpl.arizona.edu/PSP_002703_1920 ]) of the floor of the Isidis Basin was taken in coordination with the Mars flyby of the European Rosetta mission. Comparing this image with those taken by the OSIRIS camera onboard Rosetta should help calibrate HiRISE. Since OSIRIS was only able to take low resolution images of Mars, this image was targeted at a broad, bland, expanse of uniform appearance. However, it is just east of the landing ellipse for the failed European Beagle 2 lander and may help with the search for debris from that mission. This is an example of the international cooperation of HiRISE and the MRO missions. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:40 PM Degrees latitude (centered): 11.8° Degrees longitude (East): 91.1° Range to target site: 277.3 km (173.3 miles) Original image scale range: 27.7 cm/pixel (with 1 x 1 binning) so objects ~83 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.1° Phase angle: 56.9° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 188.7°, 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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Joint Observation of the Isi
…
PIA09614
Sol (our sun)
HiRISE
| Title |
Joint Observation of the Isidis Basin with the Rosetta Mission |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002703_1920 [ http://hirise.lpl.arizona.edu/PSP_002703_1920 ]) of the floor of the Isidis Basin was taken in coordination with the Mars flyby of the European Rosetta mission. Comparing this image with those taken by the OSIRIS camera onboard Rosetta should help calibrate HiRISE. Since OSIRIS was only able to take low resolution images of Mars, this image was targeted at a broad, bland, expanse of uniform appearance. However, it is just east of the landing ellipse for the failed European Beagle 2 lander and may help with the search for debris from that mission. This is an example of the international cooperation of HiRISE and the MRO missions. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:40 PM Degrees latitude (centered): 11.8° Degrees longitude (East): 91.1° Range to target site: 277.3 km (173.3 miles) Original image scale range: 27.7 cm/pixel (with 1 x 1 binning) so objects ~83 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.1° Phase angle: 56.9° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 188.7°, 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. |
|
Light-Toned Material in Mela
…
PIA09626
Sol (our sun)
HiRISE
| Title |
Light-Toned Material in Melas Chasma |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002630_1695 [ http://hirise.lpl.arizona.edu/PSP_002630_1695 ]) shows an outcrop of bright material in Melas Chasma, part of the giant Valles Marineris trough system. These troughs contain many bright deposits, often layered. The origin of these materials is still not known, but is the subject of much study because answering this question will provide important information regarding the geologic history of Mars. In this image, some layers can be seen, but much of the surface has a strange scalloped texture. The cause of this texture is unclear, but it is likely related to the mechanism of erosion of these deposits as well as their physical nature. These materials are being eroded by winds, forming elongated ridges called yardangs. These winds may also be responsible for the small-scale scalloped texture. Also, landslides have produced some talus cones, composed of piles of loose debris, these are visible in places, mostly near the base of the mound, as wedge-shaped features containing many boulders. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -10.3° Degrees longitude (East): 268.2° Range to target site: 264.7 km (165.4 miles) Original image scale range: 26.5 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: 8.5° Phase angle: 64.0° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 185.5°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
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Light-Toned Material in Mela
…
PIA09626
Sol (our sun)
HiRISE
| Title |
Light-Toned Material in Melas Chasma |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002630_1695 [ http://hirise.lpl.arizona.edu/PSP_002630_1695 ]) shows an outcrop of bright material in Melas Chasma, part of the giant Valles Marineris trough system. These troughs contain many bright deposits, often layered. The origin of these materials is still not known, but is the subject of much study because answering this question will provide important information regarding the geologic history of Mars. In this image, some layers can be seen, but much of the surface has a strange scalloped texture. The cause of this texture is unclear, but it is likely related to the mechanism of erosion of these deposits as well as their physical nature. These materials are being eroded by winds, forming elongated ridges called yardangs. These winds may also be responsible for the small-scale scalloped texture. Also, landslides have produced some talus cones, composed of piles of loose debris, these are visible in places, mostly near the base of the mound, as wedge-shaped features containing many boulders. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:41 PM Degrees latitude (centered): -10.3° Degrees longitude (East): 268.2° Range to target site: 264.7 km (165.4 miles) Original image scale range: 26.5 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: 8.5° Phase angle: 64.0° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 185.5°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
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. |
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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 Depressions with L
…
PIA09627
Sol (our sun)
HiRISE
| Title |
