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Mars and Crater of Jet Propulsion Laboratory (JPL) and Denver
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High-Resolution MOC Image of
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| title |
High-Resolution MOC Image of Phobos |
| date |
08.19.1998 |
| description |
This image of Phobos, the inner and larger of the two moons of Mars, was taken by the Mars Global Surveyor on August 19, 1998. This image shows a close-up of the largest crater on Phobos, Stickney, 10 kilometers (6 miles) in diameter. Individual boulders are visible on the near rim of the crater, and are presumed to be ejecta blocks from the impact that formed Stickney. Some of these boulders are enormous - more than 50 meters (160 feet) across. Also crossing at and near the rim of Stickney are shallow, elongated depressions called grooves. This crater is nearly half the size of Phobos and these grooves may be fractures caused by its formation. Phobos was observed by both the Mars Orbiter Camera (MOC) and Thermal Emission Spectrometer (TES). This image is one of the highest resolution images (4 meters or 13 feet per picture element or pixel) ever obtained of the Martian satellite. Malin Space Science Systems, Inc. and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Thermal Emission Spectrometer is operated by Arizona State University and was built by Raytheon Santa Barbara Remote Sensing. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. *Image Credit*: Erich Karkoschka (University of Arizona Lunar & Planetary Lab) and NASA |
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High-Resolution MOC Image of
…
| Title |
High-Resolution MOC Image of Phobos |
| Description |
This image of Phobos, the inner and larger of the two moons of Mars, was taken by the Mars Global Surveyor on August 19, 1998. This image shows a close-up of the largest crater on Phobos, Stickney, 10 kilometers (6 miles) in diameter. Individual boulders are visible on the near rim of the crater, and are presumed to be ejecta blocks from the impact that formed Stickney. Some of these boulders are enormous - more than 50 meters (160 feet) across. Also crossing at and near the rim of Stickney are shallow, elongated depressions called grooves. This crater is nearly half the size of Phobos and these grooves may be fractures caused by its formation. Phobos was observed by both the Mars Orbiter Camera (MOC) and Thermal Emission Spectrometer (TES). This image is one of the highest resolution images (4 meters or 13 feet per picture element or pixel) ever obtained of the Martian satellite. Malin Space Science Systems, Inc. and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Thermal Emission Spectrometer is operated by Arizona State University and was built by Raytheon Santa Barbara Remote Sensing. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
| Date |
08.19.1998 |
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High-Resolution MOC Image of
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| Title |
High-Resolution MOC Image of Phobos with Graphics Overlay |
| Description |
This image of Phobos, the inner and larger of the two moons of Mars, was taken by the Mars Global Surveyor on August 19, 1998. The white boxes indicate the location of the subframes or close-ups: that on the left is C and that on the right is D. Each box is 1.92 kilometers (1.19 miles) square. The image shows several new features of this lumpy moon -- features that are associated with the prominent crater seen in the upper left quarter of the image. This is the largest crater on Phobos, Stickney, 10 kilometers (6 miles) in diameter. Individual boulders are visible on the near rim of the crater (D), and are presumed to be ejecta blocks from the impact that formed Stickney. Some of these boulders are enormous - more than 50 meters (160 feet) across. Also crossing at and near the rim of Stickney are shallow, elongated depressions called grooves. This crater is nearly half the size of Phobos and these grooves may be fractures caused by its formation. The far wall of the crater shows lighter and darker streaks going down the slopes (C). Phobos was observed by both the Mars Orbiter Camera (MOC) and Thermal Emission Spectrometer (TES). This image is one of the highest resolution images (4 meters or 13 feet per picture element or pixel) ever obtained of the Martian satellite. Malin Space Science Systems, Inc. and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Thermal Emission Spectrometer is operated by Arizona State University and was built by Raytheon Santa Barbara Remote Sensing. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
| Date |
08.19.1998 |
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High-Resolution MOC Image of
…
| Title |
High-Resolution MOC Image of Phobos' Face |
| Description |
This image of Phobos, the inner and larger of the two moons of Mars, was taken by the Mars Global Surveyor on August 19, 1998. The minimum distance between the spacecraft and Phobos was 1,080 kilometers (671 miles). Phobos was observed by both the Mars Orbiter Camera (MOC) and Thermal Emission Spectrometer (TES). This image is one of the highest resolution images (4 meters or 13 feet per picture element or pixel) ever obtained of the Martian satellite. The image shows several new features of this lumpy moon -- features that are associated with the prominent crater seen in the upper left quarter of the image. This is the largest crater on Phobos, Stickney, 10 kilometers (6 miles) in diameter. Individual boulders are visible on the near rim of the crater (D), and are presumed to be ejecta blocks from the impact that formed Stickney. Some of these boulders are enormous - more than 50 meters (160 feet) across. Also crossing at and near the rim of Stickney are shallow, elongated depressions called grooves. This crater is nearly half the size of Phobos and these grooves may be fractures caused by its formation. The far wall of the crater shows lighter and darker streaks going down the slopes (C). The presence of material of different brightness on the far crater slopes and in some of the grooves shows that the satellite is heterogeneous (that is, it is made of a mixture of different types of materials). The motion of debris down slopes is guided by gravity, which is only about 1/1000th that of the Earth -- e.g., a 68-kilogram (150- pound) person would weigh only about 57 grams (2 ounces) on Phobos. Previous images from the Viking spacecraft in the 1970's were not of sufficient resolution to show the effectiveness of gravity on Phobos in moving material down slopes. Malin Space Science Systems, Inc. and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Thermal Emission Spectrometer is operated by Arizona State University and was built by Raytheon Santa Barbara Remote Sensing. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
| Date |
08.19.1998 |
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High-Resolution MOC Image of
…
| Title |
High-Resolution MOC Image of Phobos' Stickney Crater |
| Description |
This image of Phobos, the inner and larger of the two moons of Mars, was taken by the Mars Global Surveyor on August 19, 1998. This image is a close-up of the far wall of the Stickney crater, 10 kilometers (6 miles) in diameter, that is the largest crater on Phobos. This image shows lighter and darker streaks going down the slopes (C). The presence of material of different brightness on the far crater slopes and in some of the grooves shows that the satellite is heterogeneous (that is, it is made of a mixture of different types of materials). The motion of debris down slopes is guided by gravity, which is only about 1/1000th that of the Earth -- e.g., a 68-kilogram (150-pound) person would weigh only about 57 grams (2 ounces) on Phobos. Phobos was observed by both the Mars Orbiter Camera (MOC) and Thermal Emission Spectrometer (TES). This image is one of the highest resolution images (4 meters or 13 feet per picture element or pixel) ever obtained of the Martian satellite. Malin Space Science Systems, Inc. and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Thermal Emission Spectrometer is operated by Arizona State University and was built by Raytheon Santa Barbara Remote Sensing. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
| Date |
08.19.1998 |
|
Subsection of Nirgal Vallis
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| title |
Subsection of Nirgal Vallis Image |
| Description |