Scalloped Depressions with Layers in the Northern Plains |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002439_2265 [ http://hirise.lpl.arizona.edu/PSP_002439_2265 ]), of the northern plains of Mars, is marked by depressions in a layer of material that covers the region. The depressions, several of which have coalesced together, have scalloped edges and layers in their walls. Features such as these 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 ground ice, by sublimation (evaporation). This process is believed to be ongoing today. In this image, steeper scarps with layers consistently face the north pole while more gentle slopes without layers face in the direction of the equator. This is most likely due to differences in solar heating. Large boulders, some several meters in length, are scattered within the depressions and on the surrounding surface. Also on the surface surrounding the scalloped depressions is a polygonal pattern of fractures. This is commonly associated with "scalloped terrain," and indicates that the surface has undergone stress potentially caused by subsidence, desiccation, or thermal contraction. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:23 PM Degrees latitude (centered): 46.0° Degrees longitude (East): 92.1° Range to target site: 310.7 km (194.2 miles) Original image scale range: from 31.1 cm/pixel (with 1 x 1 binning) to 62.2 cm/pixel (with 2 x 2 binning) Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 14.7° Phase angle: 77.0° Solar incidence angle: 63°, with the Sun about 27° above the horizon Solar longitude: 177.0°, 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. |
|
Scalloped Depressions with L
…
PIA09627
Sol (our sun)
HiRISE
| Title |
Scalloped Depressions with Layers in the Northern Plains |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002439_2265 [ http://hirise.lpl.arizona.edu/PSP_002439_2265 ]), of the northern plains of Mars, is marked by depressions in a layer of material that covers the region. The depressions, several of which have coalesced together, have scalloped edges and layers in their walls. Features such as these 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 ground ice, by sublimation (evaporation). This process is believed to be ongoing today. In this image, steeper scarps with layers consistently face the north pole while more gentle slopes without layers face in the direction of the equator. This is most likely due to differences in solar heating. Large boulders, some several meters in length, are scattered within the depressions and on the surrounding surface. Also on the surface surrounding the scalloped depressions is a polygonal pattern of fractures. This is commonly associated with "scalloped terrain," and indicates that the surface has undergone stress potentially caused by subsidence, desiccation, or thermal contraction. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:23 PM Degrees latitude (centered): 46.0° Degrees longitude (East): 92.1° Range to target site: 310.7 km (194.2 miles) Original image scale range: from 31.1 cm/pixel (with 1 x 1 binning) to 62.2 cm/pixel (with 2 x 2 binning) Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 14.7° Phase angle: 77.0° Solar incidence angle: 63°, with the Sun about 27° above the horizon Solar longitude: 177.0°, 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. |
|
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. |
|
Ancient Lava Plain in Thauma
…
PIA09617
Sol (our sun)
HiRISE
| Title |
Ancient Lava Plain in Thaumasia Planum |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002432_1525 [ http://hirise.lpl.arizona.edu/PSP_002432_1525 ]) samples part of an ancient lava plain in Thaumasia Planum. The stack of lava flows has been folded into ridges the size of a chain of hills, as can be seen in the center of the image. The lava and the ridge has been degraded by erosion. The numerous craters and dunes attest to two of the erosional processes-meteorite impacts and the wind. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:47 PM Degrees latitude (centered): -27.4° Degrees longitude (East): 294.8° Range to target site: 252.7 km (157.9 miles) Original image scale range: 25.3 cm/pixel (with 1 x 1 binning) so objects ~76 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.3° Phase angle: 61.7° Solar incidence angle: 62°, with the Sun about 28° above the horizon Solar longitude: 176.7°, 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. |
|
Ancient Lava Plain in Thauma
…
PIA09617
Sol (our sun)
HiRISE
| Title |
Ancient Lava Plain in Thaumasia Planum |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002432_1525 [ http://hirise.lpl.arizona.edu/PSP_002432_1525 ]) samples part of an ancient lava plain in Thaumasia Planum. The stack of lava flows has been folded into ridges the size of a chain of hills, as can be seen in the center of the image. The lava and the ridge has been degraded by erosion. The numerous craters and dunes attest to two of the erosional processes-meteorite impacts and the wind. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:47 PM Degrees latitude (centered): -27.4° Degrees longitude (East): 294.8° Range to target site: 252.7 km (157.9 miles) Original image scale range: 25.3 cm/pixel (with 1 x 1 binning) so objects ~76 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 0.3° Phase angle: 61.7° Solar incidence angle: 62°, with the Sun about 28° above the horizon Solar longitude: 176.7°, 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. |
|
Sand Dune Field in Richardso
…
PIA09631
Sol (our sun)
HiRISE
| Title |
Sand Dune Field in Richardson Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002542_1080 [ http://hirise.lpl.arizona.edu/PSP_002542_1080 ]) is a view of the sand dune field in Richardson Crater covered with seasonal frost. The subimage is a close-up view of defrosting patterns on the dunes. The frost is a combination of frozen carbon dioxide and some water ice that covers the dunes in the winter and spring. As the seasonal frost sublimes away, odd features such as spots, fans, and streaks form. Small dark streaks on the dune slip face slopes may be where recent avalanches of sand, or perhaps wind, has moved the dark sand underlying the frost, or where frost has been removed to expose the sand. Alternatively, the dark streaks may be patches of coarse-grained ice that are clear enough so that the dark material below the ice is visible. The slip faces indicate that the general direction of sand transport is from the right to the left across the image. It has been hypothesized that the dark spots and fans may be "geysers" or "cold gas jets" that form when sublimation processes trap gas at the bottom of the ice. The gas is released through cracks in the ice, entraining dust from below the ice and scattering it onto the surface to form the dark spots and fans. The high resolution, stereo, and low light imaging capabilities of HiRISE has provided new insight into the processes that form these features. Repeated imaging in a variety of locations will provide a record of their development and evolution. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 4:05 PM Degrees latitude (centered): -72.0° Degrees longitude (East): 179.5° Range to target site: 251.8 km (179.5 miles) Original image scale range: 50.4 cm/pixel (with 2 x 2 binning) so objects ~151 cm across are resolved Map-projected scale: 50 cm/pixel Map-projection: POLAR STEREOGRAPHIC Emission angle: 9.2° Phase angle: 88.5° Solar incidence angle: 81°, with the Sun about 9° above the horizon Solar longitude: 181.5 °, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Sand Dune Field in Richardso
…
PIA09631
Sol (our sun)
HiRISE
| Title |
Sand Dune Field in Richardson Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002542_1080 [ http://hirise.lpl.arizona.edu/PSP_002542_1080 ]) is a view of the sand dune field in Richardson Crater covered with seasonal frost. The subimage is a close-up view of defrosting patterns on the dunes. The frost is a combination of frozen carbon dioxide and some water ice that covers the dunes in the winter and spring. As the seasonal frost sublimes away, odd features such as spots, fans, and streaks form. Small dark streaks on the dune slip face slopes may be where recent avalanches of sand, or perhaps wind, has moved the dark sand underlying the frost, or where frost has been removed to expose the sand. Alternatively, the dark streaks may be patches of coarse-grained ice that are clear enough so that the dark material below the ice is visible. The slip faces indicate that the general direction of sand transport is from the right to the left across the image. It has been hypothesized that the dark spots and fans may be "geysers" or "cold gas jets" that form when sublimation processes trap gas at the bottom of the ice. The gas is released through cracks in the ice, entraining dust from below the ice and scattering it onto the surface to form the dark spots and fans. The high resolution, stereo, and low light imaging capabilities of HiRISE has provided new insight into the processes that form these features. Repeated imaging in a variety of locations will provide a record of their development and evolution. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 4:05 PM Degrees latitude (centered): -72.0° Degrees longitude (East): 179.5° Range to target site: 251.8 km (179.5 miles) Original image scale range: 50.4 cm/pixel (with 2 x 2 binning) so objects ~151 cm across are resolved Map-projected scale: 50 cm/pixel Map-projection: POLAR STEREOGRAPHIC Emission angle: 9.2° Phase angle: 88.5° Solar incidence angle: 81°, with the Sun about 9° above the horizon Solar longitude: 181.5 °, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Sand Dune Field in Richardso
…
PIA09631
Sol (our sun)
HiRISE
| Title |
Sand Dune Field in Richardson Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002542_1080 [ http://hirise.lpl.arizona.edu/PSP_002542_1080 ]) is a view of the sand dune field in Richardson Crater covered with seasonal frost. The subimage is a close-up view of defrosting patterns on the dunes. The frost is a combination of frozen carbon dioxide and some water ice that covers the dunes in the winter and spring. As the seasonal frost sublimes away, odd features such as spots, fans, and streaks form. Small dark streaks on the dune slip face slopes may be where recent avalanches of sand, or perhaps wind, has moved the dark sand underlying the frost, or where frost has been removed to expose the sand. Alternatively, the dark streaks may be patches of coarse-grained ice that are clear enough so that the dark material below the ice is visible. The slip faces indicate that the general direction of sand transport is from the right to the left across the image. It has been hypothesized that the dark spots and fans may be "geysers" or "cold gas jets" that form when sublimation processes trap gas at the bottom of the ice. The gas is released through cracks in the ice, entraining dust from below the ice and scattering it onto the surface to form the dark spots and fans. The high resolution, stereo, and low light imaging capabilities of HiRISE has provided new insight into the processes that form these features. Repeated imaging in a variety of locations will provide a record of their development and evolution. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 4:05 PM Degrees latitude (centered): -72.0° Degrees longitude (East): 179.5° Range to target site: 251.8 km (179.5 miles) Original image scale range: 50.4 cm/pixel (with 2 x 2 binning) so objects ~151 cm across are resolved Map-projected scale: 50 cm/pixel Map-projection: POLAR STEREOGRAPHIC Emission angle: 9.2° Phase angle: 88.5° Solar incidence angle: 81°, with the Sun about 9° above the horizon Solar longitude: 181.5 °, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Proposed MSL Site in Melas C
…
PIA09639
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Melas Chasma |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002551_1700 [ http://hirise.lpl.arizona.edu/PSP_002551_1700 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Melas Chasma. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -9.7° Degrees longitude (East): 283.6° Range to target site: 262.9 km (164.3 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: 0.6° Phase angle: 57.0° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 181.9°, 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 Melas C
…
PIA09639