This image is a subsection of the MGS Nirgal Vallis "B" image (PIA00942). This subsection of frame P006_05 is shown here at reduced resolution because the full image is almost 7 MBytes in size. Because the MOC acquires its images one line at a time, the cant angle towards the sun-lit portion of the planet, the spacecraft orbital velocity, and the spacecraft rotational velocity combined to significantly distort the image. However, even in this reduced resolution version, dunes can be seen in the canyon and in areas on the upland surface around the canyon. Nigral Vallis is one of a number of canyons called valley networks or runoff channels. Much of the debate concerning the origin of these valleys centers on whether they were formed by water flowing across the surface, or by collapse and upslope erosion associated with groundwater processes. At the resolution of this image, it is just barely possible to discern an interwoven pattern of lines on the highland surrounding the valley, but it is not possible to tell whether this is a pattern of surficial debris (sand or dust), as might be expected with the amount of crater burial seen, or a pattern of drainage channels. With 4X better resolution from its mapping orbit, MOC should easily be able to tell the difference between these two possibilities. Launched on November 7, 1996, Mars Global Surveyor entered Mars orbit on Thursday, September 11, 1997. The spacecraft has been using atmospheric drag to reduce the size of its orbit for the past three weeks, and will achieve a circular orbit only 400 km (248 mi) above the surface early next year. Mapping operations begin in March 1998. At that time, MOC narrow angle images will be 5-10 times higher resolution than these pictures. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. Photo Credit: NASA/JPL/Malin Space Science Systems MRPS #84722 100297_7 605.crp, a subsection of 605.str/MOC212B 559303731.605 P006_05 |
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Rotated Perspective View of
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| title |
Rotated Perspective View of Nirgal Vallis |
| Description |
This is the full-resolution, rotated perspective image of Nirgal Vallis, a subset of PIA00942. Nigral Vallis is one of a number of canyons called valley networks or runoff channels. Much of the debate concerning the origin of these valleys centers on whether they were formed by water flowing across the surface, or by collapse and upslope erosion associated with groundwater processes. At the resolution of this image, it is just barely possible to discern an interwoven pattern of lines on the highland surrounding the valley, but it is not possible to tell whether this is a pattern of surficial debris (sand or dust), as might be expected with the amount of crater burial seen, or a pattern of drainage channels. With 4X better resolution from its mapping orbit, MOC should easily be able to tell the difference between these two possibilities. Launched on November 7, 1996, Mars Global Surveyor entered Mars orbit on Thursday, September 11, 1997. The spacecraft has been using atmospheric drag to reduce the size of its orbit for the past three weeks, and will achieve a circular orbit only 400 km (248 mi) above the surface early next year. Mapping operations begin in March 1998. At that time, MOC narrow angle images will be 5-10 times higher resolution than these pictures. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. Photo Credit: NASA/JPL/Malin Space Science Systems MRPS #84704 100197_8 605.obl.sub.str/MOC212E 559303731.605 P006_05 |
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MGS Views of Nirgal Vallis
| title |
MGS Views of Nirgal Vallis |
| Description |
At 3:08:30 AM on September 21, 1997, the MOC field of view swept across the highland valley network Nirgal Vallis at 28.5°S, 41.6 W. Although the MGS spacecraft was at an altitude of about 400 km (250 miles), the MOC was pointed obliquely across the planet at about 35°, so the distance to Nirgal Vallis was closer to 800 km (500 miles). At that range and viewing angle, the MOC field of view was about 16 km (10 miles) wide, and the resolution was about 9 meters (30 feet) per pixel. The acquired image is 36 km (23 miles) long. Five images are shown above: (A) is an excerpt from the USGS MDIM, roughly 180 km (112 mile) square. The small box outlines the MOC image acquisition. (B) is MOC frame P006_05, shown here at reduced resolution because the full image is almost 7 MBytes in size. Because the MOC acquires its images one line at a time, the cant angle towards the sun-lit portion of the planet, the spacecraft orbital velocity, and the spacecraft rotational velocity combined to significantly distort the image. However, even in this reduced resolution version, dunes can be seen in the canyon and in areas on the upland surface around the canyon. (C) shows a portion of P006_05 at the full resolution of the data. This view shows the dunes more clearly, and also illustrates better the distortion introduced by the method of data acquisition. (D) shows P006_05 skewed and rotated to the perspective that MOC was viewing at the time the image was taken. (E) shows a full-resolution version of a portion of the rotated perspective view. Nigral Vallis is one of a number of canyons called valley networks or runoff channels. Much of the debate concerning the origin of these valleys centers on whether they were formed by water flowing across the surface, or by collapse and upslope erosion associated with groundwater processes. At the resolution of this image, it is just barely possible to discern an interwoven pattern of lines on the highland surrounding the valley, but it is not possible to tell whether this is a pattern of surficial debris (sand or dust), as might be expected with the amount of crater burial seen, or a pattern of drainage channels. With 4X better resolution from its mapping orbit, MOC should easily be able to tell the difference between these two possibilities. Launched on November 7, 1996, Mars Global Surveyor entered Mars orbit on Thursday, September 11, 1997. The spacecraft has been using atmospheric drag to reduce the size of its orbit for the past three weeks, and will achieve a circular orbit only 400 km (248 mi) above the surface early next year. Mapping operations begin in March 1998. At that time, MOC narrow angle images will be 5-10 times higher resolution than these pictures. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor, Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. Photo Credit: NASA/JPL/Malin Space Science Systems MRPS #84721 100297_2 605.all.str consisting of 605.ctx.str/MOC212A, 605.str/MOC212B, 605.sub.str/MOC212C, 605.obl.str/ MOC212D, and 605.obl.sub.str/MOC212E 559303731.605 P006_05 |
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| Description |
Figure C: The third picture shows a small crater on the rim of a larger crater. Only a small portion of the wall of this larger crater is captured in the image. Immediately beneath the small crater occurs a group of gullies. The presence of these gullies also supports the groundwater hypothesis because impacting meteors will fracture the rocks into which they form a crater. In this case, there would be an initial set of subsurface fractures caused by the large impact that created the original, large crater. Then, when the smaller crater formed, it would have created additional fractures in its vicinity. These extra fractures would then have provided pathways, or conduits, through which ground water would come to the surface on the wall of the larger crater, thus creating the gullies observed. One might speculate that the group of gullies was formed by the impact that made the small crater, because of the heat and fracturing of rock during the impact process. However, the gullies are much younger than the small crater, the ejecta from the small crater has been largely eroded away or buried, and the crater partially filled, while the gullies appear sharp, crisp and fresh. This is a portion of an image located near 33.9 degrees south latitude, 160 degrees west longitude, acquired on March 31, 2006. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by NASA's Jet Propulsion Laboratory, Pasadena, Calif., a division of the California Institute of Technology, also in Pasadena. Lockheed Martin Space Systems, Denver, developed and operates the spacecraft. Malin Space Science Systems, San Diego, Calif., built and operates the Mars Orbiter Camera. For more information about images from the Mars Orbiter Camera, see http://www.msss.com/mgs/moc/index.html [ http://www.msss.com/mgs/moc/index.html ]. |
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Apollinaris Patera
| title |
Apollinaris Patera |
| Description |
This month (April 1999), the Mars Global Surveyor Mars Orbiter Camera (MOC) passed over the Apollinaris Patera volcano and captured a patch of bright clouds hanging over its summit in the early martian afternoon. This ancient volcano is located near the equator and--based on observations from the 1970s Viking Orbiters--is thought to be as much as 5 kilometers (3 miles) high. The caldera--the semi-circular crater at the volcano summit--is about 80 kilometers (50 miles) across. The color in this picture was derived from the MOC red and blue wide angle camera systems and does not represent true color as it would appear to the human eye (that is, if a human were in a position to be orbiting around the red planet). Illumination is from the upper left. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. Photo Credit: NASA/JPL/Malin Space Science Systems |
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Gusev Crater
| title |
Gusev Crater |
| Description |
This mosaic of nighttime infrared images of Gusev Crater, taken by the camera system on the Mars Odyssey spacecraft, has been draped over topography data obtained by Mars Global Surveyor. Variations in nighttime temperatures are due to differences in the abundance of rocky materials that retain their heat at night and stay relatively warm (bright). Fine grained dust and sand (dark) cools off more rapidly at night. This image mosaic covers an area approximately 180 kilometers (110 miles) on each side centered near 14 degrees S, 175 degrees E, looking toward the south in this simulated view. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The thermal emission imaging system was provided by Arizona State University, Tempe. Lockheed Martin Astronautics, Denver, Colo., is the prime contractor for the project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. Credit: NASA/JPL/Arizona State University |