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Melas Chasma |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002551_1700 [ http://hirise.lpl.arizona.edu/PSP_002551_1700 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Melas Chasma. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -9.7° Degrees longitude (East): 283.6° Range to target site: 262.9 km (164.3 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: 0.6° Phase angle: 57.0° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 181.9°, 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 Nili Fo
…
PIA09638
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Nili Fossae Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002743_1985 [ http://hirise.lpl.arizona.edu/PSP_002743_1985 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Nili Fossae Crater. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:36 PM Degrees latitude (centered): 18.5° Degrees longitude (East): 77.5° Range to target site: 283.0 km (176.9 miles) Original image scale range: 28.3 cm/pixel (with 1 x 1 binning) so objects ~85 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 9.0° Phase angle: 66.8° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 190.5°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Proposed MSL Site in Nili Fo
…
PIA09638
Sol (our sun)
HiRISE
| Title |
Proposed MSL Site in Nili Fossae Crater |
| Original Caption Released with Image |
Click on image for larger version HiRISE image (PSP_002743_1985 [ http://hirise.lpl.arizona.edu/PSP_002743_1985 ]) of proposed landing site for the Mars Science Laboratory (MSL) [ http://mars.jpl.nasa.gov/msl/ ] in Nili Fossae Crater. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:36 PM Degrees latitude (centered): 18.5° Degrees longitude (East): 77.5° Range to target site: 283.0 km (176.9 miles) Original image scale range: 28.3 cm/pixel (with 1 x 1 binning) so objects ~85 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 9.0° Phase angle: 66.8° Solar incidence angle: 58°, with the Sun about 32° above the horizon Solar longitude: 190.5°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Layered Rocks in a Crater in
…
PIA09658
Sol (our sun)
HiRISE
| Title |
Layered Rocks in a Crater in Arabia Terra |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002574_1865 [ http://hirise.lpl.arizona.edu/PSP_002574_1865 ]) shows a ground surface composed of many thin light- and dark-toned layers. These layers are mostly parallel with adjacent layers, and sets of layers often form intricate curved shapes that are reminiscent of wood grain. What we see here is actually a series of rock layers that have been sequentially laid down on the floor of a large impact crater. These layers create interesting geometric patterns because they initially accumulated as large ripples, or sand dunes. Subsequently, the ground surface was eroded away by the wind, revealing these underground layers of bedrock. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:42 PM Degrees latitude (centered): 6.6° Degrees longitude (East): 14.1° Range to target site: 275.1 km (171.9 miles) Original image scale range: 27.5 cm/pixel (with 1 x 1 binning) so objects ~83 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 4.8° Phase angle: 51.3° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 183.0°, 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. |
|
Layered Rocks in a Crater in
…
PIA09658
Sol (our sun)
HiRISE
| Title |
Layered Rocks in a Crater in Arabia Terra |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002574_1865 [ http://hirise.lpl.arizona.edu/PSP_002574_1865 ]) shows a ground surface composed of many thin light- and dark-toned layers. These layers are mostly parallel with adjacent layers, and sets of layers often form intricate curved shapes that are reminiscent of wood grain. What we see here is actually a series of rock layers that have been sequentially laid down on the floor of a large impact crater. These layers create interesting geometric patterns because they initially accumulated as large ripples, or sand dunes. Subsequently, the ground surface was eroded away by the wind, revealing these underground layers of bedrock. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:42 PM Degrees latitude (centered): 6.6° Degrees longitude (East): 14.1° Range to target site: 275.1 km (171.9 miles) Original image scale range: 27.5 cm/pixel (with 1 x 1 binning) so objects ~83 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 4.8° Phase angle: 51.3° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 183.0°, 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. |
|
Floor of Ius Chasma
PIA09605
Sol (our sun)
HiRISE
| Title |
Floor of Ius Chasma |
| Original Caption Released with Image |
Click on image for larger version Ius Chasma is one of several canyons that make up Valles Marineris, the largest canyon system in the Solar System. The canyons likely formed by extension in association with the development of the Tharsis plateau and volcanoes to the west. Wind and possibly water have modified the canyons after they formed. This HiRISE image (PSP_002538_1720 [ http://hirise.lpl.arizona.edu/PSP_002538_1720 ]) shows the floor of Ius Chasma. The floor is bounded to the north and south by higher standing wallrock, with a few exposures of wallrock seen in the north (top) of the picture. Much of the floor is covered by ripples that are oriented approximately north-south, indicating an east to west wind flow, parallel to the orientation of Ius Chasma. Layered deposits and bright patches of material are also seen along portions of the Ius Chasma floor. The layered deposits appear distinct in morphology from the nearby wallrock. These layered deposits could be lava flows, sediments deposited in a former lake, or fines that settled out from the atmosphere over time, such as dust or volcanic ash. The bright outcrops visible further south in the image have been seen elsewhere in Valles Marineris as well as other locations on Mars and tend to have mineral signatures consistent with sulfates. Data from the CRISM instrument (also on Mars Reconnaissance Orbiter) of the composition of these bright patches in Ius Chasma could shed insight into their origin. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -8.0° Degrees longitude (East): 278.4° Range to target site: 265.7 km (166.0 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: 0.1° Phase angle: 56.2° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 181.4°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Floor of Ius Chasma
PIA09605
Sol (our sun)
HiRISE
| Title |
Floor of Ius Chasma |
| Original Caption Released with Image |
Click on image for larger version Ius Chasma is one of several canyons that make up Valles Marineris, the largest canyon system in the Solar System. The canyons likely formed by extension in association with the development of the Tharsis plateau and volcanoes to the west. Wind and possibly water have modified the canyons after they formed. This HiRISE image (PSP_002538_1720 [ http://hirise.lpl.arizona.edu/PSP_002538_1720 ]) shows the floor of Ius Chasma. The floor is bounded to the north and south by higher standing wallrock, with a few exposures of wallrock seen in the north (top) of the picture. Much of the floor is covered by ripples that are oriented approximately north-south, indicating an east to west wind flow, parallel to the orientation of Ius Chasma. Layered deposits and bright patches of material are also seen along portions of the Ius Chasma floor. The layered deposits appear distinct in morphology from the nearby wallrock. These layered deposits could be lava flows, sediments deposited in a former lake, or fines that settled out from the atmosphere over time, such as dust or volcanic ash. The bright outcrops visible further south in the image have been seen elsewhere in Valles Marineris as well as other locations on Mars and tend to have mineral signatures consistent with sulfates. Data from the CRISM instrument (also on Mars Reconnaissance Orbiter) of the composition of these bright patches in Ius Chasma could shed insight into their origin. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -8.0° Degrees longitude (East): 278.4° Range to target site: 265.7 km (166.0 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: 0.1° Phase angle: 56.2° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 181.4°, Northern Autumn NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo. |
|
Proctor Crater Dune Field
PIA09606
Sol (our sun)
HiRISE
| Title |
Proctor Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version Image (PSP_002455_1320 [ http://hirise.lpl.arizona.edu/PSP_002455_1320 ]) shows the edge of a dark dune field on the floor of Proctor crater, a 150 kilometer diameter crater in the southern highlands of Mars. The subimage is a close-up view of the dark dunes. These dunes are most likely composed of basaltic sand that has collected on the bottom of the crater. Superimposed on their surface are smaller secondary dunes which are commonly seen on terrestrial dunes of this size. Near the crests of the dark dunes are bright patches of frost. Dark spots within the frost patches are areas where defrosting is occurring. Many smaller and brighter bed forms, most likely small dunes or granule ripples, cover the substrate between the larger dark dunes as well as most of the floor of Proctor Crater. In many locations, large boulders are seen on the same surfaces as the bright bed forms. The dark dunes stratigraphically overlie the small bright bed forms indicating that the darker dunes formed more recently. However in several areas, the dark dunes appear to influence the orientation of the small bright dunes, possibly by wind flowing around the larger dunes, suggesting that both dark and bright bed forms are coeval. Observation Toolbox: Acquisition date: 2 February 2007 Local Mars time: 3:56 PM Degrees latitude (centered): -47.8° Degrees longitude (East): 30.7° Range to target site: 253.5 km (158.4 miles) Original image scale range: 25.4 cm/pixel (with 1 x 1 binning) so objects ~76 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 6.8° Phase angle: 65.1° Solar incidence angle: 71°, with the Sun about 19° above the horizon Solar longitude: 177.7°, 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. |
|
Proctor Crater Dune Field
PIA09606
Sol (our sun)
HiRISE
| Title |
Proctor Crater Dune Field |
| Original Caption Released with Image |
Click on image for larger version Image (PSP_002455_1320 [ http://hirise.lpl.arizona.edu/PSP_002455_1320 ]) shows the edge of a dark dune field on the floor of Proctor crater, a 150 kilometer diameter crater in the southern highlands of Mars. The subimage is a close-up view of the dark dunes. These dunes are most likely composed of basaltic sand that has collected on the bottom of the crater. Superimposed on their surface are smaller secondary dunes which are commonly seen on terrestrial dunes of this size. Near the crests of the dark dunes are bright patches of frost. Dark spots within the frost patches are areas where defrosting is occurring. Many smaller and brighter bed forms, most likely small dunes or granule ripples, cover the substrate between the larger dark dunes as well as most of the floor of Proctor Crater. In many locations, large boulders are seen on the same surfaces as the bright bed forms. The dark dunes stratigraphically overlie the small bright bed forms indicating that the darker dunes formed more recently. However in several areas, the dark dunes appear to influence the orientation of the small bright dunes, possibly by wind flowing around the larger dunes, suggesting that both dark and bright bed forms are coeval. Observation Toolbox: Acquisition date: 2 February 2007 Local Mars time: 3:56 PM Degrees latitude (centered): -47.8° Degrees longitude (East): 30.7° Range to target site: 253.5 km (158.4 miles) Original image scale range: 25.4 cm/pixel (with 1 x 1 binning) so objects ~76 cm across are resolved Map-projected scale: 25 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 6.8° Phase angle: 65.1° Solar incidence angle: 71°, with the Sun about 19° above the horizon Solar longitude: 177.7°, 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. |
|
Pit Craters of Tractus Caten
…
PIA09607
Sol (our sun)
HiRISE
| Title |
Pit Craters of Tractus Catena |
| Original Caption Released with Image |