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Western Arcadia Planitia
| title |
Western Arcadia Planitia |
| Description |
This is a Mars Odyssey visible color image of an unnamed crater in western Arcadia Planitia (near 39 degrees N, 179 degrees E). The crater shows a number of interesting internal and external features that suggest that it has undergone substantial modification since it formed. These features include concentric layers and radial streaks of brighter, redder materials inside the crater, and a heavily degraded rim and ejecta blanket. The patterns inside the crater suggest that material has flowed or slumped towards the center. Other craters with features like this have been seen at both northern and southern mid latitudes The distribution of these kinds of craters suggests the possible influence of surface or subsurface ice in the formation of these enigmatic features. The image was taken on September 29, 2002 during late northern spring. This is an approximate true color image, generated from a long strip of visible red (654 nm), green (540 nm), and blue (425 nm) filter images that were calibrated using a combination of pre-flight measurements and Hubble images of Mars. The colors appear perhaps a bit darker than one might expect, this is most likely because the images were acquired in late afternoon (roughly 4:40 p.m. local solar time) and the low Sun angle results in an overall darker surface. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The thermal emission imaging system was provided by Arizona State University, Tempe. Lockheed Martin Astronautics, Denver, Colo., is the prime contractor for the project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. Credit: NASA/JPL/Arizona State University/Cornell University |
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Gusev Crater
| title |
Gusev Crater |
| Description |
This mosaic of daytime infrared images of Gusev Crater, taken by the camera system on the Mars Odyssey spacecraft, has been draped over topography data obtained by Mars Global Surveyor. The daytime temperatures range from approximately minus 45 degrees C (black) to minus 5 degrees C (white). The temperature differences in these daytime images are due primarily to lighting effects, where sunlit slopes are warm (bright) and shadowed slopes are cool (dark). Gusev crater is a potential landing site for the Mars Exploration Rovers. The large ancient river channel of Ma'Adim that once flowed into Gusev can be seen at the top of the mosaic. This image mosaic covers an area approximately 180 kilometers (110 miles) on each side centered near 14 degrees S, 175 degrees E, looking toward the south in this simulated view. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The thermal emission imaging system was provided by Arizona State University, Tempe. Lockheed Martin Astronautics, Denver, Colo., is the prime contractor for the project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. Credit: NASA/JPL/Arizona State University |
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Odyssey/ Becquerel
| title |
Odyssey/ Becquerel |
| Description |
These images from Mars Odyssey look at the Becquerel crater in different lights -- visible, daytime infrared and nighttime infrared. The daytime images (left and center) were acquired on March 28, 2002 and the nighttime image (right) was acquired on March 2, 2002, by the thermal emission imaging system aboard Mars Odyssey. Thermal infrared is the wavelength range associated with heat. Looking at the Martian surface in the infrared wavelengths allows scientists to identify and distinguish bedrock from sand or dust covered areas. The Becquerel deposit is relatively bright in the visible wavelengths. Its surface has been scoured by windblown sand to produce the ridged topography seen in the visible image, which spans an 18-kilometer (11 mile)-wide portion of the deposit. Dark sand is seen in the lower right of the visible image. This same scene in the 32-kilometer (20 mile)-wide daytime infrared image looks remarkably similar to a photographic negative of the visible image due to the effects of solar heating. Darker tones represent cooler surfaces, brighter tones are warmer ones. During the day, visibly dark surfaces heat up much more efficiently than bright surfaces. The relatively bright sediments of the mound reflect more solar energy than the darker sand, allowing the mound to stay cooler than the sand. In the nighttime infrared image, the mound and the sand are warmer than their surroundings. The dark portions of the image represent cold surfaces that are covered in dust particles. Dust does not retain heat during the cold Martian night and quickly gives up any heat received during the day. Sand particles, because they are larger than dust particles, are able to retain heat better, producing the brighter swath around the mound. The infrared image has a resolution of 100 meters (328 feet) per pixel and is 32 kilometers (20 miles) wide. The visible image has a resolution of 18 meters per pixel and is approximately 18 kilometers (11 miles) wide. The images are centered at 21.4 degrees north latitude and 351.8 degrees east longitude. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. Credit: NASA/JPL/Arizona State University |
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Odyssey/White Rock
| title |
Odyssey/White Rock |
| Description |
These Mars Odyssey images show the "White Rock" feature on Mars in both infrared (left) and visible (right) wavelengths. The images were acquired simultaneously on March 11, 2002. The box shows where the visible image is located in the infrared image. "White Rock" is the unofficial name for this unusual landform that was first observed during the Mariner 9 mission in the early 1970's. The variations in brightness in the infrared image are due to differences in surface temperature, where dark is cool and bright is warm. The dramatic differences between the infrared and visible views of White Rock are the result of solar heating. The relatively bright surfaces observed at visible wavelengths reflect more solar energy than the darker surfaces, allowing them to stay cooler and thus they appear dark in the infrared image. The new thermal emission imaging system data will help to address the long standing question of whether the White Rock deposit was produced in an ancient crater lake or by dry processes of volcanic or wind deposition. The infrared image has a resolution of 100 meters (328 feet) per pixel and is 32 kilometers (20 miles) wide. The visible image has a resolution of 18 meters per pixel and is approximately 18 kilometers (11 miles) wide. The images are centered at 8.2 degrees south latitude and 24.9 degrees east longitude. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. Credit: NASA/JPL/Arizona State University |
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Martian Dunes in Infrared
| title |
Martian Dunes in Infrared |
| Description |
This collage of six images taken by the camera system on NASA's Mars Odyssey, shows examples of the daytime temperature patterns of martian dunes seen by the infrared camera. The dunes can be seen in this daytime image because of the temperature differences between the sunlit (warm and bright) and shadowed (cold and dark) slopes of the dunes. The temperatures in each image vary, but typically range from approximately -35 degrees Celsius (-31 degrees Fahrenheit) to -15 degrees Celsius (5 degrees Fahrenheit). Each image covers an area approximately 32 by 32 kilometers (20 by 20 miles) and was acquired using the infrared Band 9, centered at 12.6 micrometers. Clockwise from the upper left, these images are: (a) Russel crater, 54 degrees south latitude, 13 degrees east longitude, (b) Kaiser crater. 45 degrees south latitude, 19 degrees east longitude, (c) Rabe crater, 43 south latitude, 35 east longitude, (d) 22 north latitude, 66 degrees east longitude, (e) Proctor crater. 47 degrees south latitude, 30 degrees east longitude, (f) 61 degrees south latitude, 201 degrees east longitude. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the 2001 Mars Odyssey mission for NASA's Office of Space Science in Washington, D.C. Investigators at Arizona State University in Tempe, the University of Arizona in Tucson and NASA's Johnson Space Center, Houston, operate the science instruments. Additional science partners are located at the Russian Aviation and Space Agency and at Los Alamos National Laboratories, New Mexico. Lockheed Martin Astronautics, Denver, is the prime contractor for the project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL. Image credit: NASA/JPL/Arizona State University. |
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| Description |