Click on image for larger version These pits formed through collapse above an underground void. The movement of rock along faults may have created this void deep underground. Faults are commonly thought of as planar cracks in the ground. In reality, faults have very rough surfaces that can create voids as the rocks slide along the fault. Alternatively, the movement of magma (molten rock) underground may have also created such underground voids. As magma moves underground, it pushes aside the bedrock, making an underground tunnel. This tunnel remains behind as the magma drains away and subsequent collapse can occur into it. A combination of processes may also result in pit crater formation, as faults are pre-made passageways for the magma to move underground. There is much evidence of faulting in this scene. The series of stair-stepped cliffs are actually faults, with each cliff representing the approximate location of a fault. Thus it seems likely that faults played an important role in the formation of these pit craters. The role of magma flow in the formation of these pit craters remains unknown. The presence of eruptive vents near these pits would be a clue to the past presence of magma. Such vents are not observed in this image, although the absence of these vents does not rule out magma. Magma does not always erupt at the surface and can remain entirely underground. This HiRISE image is PSP_002420_2040 [ http://hirise.lpl.arizona.edu/PSP_002420_2040 ]. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:37 PM Degrees latitude (centered): 23.8° Degrees longitude (East): 256.2° Range to target site: 280.6 km (175.3 miles) Original image scale range: 56.1 cm/pixel (with 2 x 2 binning) so objects ~168 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 3.1° Phase angle: 54.1° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 176.2°, 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. |
|
Pit Craters of Tractus Caten
…
PIA09607
Sol (our sun)
HiRISE
| Title |
Pit Craters of Tractus Catena |
| Original Caption Released with Image |
Click on image for larger version These pits formed through collapse above an underground void. The movement of rock along faults may have created this void deep underground. Faults are commonly thought of as planar cracks in the ground. In reality, faults have very rough surfaces that can create voids as the rocks slide along the fault. Alternatively, the movement of magma (molten rock) underground may have also created such underground voids. As magma moves underground, it pushes aside the bedrock, making an underground tunnel. This tunnel remains behind as the magma drains away and subsequent collapse can occur into it. A combination of processes may also result in pit crater formation, as faults are pre-made passageways for the magma to move underground. There is much evidence of faulting in this scene. The series of stair-stepped cliffs are actually faults, with each cliff representing the approximate location of a fault. Thus it seems likely that faults played an important role in the formation of these pit craters. The role of magma flow in the formation of these pit craters remains unknown. The presence of eruptive vents near these pits would be a clue to the past presence of magma. Such vents are not observed in this image, although the absence of these vents does not rule out magma. Magma does not always erupt at the surface and can remain entirely underground. This HiRISE image is PSP_002420_2040 [ http://hirise.lpl.arizona.edu/PSP_002420_2040 ]. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:37 PM Degrees latitude (centered): 23.8° Degrees longitude (East): 256.2° Range to target site: 280.6 km (175.3 miles) Original image scale range: 56.1 cm/pixel (with 2 x 2 binning) so objects ~168 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 3.1° Phase angle: 54.1° Solar incidence angle: 57°, with the Sun about 33° above the horizon Solar longitude: 176.2°, 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. |
|
Layers Exposed on Slope in E
…
PIA09590
Sol (our sun)
HiRISE
| Title |
Layers Exposed on Slope in Echus Chasma Region |
| Original Caption Released with Image |
Click on image for larger version The layers seen in the HiRISE subimage of Echus Chasma are very different from the light-toned, thinly bedded layers HiRISE has observed in deposits seen elsewhere in Valles Marineris. The HiRISE view of these layers in Echus Chasma shows they are rough, with knobs of rock sticking out through the dust and talus (loose debris) on the slope. This indicates that perhaps these layers are made of different materials than the light-toned deposits, which appear more friable in nature. These rough layers may be exposures of lavas, or they might just be more resistant forms of sedimentary rocks. The layers are typical of those seen in chasma slopes and crater rims elsewhere on the Martian surface. This HiRISE image is PSP_002472_1810 [ http://hirise.lpl.arizona.edu/PSP_002472_1810 ]. Observation Geometry Acquisition date: 2 February 2007 Local Mars time: 3:39 PM Degrees latitude (centered): 1.1 ° Degrees longitude (East): 278.6 ° Range to target site: 268.8 km (168.0 miles) Original image scale range: 26.9 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: 7.6 ° Phase angle: 62.4 ° Solar incidence angle: 55 °, with the Sun about 35 ° above the horizon Solar longitude: 178.5 °, 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. |
|
Layers Exposed on Slope in E
…
PIA09590
Sol (our sun)
HiRISE
| Title |
Layers Exposed on Slope in Echus Chasma Region |
| Original Caption Released with Image |