A further zoom emphasizes a small, fresh crater about 350 meters (1,150 feet) in diameter near the center of the scene. The adjacent cliff contains numerous individual layers. An unusual set of small mesas, seen in the lower right part of the image, is being eroded from the polar layered material. The images making up this mosaic have a spatial resolution of 36 meters (118 feet) per pixel, allowing detection of features as small as 75 to 100 meters (246 to 328 feet) across. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for the NASA Office of Space Science, Washington. The thermal emission imaging system on Odyssey was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. Lockheed Martin Space Systems, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. Credit: NASA/JPL/Arizona State University ### |
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Mars Odyssey All Stars - Udz
…
marscollection, nasa
Although it is 45 kilometers
…
504646main_pia13657-43
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2010-12-08 |
| creator |
NASA |
| identifier |
504646main_pia13657-43 |
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Mars Odyssey All Stars - Bun
…
marscollection, nasa
Fans and ribbons of dark san
…
504750main_pia13654b
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2010-12-08 |
| creator |
NASA |
| identifier |
504750main_pia13654b |
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Mars Odyssey All Stars -- Ar
…
marscollection, nasa
Sand dunes shaped like blue-
…
504660main_pia13658
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2010-12-08 |
| creator |
NASA |
| identifier |
504660main_pia13658 |
|
Mars Odyssey All Stars -- Du
…
marscollection, nasa
If a meteorite breaks in two
…
504693main_pia13660
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2010-12-08 |
| creator |
NASA |
| identifier |
504693main_pia13660 |
|
Mars Odyssey All Stars -- Du
…
marscollection, nasa
A vast dune field lies near
…
504704main_pia13661
| mediatype |
IMAGE |
| mediatype |
image |
| date |
2010-12-08 |
| creator |
NASA |
| identifier |
504704main_pia13661 |
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Channels on Bakhuysen Crater
…
PIA01506
Sol (our sun)
Mars Orbiter Camera
| Title |
Channels on Bakhuysen Crater Wall |
| Original Caption Released with Image |
Portion of channels on the wall of Bakhuysen crater (MOC 10605). These channels (22.1°S, 344.9°W) are the best examples of integrated drainage reminiscent of terrestrial systems. The pattern is topographically controlled, the relationships emphasized by light-colored sediments viewed in this low incidence angle (11.2°), nadir viewing (emission angle = 1.5°) image. The crater rim is marked by the escarpment running diagonally in the middle left to upper right of the image (downtrack scale = 8.4 m/pixel, crosstrack = 5.8 m/pixel). No channels outside the crater rim. This suggests that the source of the fluid was confined within the crater. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Gusev Crater
PIA04261
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Gusev Crater |
| Original Caption Released with Image |
This mosaic of nighttime infrared images of Gusev Crater, taken by the camera system on the Mars Odyssey spacecraft, has been draped over topography data obtained by Mars Global Surveyor. Variations in nighttime temperatures are due to differences in the abundance of rocky materials that retain their heat at night and stay relatively warm (bright). Fine grained dust and sand (dark) cools off more rapidly at night. This image mosaic covers an area approximately 180 kilometers (110 miles) on each side centered near 14 degrees S, 175 degrees E, looking toward the south in this simulated view. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The thermal emission imaging system was provided by Arizona State University, Tempe. Lockheed Martin Astronautics, Denver, Colo., is the prime contractor for the project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Gusev Crater
PIA04260
Sol (our sun)
Thermal Emission Imaging Sys
…
| Title |
Gusev Crater |
| Original Caption Released with Image |
This mosaic of daytime infrared images of Gusev Crater, taken by the camera system on the Mars Odyssey spacecraft, has been draped over topography data obtained by Mars Global Surveyor. The daytime temperatures range from approximately minus 45 degrees C (black) to minus 5 degrees C (white). The temperature differences in these daytime images are due primarily to lighting effects, where sunlit slopes are warm (bright) and shadowed slopes are cool (dark). Gusev crater is a potential landing site for the Mars Exploration Rovers. The large ancient river channel of Ma'Adim that once flowed into Gusev can be seen at the top of the mosaic. This image mosaic covers an area approximately 180 kilometers (110 miles) on each side centered near 14 degrees S, 175 degrees E, looking toward the south in this simulated view. NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The thermal emission imaging system was provided by Arizona State University, Tempe. Lockheed Martin Astronautics, Denver, Colo., is the prime contractor for the project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. |
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Flow Ejecta and Slope Landsl
…
PIA01156
Sol (our sun)
Mars Orbiter Camera
| Title |
Flow Ejecta and Slope Landslides in Small Crater - High Resolution Image |
| Original Caption Released with Image |
This high resolution picture of a moderately small impact crater on Mars was taken by the Mars Global Surveyor Orbiter Camera (MOC) on October 17, 1997 at 4:11:07 PM PST, during MGS orbit 22. The image covers an area 2.9 by 48.4 kilometers (1.8 by 30 miles) at 9.6 m (31.5 feet) per picture element, and is centered at 21.3 degrees N, 179.8 degrees W, near Orcus Patera. The MOC image is a factor of 15X better than pervious Viking views of this particular crater. The unnamed crater is one of three closely adjacent impact features that display the ejecta pattern characteristic of one type of "flow-ejecta" crater. Such patterns are considered evidence of fluidized movement of the materials ejected during the cratering event, and are believed to indicate the presence of subsurface ice or liquid water. Long, linear features of different brightness values can be seen on the on the steep slopes inside and outside the crater rim. This type of feature, first identified in Viking Orbiter images acquired over 20 years ago, are more clearly seen in this new view (about 3 times better than the best previous observations). Their most likely explanation is that small land or dirt slides, initiated by seismic or wind action, have flowed down the steep slopes. Initially dark because of the nature of the surface disturbance, these features get lighter with time as the ubiquitous fine, bright dust settles onto them from the martian atmosphere. Based on estimates of the dust fall-out rate, many of these features are probably only a few tens to hundreds of years old. Thus, they are evidence of a process that is active on Mars today. Malin Space Science Systems (MSSS) and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Schiaparelli Crater Rim and
…
PIA01157
Sol (our sun)
Mars Orbiter Camera
| Title |
Schiaparelli Crater Rim and Interior Deposits |
| Original Caption Released with Image |
A portion of the rim and interior of the large impact crater Schiaparelli is seen at different resolutions in images acquired October 18, 1997 by the Mars Global Surveyor Orbiter Camera (MOC) and by the Viking Orbiter 1 twenty years earlier. The left image is a MOC wide angle camera "context" image showing much of the eastern portion of the crater at roughly 1 km (0.6 mi) per picture element. The image is about 390 by 730 km (240 X 450 miles). Shown within the wide angle image is the outline of a portion of the best Viking image (center, 371S53), acquired at a resolution of about 240 m/pixel (790 feet). The area covered is 144 X 144 km (89 X 89 miles). The right image is the high resolution narrow angle camera view. The area covered is very small--3.9 X 10.2 km (2.4 X 6.33 mi)--but is seen at 63 times higher resolution than the Viking image. The subdued relief and bright surface are attributed to blanketing by dust, many small craters have been completely filled in, and only the most recent (and very small) craters appear sharp and bowl-shaped. Some of the small craters are only 10-12 m (30-35 feet) across. Occasional dark streaks on steeper slopes are small debris slides that have probably occurred in the past few decades. The two prominent, narrow ridges in the center of the image may be related to the adjustment of the crater floor to age or the weight of the material filling the basin. Malin Space Science Systems (MSSS) and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Flow-ejecta Crater in Icaria
…
PIA01162
Sol (our sun)
Mars Orbiter Camera
| Title |
Flow-ejecta Crater in Icaria Planum - High Resolution Image |
| Original Caption Released with Image |
The Mars Global Surveyor Orbiter Camera (MOC) acquired this high resolution image of a flow ejecta crater on November 19, 1997, at 8:26 PM PST, about 18 minutes after the start the 45th orbit of Mars. The area shown is roughly 6.5 by 40.2 kilometers (4 by 25 miles), and is located near 40 degrees South latitude, 120 degrees West longitude. Features as small as 15-18 m (50-60 feet) across are visible in the picture. Flow ejecta craters are so named because the material blasted out of the crater during the impact process appears to have flowed across the surface of Mars. First seen in Mariner 9 images in 1973, and described in detail using Viking Orbiter images acquired in 1976-78, flow-ejecta craters are considered by many scientists to be evidence that liquid water could be found in the near-subsurface at the time the craters formed. This image, a factor of two better than any previous view of such features (and a factor of 33 better than the best Viking frame of the specific crater, 056A61), shows two smaller, pre-existing craters and the interaction of the flowing ejecta with these craters. The uppermost small crater has been over-topped and partly buried by the flow, while the flow has been diverted around the lower crater. Ridges formed where the flow "stacked up" behind obstacles, or came to rest. Malin Space Science Systems (MSSS) and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Flow-ejecta Crater in Icaria