Click on image for larger version The layers seen in the HiRISE subimage of Echus Chasma are very different from the light-toned, thinly bedded layers HiRISE has observed in deposits seen elsewhere in Valles Marineris. The HiRISE view of these layers in Echus Chasma shows they are rough, with knobs of rock sticking out through the dust and talus (loose debris) on the slope. This indicates that perhaps these layers are made of different materials than the light-toned deposits, which appear more friable in nature. These rough layers may be exposures of lavas, or they might just be more resistant forms of sedimentary rocks. The layers are typical of those seen in chasma slopes and crater rims elsewhere on the Martian surface. This HiRISE image is PSP_002472_1810 [ http://hirise.lpl.arizona.edu/PSP_002472_1810 ]. Observation Geometry Acquisition date: 2 February 2007 Local Mars time: 3:39 PM Degrees latitude (centered): 1.1 ° Degrees longitude (East): 278.6 ° Range to target site: 268.8 km (168.0 miles) Original image scale range: 26.9 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: 7.6 ° Phase angle: 62.4 ° Solar incidence angle: 55 °, with the Sun about 35 ° above the horizon Solar longitude: 178.5 °, 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. |
|
Possible Cinder Cone on the
…
PIA09719
Sol (our sun)
HiRISE
| Title |
Possible Cinder Cone on the Southern Flank of Pavonis Mons |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002671_1790 [ http://hirise.lpl.arizona.edu/PSP_002671_1790 ]) is centered on a small cone on the side of one of Mars' giant shield volcanoes. The cone shows some layers of hard rock but most of it is made of relatively soft material. This appears to be an example of a "cinder" cone composed of pieces of lava thrown into the air during a small volcanic eruption. Typically, such eruptions produce fountains of molten lava. Most of the lava would have cooled in this fountain, producing a loose pile of lava rocks. However, it appears that some pulses of the eruption allowed the lava to land without cooling much. These pieces were hot enough to weld together to make the hard layers we see today. The cone is 700 x 1100 m (2300 x 3600 feet) in size, similar to many cinder cones on Earth. In other parts of the image, we see channels carved by lava. It is sometimes difficult to tell if a channel was formed by flowing water or lava, in this case, it is possible to see that lava flows feed out of these channels. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -1.1° Degrees longitude (East): 246.6° Range to target site: 254.5 km (159.1 miles) Original image scale range: 50.9 cm/pixel (with 2 x 2 binning) so objects ~153 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.6° Phase angle: 53.3° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 187.3°, 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. |
|
Possible Cinder Cone on the
…
PIA09719
Sol (our sun)
HiRISE
| Title |
Possible Cinder Cone on the Southern Flank of Pavonis Mons |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002671_1790 [ http://hirise.lpl.arizona.edu/PSP_002671_1790 ]) is centered on a small cone on the side of one of Mars' giant shield volcanoes. The cone shows some layers of hard rock but most of it is made of relatively soft material. This appears to be an example of a "cinder" cone composed of pieces of lava thrown into the air during a small volcanic eruption. Typically, such eruptions produce fountains of molten lava. Most of the lava would have cooled in this fountain, producing a loose pile of lava rocks. However, it appears that some pulses of the eruption allowed the lava to land without cooling much. These pieces were hot enough to weld together to make the hard layers we see today. The cone is 700 x 1100 m (2300 x 3600 feet) in size, similar to many cinder cones on Earth. In other parts of the image, we see channels carved by lava. It is sometimes difficult to tell if a channel was formed by flowing water or lava, in this case, it is possible to see that lava flows feed out of these channels. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:43 PM Degrees latitude (centered): -1.1° Degrees longitude (East): 246.6° Range to target site: 254.5 km (159.1 miles) Original image scale range: 50.9 cm/pixel (with 2 x 2 binning) so objects ~153 cm across are resolved Map-projected scale: 50 cm/pixel and north is up Map-projection: EQUIRECTANGULAR Emission angle: 2.6° Phase angle: 53.3° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 187.3°, 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. |
|
Very Fine Layers in Juventae
…
PIA09709
Sol (our sun)
HiRISE
| Title |
Very Fine Layers in Juventae Chasma |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002590_1765 [ http://hirise.lpl.arizona.edu/PSP_002590_1765 ]) shows a portion of the light-toned layered deposits in Juventae Chasma. Juventae Chasma is a large trough just north of the main part of Valles Marineris, and may have been the source region for giant floods long ago. There are currently several large hills of layered rock on the chasma floor, likely remnants of a deposit which was once more extensive. Among the possible origins of the layered deposits are lake sediments, volcanic material of various origins (possibly erupted under ice), or deposits of aeolian sand and dust. The subimage shows some extremely thin beds within one of the mounds (center). These are probably sheets of material lying nearly flat, and are some of the finest-scale layers observed on Mars. It is possible that in places layer boundaries are accentuated by variable amounts of dark wind-blown dust, which buries the layers in some parts of the image, nevertheless, some of the layering must be extremely thin. The layers are actually even more thin than they appear, since the slope of the mound makes them appear wider. The occurrence of many thin layers indicates many events or variations in deposition while this material was forming. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:43PM Degrees latitude (centered): -3.3° Degrees longitude (East): 298.3° Range to target site: 266.8 km (166.7 miles) Original image scale range: 26.7 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: 2.4° Phase angle: 53.6° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 183.7°, 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. |
|
Very Fine Layers in Juventae
…
PIA09709
Sol (our sun)
HiRISE
| Title |