…
PIA01161
Sol (our sun)
Mars Orbiter Camera
| Title |
Flow-ejecta Crater in Icaria Planum |
| Original Caption Released with Image |
The Mars Global Surveyor Orbiter Camera (MOC) acquired this high resolution image of a flow ejecta crater on November 19, 1997, at 8:26 PM PST, about 18 minutes after the start the 45th orbit of Mars. The area shown is roughly 6.5 by 40.2 kilometers (4 by 25 miles), and is located near 40 degrees South latitude, 120 degrees West longitude. Features as small as 15-18 m (50-60 feet) across are visible in the picture. Flow ejecta craters are so named because the material blasted out of the crater during the impact process appears to have flowed across the surface of Mars. First seen in Mariner 9 images in 1973, and described in detail using Viking Orbiter images acquired in 1976-78, flow-ejecta craters are considered by many scientists to be evidence that liquid water could be found in the near-subsurface at the time the craters formed. This image (right), a factor of two better than any previous view of such features (and a factor of 33 better than the best Viking frame of the specific crater, 056A61, left), shows two smaller, pre-existing craters and the interaction of the flowing ejecta with these craters. The uppermost small crater has been over-topped and partly buried by the flow, while the flow has been diverted around the lower crater. Ridges formed where the flow "stacked up" behind obstacles, or came to rest. Malin Space Science Systems (MSSS) and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Schiaparelli Crater Rim and
…
PIA01158
Sol (our sun)
Mars Orbiter Camera
| Title |
Schiaparelli Crater Rim and Interior Deposits - High Resolution Image |
| Original Caption Released with Image |
A portion of the rim and interior of the large impact crater Schiaparelli is seen at high resolution in this image acquired October 18, 1997 by the Mars Global Surveyor Orbiter Camera (MOC). The area covered is very small--3.9 X 10.2 km (2.4 X 6.33 mi)--but is seen at 63 times higher resolution than the Viking image. The subdued relief and bright surface are attributed to blanketing by dust, many small craters have been completely filled in, and only the most recent (and very small) craters appear sharp and bowl-shaped. Some of the small craters are only 10-12 m (30-35 feet) across. Occasional dark streaks on steeper slopes are small debris slides that have probably occurred in the past few decades. The two prominent, narrow ridges in the center of the image may be related to the adjustment of the crater floor to age or the weight of the material filling the basin. Malin Space Science Systems (MSSS) and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Flow Ejecta and Slope Landsl
…
PIA01155
Sol (our sun)
Mars Orbiter Camera
| Title |
Flow Ejecta and Slope Landslides in Small Crater |
| Original Caption Released with Image |
This high resolution picture of a moderately small impact crater on Mars was taken by the Mars Global Surveyor Orbiter Camera (MOC) on October 17, 1997 at 4:11:07 PM PST, during MGS orbit 22. The image covers an area 2.9 by 48.4 kilometers (1.8 by 30 miles) at 9.6 m (31.5 feet) per picture element, and is centered at 21.3 degrees N, 179.8 degrees W, near Orcus Patera. The MOC image is a factor of 15X better than pervious Viking views of this particular crater (left, Viking image 545A49). The unnamed crater is one of three closely adjacent impact features that display the ejecta pattern characteristic of one type of "flow-ejecta" crater. Such patterns are considered evidence of fluidized movement of the materials ejected during the cratering event, and are believed to indicate the presence of subsurface ice or liquid water. Long, linear features of different brightness values can be seen on the on the steep slopes inside and outside the crater rim. This type of feature, first identified in Viking Orbiter images acquired over 20 years ago, are more clearly seen in this new view (about 3 times better than the best previous observations). Their most likely explanation is that small land or dirt slides, initiated by seismic or wind action, have flowed down the steep slopes. Initially dark because of the nature of the surface disturbance, these features get lighter with time as the ubiquitous fine, bright dust settles onto them from the martian atmosphere. Based on estimates of the dust fall-out rate, many of these features are probably only a few tens to hundreds of years old. Thus, they are evidence of a process that is active on Mars today. Malin Space Science Systems (MSSS) and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Small Valley Network Near Sc
…
PIA01508
Sol (our sun)
Mars Orbiter Camera
| Title |
Small Valley Network Near Schiaparelli Crater |
| Original Caption Released with Image |
Mars Orbiter Camera image 36204 shows a small Martian valley network east of the impact basin Schiaparelli near 1.5°S, 335°W. One of the lowest resolution views taken by MOC during its first year in orbit (original scale is 16 m per picture element), it nonetheless illustrates important attributes of the valley networks. The area is heavily blanketed with windblown dust and sand (the latter seen as dunes within the valley). The upland surface shows tributaries about 1 km across, but none smaller. Since impact craters smaller than 1 km are preserved but often mantled, the smaller tributaries, if formed by surface runoff from precipitation, should be visible. Their absence suggests that groundwater processes have played a more substantive role in the formation of the valley systems than rainfall. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Northern Plains Textures Vis
…
PIA01697
Sol (our sun)
Mars Orbiter Camera
| Title |
Northern Plains Textures Visible Near the Terminator |
| Original Caption Released with Image |
Each day, Mars Global Surveyor makes 12 orbits around the red planet. On each orbit at the present time (April 1999), the spacecraft passes from daylight into night somewhere over the northern plains of Mars, and re-emerges into daylight over the southern cratered highlands. The illumination conditions near the martian terminator--the line between night and day--are perfect for observing surface texture and topography. This picture shows a common, rough and bumpy texture that MOC has revealed on the northern plains of Mars. Note the eroded impact crater at the bottom right--small black dots along its rim are interpreted to be boulders. This image covers an area 3 kilometers (1.9 miles) wide by 8 kilometers (5 miles) long and is illuminated by the sun shining low from the northeastern horizon(from the upper right). Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Mariner 4 Meets Mars Global
…
PIA01685
Sol (our sun)
Mars Orbiter Camera
| Title |
Mariner 4 Meets Mars Global Surveyor--Mariner Crater 1965 and 1999 |
| Original Caption Released with Image |
Mars exploration in the last half of the 20th Century comes full circle with a modern view of Mariner Crater obtained by the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) in early March 1999. Mariner 4 was the first spacecraft to reach the red planet and take close-up pictures that revealed its ancient, cratered surface. The picture on the left, above, is the 11th image taken by Mariner 4 during its July 1965 flyby. The center of the Mariner 4 image is dominated by a crater that is about 155 kilometers (96 miles) in diameter and located at 32°S latitude and 164°W longitude. The crater was named "Mariner" in 1967 by the International Astronomical Union in honor of its discovery by Mariner 4. The white arrow indicates the location of the new MGS MOC image. The picture on the right represents an improvement in resolution of almost a factor of 400. It shows a view of a tiny portion of the southeastern floor of Mariner Crater, as it appeared to the MGS MOC in 1999. In 1965, it was a surprise to find that the martian surface is pocked with craters. In 1999, using the MGS MOC, we now have the ability to see objects the size of automobiles on the martian surface. This view of the Mariner Crater floor has a spatial resolution of 1.5 meters(5 feet) per pixel and covers an area only 1.5 km (0.9 mi) wide by 2.2 km (1.4 mi)long. Illumination is from the upper left in both the Mariner and MGS images. For a mercator-projected Viking 1 Orbiter view of this crater (obtained in 1978)click here. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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High Resolution View of Nort
…
PIA01677
Sol (our sun)
Mars Orbiter Camera
| Title |
High Resolution View of Northern Plains Surface |
| Original Caption Released with Image |
Until now, the vast northern plains of Mars have largely eluded the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) because these plains were obscured by winter and springtime clouds during most of the 1997 and 1998 Aerobraking and Science Phasing portions of the MGS Mission. However, now in March 1999 it is summertime in the northern hemisphere of Mars, and the northern plains are clearly in view. This image was taken at a resolution of 3 meters (10 feet) per pixel in order to characterize the nature of these plains. The image is located near Lomonosov Crater on the Vastitas Borealis plain. The image shows a patterned surface with two distinct rings that are suspected to be the locations of buried impact craters. The larger such ring (right) has dark spots clustered in several patches along its margins--these are fields boulders and rocks. The image covers an area 3 kilometers (1.9 miles) across and is illuminated from the lower left. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Patches of Remnant Frost/Sno
…
PIA01688
Sol (our sun)
Mars Orbiter Camera
| Title |
Patches of Remnant Frost/Snow on Crater Rim in Northern Summer |
| Original Caption Released with Image |
March 1999--it is summer in the martian northern hemisphere, yet patches of frost or snow persist in some areas of the northern plains. Winter ended eight months earlier, in July 1998. Recently, the Mars Orbiter Camera (MOC) passed over a relatively small impact crater located at latitude 68°N (on the Vastitas Borealis plain, north of Utopia Planitia) and took the picture seen at the left, above. The curved crater rims are visible in the upper and lower quarters of the image, and the crater floor is visible at the center right. The picture on the right is a magnified view of the crater rim area outlined by a white box in the image on the left. The bright patches are snow or frost left over from the martian winter. These snowfields are so small that a human could walk across one of them in a matter of minutes--or perhaps sled down the small, sloping patch that is seen in a shadowed area near the lower left. In winter, the entire scene shown here would be covered by frost. The long strip at the left covers an area 3 km (1.9 mi) wide by 26 km (16 mi) long. The expanded view on the right covers an area 2.9 km (1.8 mi) by 5.3 km (3.3 mi). Illumination is from the upper right. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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A Complex, Ridged Terrain in
…
PIA01699
Sol (our sun)
Mars Orbiter Camera
| Title |
A Complex, Ridged Terrain in North Terra Cimmeria |
| Original Caption Released with Image |
Mars Global Surveyor's Mars Orbiter Camera continues to reveal a surface of variety. Never before has Mars been scrutinized in such detail, with images sampling narrow strips of terrain that are as varied as the surface of our own Earth. This picture provides an example of just how strange Mars looks at this new resolution. This surface--located in northern Terra Cimmeria about 210 km (130 mi)southwest of Gusev Crater--shows rounded, rocky ridges separated by lowlands filled with sand or dust. The fill--whether sand or dust--is probably hardened to form a surface strong enough to have bright windblown ripples and small impact craters on it. This picture covers an area 3 km (1.9 mi) wide by 3.9 km (2.4 mi) and is illuminated from the upper left. By the way, do you see a duck in this picture? Look carefully. If you give up, click here! [ http://www.msss.com/mars/global_surveyor/camera/images/4_8_99_bumpy/quack.html ] Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Craters and Bright Dunes of
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PIA01678
Sol (our sun)
Mars Orbiter Camera
| Title |
Craters and Bright Dunes of Isidis Planitia |
| Original Caption Released with Image |
In this first week of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC)Mapping operations--i.e., early March 1999--seeing the red planet at 1.5 meters(5 feet) per pixel is quite a new and novel experience. This picture covers a 1.5 kilometer (0.9 miles) wide portion of Isidis Planitia. A person could walk across this scene in a matter of minutes. That person would encounter a variety of small, bright dunes that are perhaps only a few meters/yards high. Careful exploration would also show that the rims of the younger impact craters have rocks and boulders on them (e.g., see crater at center of the picture). Many more images of this quality and resolution lie ahead for MOC as it begins its 687-day Mapping mission. In this picture, the Sun's illumination is from the upper left. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Floor of Alexey Tolstoy Crat
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PIA01687
Sol (our sun)
Mars Orbiter Camera
| Title |
Floor of Alexey Tolstoy Crater |
| Original Caption Released with Image |
The circular, polar orbit of Mars Global Surveyor (MGS) achieved in early 1999 has begun to provide many opportunities to examine features in the martian southern hemisphere at high resolution. One of our favorite examples (thus far) is this picture of a small portion of the floor of Alexey Tolstoy Crater. The top of the image shows a dark surface that is extremely rough and rocky. The rest of the image shows a brighter, smoother material. It appears that the bright material has been eroded back, exposing the lower, darker surface. The small crater that dominates this picture is only about 850 meters (930 yards) wide and has also been partly exhumed/exposed from beneath the bright, smooth material. Illumination is from the upper left. Alexey (or Aleksey) Tolstoy Crater, in which the small unnamed crater seen in this picture occurs, was named by the International Astronomical Union in 1982 to honor the Soviet writer who died in 1945. It is one of only a few craters on Mars designated by both the first and last names of the honored person. The Alexey Tolstoy Crater has a diameter of 94 kilometers (58 miles) and is centered at 47.6°S latitude, 234.6°W longitude in eastern Promethei Terra. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Once Pitted, Twice Spied: A
…
PIA02007
Sol (our sun)
Mars Orbiter Camera
| Title |
Once Pitted, Twice Spied: A New High Resolution View Inside Escalante Crater |
| Original Caption Released with Image |
During the year spent waiting to achieve the planned circular, polar Mapping Orbit, the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) took about 1170pictures that had resolutions in the 2 to 20 meters (7-66 feet) per pixel range. These pictures were obtained between September 1997 and September 1998, and are now archived with NASA and available to the public at NASAPDS--http://ida.wr.usgs.gov/ [ http://ida.wr.usgs.gov/ ] . Although these pictures were generally a vast improvement in spatial resolution compared to the previous images from Viking and Mariner, the latest pictures from MOC--taken this month (April 1999) from the proper Mapping Orbit--demonstrate the power of the MOC when in focus and operating at the correct altitude (~380 km or 235 miles). The Viking Orbiter picture on the left, above, shows the 83 kilometers-(52 miles)-wide crater, Escalante. Located on the martian equator at 245°W longitude, a portion of this crater's floor was seen by MOC before the mapping mission began, at a resolution of 9.4 meters (31 feet) per pixel as shown in the middle image. The new picture--on the right--peers down into one of the pits seen in the earlier MOC image--only now it is viewed at 1.8 meters (6 feet) per pixel. The new high resolution image (right) covers an area only 1.5 kilometers (0.9 miles)wide and shows that the crater floor--which appears relatively smooth in the context view on the left--is actually quite rough at the scale that a human being would notice if trying to hike around in this landscape. The latest picture also shows small, bright windblown dunes that were not visible in the earlier MOC image. MOC2-120a is a mosaic of Viking Orbiter images 381s62 and 379s47, and MOC2-120b is a subframe of MGS MOC image SPO-2-382/04. The large white box shows the location of MOC2-120b, and the small white box shows the location of MOC2-120c. In MOC2-120a and MOC2-120b, illumination is from the right/upper right, in MOC2-120c it is from the left. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Once Pitted, Twice Spied: A
…
PIA02007
Sol (our sun)
Mars Orbiter Camera
| Title |
Once Pitted, Twice Spied: A New High Resolution View Inside Escalante Crater |
| Original Caption Released with Image |