Very Fine Layers in Juventae Chasma |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002590_1765 [ http://hirise.lpl.arizona.edu/PSP_002590_1765 ]) shows a portion of the light-toned layered deposits in Juventae Chasma. Juventae Chasma is a large trough just north of the main part of Valles Marineris, and may have been the source region for giant floods long ago. There are currently several large hills of layered rock on the chasma floor, likely remnants of a deposit which was once more extensive. Among the possible origins of the layered deposits are lake sediments, volcanic material of various origins (possibly erupted under ice), or deposits of aeolian sand and dust. The subimage shows some extremely thin beds within one of the mounds (center). These are probably sheets of material lying nearly flat, and are some of the finest-scale layers observed on Mars. It is possible that in places layer boundaries are accentuated by variable amounts of dark wind-blown dust, which buries the layers in some parts of the image, nevertheless, some of the layering must be extremely thin. The layers are actually even more thin than they appear, since the slope of the mound makes them appear wider. The occurrence of many thin layers indicates many events or variations in deposition while this material was forming. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:43PM Degrees latitude (centered): -3.3° Degrees longitude (East): 298.3° Range to target site: 266.8 km (166.7 miles) Original image scale range: 26.7 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: 2.4° Phase angle: 53.6° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 183.7°, 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. |
|
Very Fine Layers in Juventae
…
PIA09709
Sol (our sun)
HiRISE
| Title |
Very Fine Layers in Juventae Chasma |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002590_1765 [ http://hirise.lpl.arizona.edu/PSP_002590_1765 ]) shows a portion of the light-toned layered deposits in Juventae Chasma. Juventae Chasma is a large trough just north of the main part of Valles Marineris, and may have been the source region for giant floods long ago. There are currently several large hills of layered rock on the chasma floor, likely remnants of a deposit which was once more extensive. Among the possible origins of the layered deposits are lake sediments, volcanic material of various origins (possibly erupted under ice), or deposits of aeolian sand and dust. The subimage shows some extremely thin beds within one of the mounds (center). These are probably sheets of material lying nearly flat, and are some of the finest-scale layers observed on Mars. It is possible that in places layer boundaries are accentuated by variable amounts of dark wind-blown dust, which buries the layers in some parts of the image, nevertheless, some of the layering must be extremely thin. The layers are actually even more thin than they appear, since the slope of the mound makes them appear wider. The occurrence of many thin layers indicates many events or variations in deposition while this material was forming. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:43PM Degrees latitude (centered): -3.3° Degrees longitude (East): 298.3° Range to target site: 266.8 km (166.7 miles) Original image scale range: 26.7 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: 2.4° Phase angle: 53.6° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 183.7°, 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. |
|
Dunes in Herschel Crater
PIA09718
Sol (our sun)
HiRISE
| Title |
Dunes in Herschel Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002728_1645 [ http://hirise.lpl.arizona.edu/PSP_002728_1645 ]) shows dunes on the floor of Herschel Crater. The steep faces ("slipfaces") are oriented downwind, in the direction of motion of the dunes. One feature of particular interest is the dune-free area downwind of the crater at the image center. Some sand has been trapped in the crater, but the crater prevents the dunes from migrating directly downwind. Sand dunes form naturally as a result of the transport of sand by the wind. The dunes in this image are somewhat crescent-shaped, but are being extended and distorted downwind and merging with nearby dunes, this complex behavior is common in dune fields on Earth. In the southern part of the image the sand lies in sheets rather than well-defined dunes. At high resolution, the dune surfaces are covered in small ripples and scallops, also shaped by the wind. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:45 PM Degrees latitude (centered): -15.1° Degrees longitude (East): 131.9° 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: 0.2° Phase angle: 56.4° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 189.9°, 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. |
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Dunes in Herschel Crater
PIA09718
Sol (our sun)
HiRISE
| Title |
Dunes in Herschel Crater |
| Original Caption Released with Image |
Click on image for larger version This HiRISE image (PSP_002728_1645 [ http://hirise.lpl.arizona.edu/PSP_002728_1645 ]) shows dunes on the floor of Herschel Crater. The steep faces ("slipfaces") are oriented downwind, in the direction of motion of the dunes. One feature of particular interest is the dune-free area downwind of the crater at the image center. Some sand has been trapped in the crater, but the crater prevents the dunes from migrating directly downwind. Sand dunes form naturally as a result of the transport of sand by the wind. The dunes in this image are somewhat crescent-shaped, but are being extended and distorted downwind and merging with nearby dunes, this complex behavior is common in dune fields on Earth. In the southern part of the image the sand lies in sheets rather than well-defined dunes. At high resolution, the dune surfaces are covered in small ripples and scallops, also shaped by the wind. Observation Toolbox Acquisition date: 2 February 2007 Local Mars time: 3:45 PM Degrees latitude (centered): -15.1° Degrees longitude (East): 131.9° 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: 0.2° Phase angle: 56.4° Solar incidence angle: 56°, with the Sun about 34° above the horizon Solar longitude: 189.9°, 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. |
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