During the year spent waiting to achieve the planned circular, polar Mapping Orbit, the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) took about 1170pictures that had resolutions in the 2 to 20 meters (7-66 feet) per pixel range. These pictures were obtained between September 1997 and September 1998, and are now archived with NASA and available to the public at NASAPDS--http://ida.wr.usgs.gov/ [ http://ida.wr.usgs.gov/ ] . Although these pictures were generally a vast improvement in spatial resolution compared to the previous images from Viking and Mariner, the latest pictures from MOC--taken this month (April 1999) from the proper Mapping Orbit--demonstrate the power of the MOC when in focus and operating at the correct altitude (~380 km or 235 miles). The Viking Orbiter picture on the left, above, shows the 83 kilometers-(52 miles)-wide crater, Escalante. Located on the martian equator at 245°W longitude, a portion of this crater's floor was seen by MOC before the mapping mission began, at a resolution of 9.4 meters (31 feet) per pixel as shown in the middle image. The new picture--on the right--peers down into one of the pits seen in the earlier MOC image--only now it is viewed at 1.8 meters (6 feet) per pixel. The new high resolution image (right) covers an area only 1.5 kilometers (0.9 miles)wide and shows that the crater floor--which appears relatively smooth in the context view on the left--is actually quite rough at the scale that a human being would notice if trying to hike around in this landscape. The latest picture also shows small, bright windblown dunes that were not visible in the earlier MOC image. MOC2-120a is a mosaic of Viking Orbiter images 381s62 and 379s47, and MOC2-120b is a subframe of MGS MOC image SPO-2-382/04. The large white box shows the location of MOC2-120b, and the small white box shows the location of MOC2-120c. In MOC2-120a and MOC2-120b, illumination is from the right/upper right, in MOC2-120c it is from the left. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Once Pitted, Twice Spied: A
…
PIA02007
Sol (our sun)
Mars Orbiter Camera
| Title |
Once Pitted, Twice Spied: A New High Resolution View Inside Escalante Crater |
| Original Caption Released with Image |
During the year spent waiting to achieve the planned circular, polar Mapping Orbit, the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) took about 1170pictures that had resolutions in the 2 to 20 meters (7-66 feet) per pixel range. These pictures were obtained between September 1997 and September 1998, and are now archived with NASA and available to the public at NASAPDS--http://ida.wr.usgs.gov/ [ http://ida.wr.usgs.gov/ ] . Although these pictures were generally a vast improvement in spatial resolution compared to the previous images from Viking and Mariner, the latest pictures from MOC--taken this month (April 1999) from the proper Mapping Orbit--demonstrate the power of the MOC when in focus and operating at the correct altitude (~380 km or 235 miles). The Viking Orbiter picture on the left, above, shows the 83 kilometers-(52 miles)-wide crater, Escalante. Located on the martian equator at 245°W longitude, a portion of this crater's floor was seen by MOC before the mapping mission began, at a resolution of 9.4 meters (31 feet) per pixel as shown in the middle image. The new picture--on the right--peers down into one of the pits seen in the earlier MOC image--only now it is viewed at 1.8 meters (6 feet) per pixel. The new high resolution image (right) covers an area only 1.5 kilometers (0.9 miles)wide and shows that the crater floor--which appears relatively smooth in the context view on the left--is actually quite rough at the scale that a human being would notice if trying to hike around in this landscape. The latest picture also shows small, bright windblown dunes that were not visible in the earlier MOC image. MOC2-120a is a mosaic of Viking Orbiter images 381s62 and 379s47, and MOC2-120b is a subframe of MGS MOC image SPO-2-382/04. The large white box shows the location of MOC2-120b, and the small white box shows the location of MOC2-120c. In MOC2-120a and MOC2-120b, illumination is from the right/upper right, in MOC2-120c it is from the left. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Once Pitted, Twice Spied: A
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PIA02007
Sol (our sun)
Mars Orbiter Camera
| Title |
Once Pitted, Twice Spied: A New High Resolution View Inside Escalante Crater |
| Original Caption Released with Image |
During the year spent waiting to achieve the planned circular, polar Mapping Orbit, the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) took about 1170pictures that had resolutions in the 2 to 20 meters (7-66 feet) per pixel range. These pictures were obtained between September 1997 and September 1998, and are now archived with NASA and available to the public at NASAPDS--http://ida.wr.usgs.gov/ [ http://ida.wr.usgs.gov/ ] . Although these pictures were generally a vast improvement in spatial resolution compared to the previous images from Viking and Mariner, the latest pictures from MOC--taken this month (April 1999) from the proper Mapping Orbit--demonstrate the power of the MOC when in focus and operating at the correct altitude (~380 km or 235 miles). The Viking Orbiter picture on the left, above, shows the 83 kilometers-(52 miles)-wide crater, Escalante. Located on the martian equator at 245°W longitude, a portion of this crater's floor was seen by MOC before the mapping mission began, at a resolution of 9.4 meters (31 feet) per pixel as shown in the middle image. The new picture--on the right--peers down into one of the pits seen in the earlier MOC image--only now it is viewed at 1.8 meters (6 feet) per pixel. The new high resolution image (right) covers an area only 1.5 kilometers (0.9 miles)wide and shows that the crater floor--which appears relatively smooth in the context view on the left--is actually quite rough at the scale that a human being would notice if trying to hike around in this landscape. The latest picture also shows small, bright windblown dunes that were not visible in the earlier MOC image. MOC2-120a is a mosaic of Viking Orbiter images 381s62 and 379s47, and MOC2-120b is a subframe of MGS MOC image SPO-2-382/04. The large white box shows the location of MOC2-120b, and the small white box shows the location of MOC2-120c. In MOC2-120a and MOC2-120b, illumination is from the right/upper right, in MOC2-120c it is from the left. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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The Geodesy Campaign
PIA02023
Sol (our sun)
Mars Orbiter Camera
| Title |
The Geodesy Campaign |
| Original Caption Released with Image |
Every day, Mars Global Surveyor (MGS) circles the red planet just over twelve times, and from their vantage point at 400 km altitude, the fisheye lenses of the Mars Orbiter Camera (MOC)Wide Angle (WA) cameras can see the entire surface. During typical operations, highly-summed two-color image strips are transmitted for each orbit and assembled into daily global weather maps, with a resolution of about 7.5 km (4.6 miles) per pixel. The small size and low resolution of these strips leaves most of the data bandwidth available for higher-priority Narrow Angle images. During May 1999, however, the Wide Angle cameras are being used instead to map the whole planet at the intrinsic resolution of the WA camera -- 230 meters (750 feet) per pixel. While the blue WA camera continues to capture the global map so that daily weather can still be monitored, the other WA camera (with the red filter) is building up swaths of full-resolution coverage. The Deep Space Network is tracking the spacecraft 24 hours a day during this geodesy campaign, and imaging data are being returned for about two-thirds of the time at 69 kbits/sec(somewhat faster than a 56K modem). During the other third of the time, the spacecraft is transmitting back to Earth one day's worth of recorded data from the other science instruments. Geodesy is the measurement of a planet's shape and the location of features on its surface. The intent of the geodesy campaign is to acquire, during a short period of time, simultaneous measurements by the Mars Orbiter Laser Altimeter (MOLA), the Radio Science (RS)investigation, and the MOC. MOLA observations provide precise, absolute measurements of a set of profiles around the planet, but their spacing is quite large relative to their resolution. RS measurements provide detailed information about the position of the spacecraft, critical to processing both the MOC and MOLA data. MOC provides both a higher resolution base map on which the other data can be overlain and, using stereoscopic measurements, provides the potential for a ten-fold improvement in the spatial resolution of the topography. Owing to the nature of the MGS orbit, the groundtrack returns to within about 30 km of a given orbit 88 orbits (about one week) later. Thus, it takes a week to build up global coverage at full resolution. Figure MOC2-127a [ http://photojournal.jpl.nasa.gov/catalog/PIA02022 ], shows the planning map of coverage during the first week of the campaign (top), and the resulting actual coverage (bottom). Gaps caused by recorder playbacks must be filled in a second week of imaging by moving the times of the playbacks. Also in the second week, stereo coverage is acquired by re-imaging areas from adjacent orbits at aside-looking angle. Figure MOC2-127b shows an example of such stereo from the Mare Tyrrhenum region, centered at 27.3°S, 227.0°W (NOTE: Red-blue glasses are needed to view the stereo effect). The crater that dominates the center of Figure MOC2-127b is about 50 kilometers (31 miles) across. Stereo coverage will be completed in the third and fourth weeks. The remaining data volume will be used to fill in gaps created by data losses, and to acquire a somewhat lower resolution global color image through the blue wide angle camera. The resulting dataset will provide global color and stereo coverage at about 300 m/pixel. Although similar coverage was obtained by the Viking mission in the late 1970s, Viking took over three years to cover the planet, and there are significant variations in lighting, weather, and surface features in the Viking images. A substantial improvement in the longitude/latitude grid is expected, which will have important benefits to future Mars exploration. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Lower Northeastern Flank of
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PIA02012
Sol (our sun)
Mars Orbiter Camera
| Title |
Lower Northeastern Flank of Tyrrhena Patera |
| Original Caption Released with Image |
Tyrrhenna Patera is thought to be an ancient volcano. It is located in Hesperia Planum in the martian southern hemisphere. The Mars Orbiter Camera recently acquired this view of escarpments and valleys on the lower northeast flank of the volcano. Small, bright dunes cover low areas such as valley and crater floors. The picture is illuminated from the lower right and covers an area 3 kilometers (1.9 miles) across. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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MOC "Looking Into" Martian C
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PIA02018
Sol (our sun)
Mars Orbiter Camera
| Title |
MOC "Looking Into" Martian Craters |
| Original Caption Released with Image |
During the first week of May 1999, the Mars Orbiter Camera (MOC) spent sometime peering into martian impact craters. This crater is located in south-central Syria Planum and is about 7.0 kilometers (4.4 miles) across. Illumination is from the upper left. If you have ever visited the famous Meteor Crater in northern Arizona, U.S.A., then you are aware of its immense size on a human scale. The Arizona crater, however, is only 1 kilometer across (0.62 miles), whereas this crater is seven times wider. This crater was formed by the impact and explosion of a meteorite at some time in the martian past. After the crater formed, it was modified by wind and erosion. The crater shows deposits of sand and dust on the floor and in low areas around their rim, also boulders and other debris that has slid down the inside walls of the crater, and some crater walls show exposures of bedrock. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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Apollinaris Patera, Mars
PIA02006
Sol (our sun)
Mars Orbiter Camera
| Title |
Apollinaris Patera, Mars |
| Original Caption Released with Image |
This month (April 1999), the Mars Global Surveyor Mars Orbiter Camera (MOC) passed over the Apollinaris Patera volcano and captured a patch of bright clouds hanging over its summit in the early martian afternoon. This ancient volcano is located near the equator and--based on observations from the 1970s Viking Orbiters--is thought to be as much as 5 kilometers (3 miles) high. The caldera--the semi-circular crater at the volcano summit--is about 80 kilometers (50 miles) across. The color in this picture was derived from the MOC red and blue wide angle camera systems and does not represent true color as it would appear to the human eye (that is, if a human were in a position to be orbiting around the red planet). Illumination is from the upper left. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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The Geodesy Campaign
PIA02022
Sol (our sun)
Mars Orbiter Camera
| Title |
The Geodesy Campaign |
| Original Caption Released with Image |
Figure MOC2-127b [ http://photojournal.jpl.nasa.gov/catalog/PIA02023 ] is about 50 kilometers (31 miles) across. Stereo coverage will be completed in the third and fourth weeks. The remaining data volume will be used to fill in gaps created by data losses, and to acquire a somewhat lower resolution global color image through the blue wide angle camera. The resulting dataset will provide global color and stereo coverage at about 300 m/pixel. Although similar coverage was obtained by the Viking mission in the late 1970s, Viking took over three years to cover the planet, and there are significant variations in lighting, weather, and surface features in the Viking images. A substantial improvement in the longitude/latitude grid is expected, which will have important benefits to future Mars exploration. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO., Every day, Mars Global Surveyor (MGS) circles the red planet just over twelve times, and from their vantage point at 400 km altitude, the fisheye lenses of the Mars Orbiter Camera (MOC)Wide Angle (WA) cameras can see the entire surface. During typical operations, highly-summed two-color image strips are transmitted for each orbit and assembled into daily global weather maps, with a resolution of about 7.5 km (4.6 miles) per pixel. The small size and low resolution of these strips leaves most of the data bandwidth available for higher-priority narrow Angle images. During May 1999, however, the Wide Angle cameras are being used instead to map the whole planet at the intrinsic resolution of the WA camera -- 230 meters (750 feet) per pixel. While the blue WA camera continues to capture the global map so that daily weather can still be monitored, the other WA camera (with the red filter) is building up swaths of full-resolution coverage. The Deep Space Network is tracking the spacecraft 24 hours a day during this geodesy campaign, and imaging data are being returned for about two-thirds of the time at 69 kbits/sec (somewhat faster than a 56K modem). During the other third of the time, the spacecraft is transmitting back to Earth one day's worth of recorded data from the other science instruments. Geodesy is the measurement of a planet's shape and the location of features on its surface. The intent of the geodesy campaign is to acquire, during a short period of time, simultaneous measurements by the Mars Orbiter Laser Altimeter (MOLA), the Radio Science (RS)investigation, and the MOC. MOLA observations provide precise, absolute measurements of a set of profiles around the planet, but their spacing is quite large relative to their resolution. RS measurements provide detailed information about the position of the spacecraft, critical to processing both the MOC and MOLA data. MOC provides both a higher resolution base map on which the other data can be overlain and, using stereoscopic measurements, provides the potential for a ten-fold improvement in the spatial resolution of the topography. Owing to the nature of the MGS orbit, the groundtrack returns to within about 30 km of a given orbit 88 orbits (about one week) later. Thus, it takes a week to build up global coverage at full resolution. Figure MOC2-127a shows the planning map of coverage during the first week of the campaign (top), and the resulting actual coverage (bottom). Gaps caused by recorder playbacks must be filled in a second week of imaging by moving the times of the playbacks. Also in the second week, stereo coverage is acquired by re-imaging areas from adjacent orbits at aside-looking angle. Figure MOC2-127b [ http://photojournal.jpl.nasa.gov/catalog/PIA02023 ] shows an example of such stereo from the Mare Tyrrhenum region, centered at 27.3°S, 227.0°W (NOTE: Red-blue glasses are needed to view the stereo effect). The crater that dominates the center of |
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MOC "Looking Into" Martian C
…
PIA02017
Sol (our sun)
Mars Orbiter Camera
| Title |
MOC "Looking Into" Martian Craters |
| Original Caption Released with Image |
During the first week of May 1999, the Mars Orbiter Camera (MOC) spent sometime peering into martian impact craters. This crater is located on a plain west of the Tartarus Montes (east of Elysium Mons volcano). The crater is about 2.7 kilometers (1.7 miles) across. Illumination is from the left. If you have ever visited the famous Meteor Crater in northern Arizona, U.S.A., then you are aware of its immense size on a human scale. The Arizona crater, however, is only 1 kilometer across (0.62 miles), whereas this crater is nearly three times that size. This crater was formed by the impact and explosion of a meteorite at some time in the martian past. After the crater formed, it was modified by wind and erosion. The crater shows deposits of sand and dust on the floor and in low areas around the rim, also boulders and other debris that has slid down the inside walls of the crater, and some crater walls show exposures of bedrock. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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MOC "Looking Into" Martian C
…
PIA02019
Sol (our sun)
Mars Orbiter Camera
| Title |
MOC "Looking Into" Martian Craters |
| Original Caption Released with Image |
During the first week of May 1999, the Mars Orbiter Camera (MOC) spent sometime peering into martian impact craters. This crater is found on Hesperia Planum and is 7.3 kilometers (4.5 miles) across. Illumination is from the upper left. If you have ever visited the famous Meteor Crater in northern Arizona, U.S.A., then you are aware of its immense size on a human scale. The Arizona crater, however, is only 1 kilometer across (0.62 miles), this crater is seven times wider. This crater was formed by the impact and explosion of a meteorite at some time in the martian past. After the crater formed, it was modified by wind and erosion. The crater shows deposits of sand and dust on the floor and in low areas around their rim, also boulders and other debris that has slid down the inside walls of the crater, and some crater walls show exposures of bedrock. Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO. |
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