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The depressions in this image captured by NASA's 2001 Mars Odyssey spacecraft are located in the material that fills Asimov Crater. | Context imageThe depressions in this VIS image are located in the material that fills Asimov Crater.Orbit Number: 50134 Latitude: -47.3006 Longitude: 5.85108 Instrument: VIS Captured: 2013-04-03 01:11Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image released on August 6, 2004 from NASA's 2001 Mars Odyssey shows a decorrelation stretch near Nili Fosse. Pink/magenta colors usually represent basaltic dunes, cyan indicates the presence of water ice clouds, while green can represent dust. | Released August 6, 2004This image shows two representations of the same infra-red image near Nili Fosse in the Isidis region of Mars. On the left is a grayscale image showing surface temperature, and on the right is a false-color composite made from 3 individual THEMIS bands. The false-color image is colorized using a technique called decorrelation stretch (DCS), which emphasizes the spectral differences between the bands to highlight compositional variations.In many cases craters trap sand in their topographic depressions, interrupting the sand's migration across the Martian surface. This image is particularly interesting because there appears to be more than 1 type of sand in the bottom of this crater and in the hummocky terrain near the bottom of the image. The pink/magenta areas are characteristic of a basaltic composition, but there are also orange areas that are likely caused by the presence of andesite. These two compositions, basalt and andesite, are some of the most common found on Mars.Image information: IR instrument. Latitude 24, Longitude 80.7 East (297.3 West). 100 meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Global Surveyor shows a full-circle view of a layered rock called 'Tetl' in the 'Columbia Hills'' on Mars. | This 360-degree view combines frames taken by the navigation camera on NASA's Mars Exploration Rover Spirit during the rover's 271st martian day, or sol, on Oct. 7, 2004. The rover had just driven into position for using the tools on its robotic arm (not in the picture) to examine a layered rock called "Tetl" in the "Columbia Hills." Spirit's total driving distance from its landing to this point was 3,641 meters (2.26 miles), more than six times the distance set as a criterion for mission success. The view presented here in a vertical projection with geometric seam correction. | |
The 'tail' behind the crater at the top of this image from NASA's 2001 Mars Odyssey spacecraft is called a windstreak. This feature is formed by winds blowing over/in and around the crater. | Context image The "tail" behind the crater at the top of this VIS image is called a windstreak. This feature is formed by winds blowing over/in and around the crater. Turbulence in the wind will erode or deposit fine materials, creating the windstreak. Windstreaks form on the down wind side of the crater, and indicate winds from the ESE. The small hills below the windstreak are small volcanic constructs. This image is located in the extensive lava plains called Daedalia Planum.Orbit Number: 65310 Latitude: -10.2729 Longitude: 226.476 Instrument: VIS Captured: 2016-09-03 11:24Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of the floor of Schiaparelli Crater. | Context image The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of the floor of Schiaparelli Crater.Orbit Number: 44366 Latitude: -1.13235 Longitude: 14.4773 Instrument: VIS Captured: 2011-12-15 07:21Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
The High-Resolution Imaging Science Experiment (Hi-RISE) camera aboard NASA's Mars Reconnaissance Orbiter captured this avalanche plunging down a 1,640-foot-tall (500-meter-tall) cliff on May 29, 2019. | The High-Resolution Imaging Science Experiment (Hi-RISE) camera aboard NASA's Mars Reconnaissance Orbiter captured this avalanche plunging down a 1,640-foot-tall (500-meter-tall) cliff on May 29, 2019. The image also reveals layers at Mars' north pole during spring. As temperatures increase and vaporize ice, the destabilized ice blocks break loose and kick up dust.NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate in Washington. Lockheed Martin Space in Denver is the prime contractor for the project and built the spacecraft. The University of Arizona, in Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., in Boulder, Colorado. | |
NASA's Mars Global Surveyor shows | MGS MOC Release No. MOC2-571, 11 December 2003This October 2003 Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows gullies cut into debris on the southeast-facing wall of an old meteor impact crater in southeastern Hellas Planitia. This view is located near 44.5°S, 277.0°W. The 200 meter scale bar is approximately 656 feet across; the picture is illuminated from the upper left. | |
This image shows the tracks and trench marks made by NASA's Mars Exploration Rover Opportunity at Meridiani Planum, Mars. The rover can be seen to the lower left of the lander. | This image shows the tracks and trench marks made by the Mars Exploration Rover Opportunity at Meridiani Planum, Mars. The rover can be seen to the lower left of the lander. The trench is visible to the upper left of the rover, which has traveled a total of 35.3 meters (116 feet) since leaving the lander on sol 7 (January 31, 2004). On sol 23 (February 16, 2004), the rover used one of its wheels to dig a trench measuring approximately 10 centimeters (4 inches) deep, 50 centimeters (20 inches) long, and 20 centimeters (8 inches) wide. This vertically projected image was created using a combination of images from the rover's navigation camera and hazard-avoidance cameras. | |
This is the 3-D version of NASA's Mars Exploration Rover Opportunity's view on its 56th sol on Mars, before it left 'Eagle Crater.' 3D glasses are necessary to view this image. | This is the 3-D version of the Mars Exploration Rover Opportunity's view on its 56th sol on Mars, before it left "Eagle Crater." To the right, the rover tracks are visible at the original spot where the rover attempted unsuccessfully to exit the crater. After a one-sol delay, Opportunity took another route to the plains of Meridiani Planum. This image was taken by the rover's navigation camera. | |
A color image fro NASA's Viking Orbiter of the Hellas Planitia region of Mars; north toward top. The scene shows the Hellas plain within the 1,800- km-diameter Hellas basin, an ancient impact basin. | A color image of the Hellas Planitia region of Mars; north toward top. The scene shows the Hellas plain within the 1,800- km-diameter Hellas basin, an ancient impact basin (and the largest basin on Mars) formed when a large projectile (asteroid, comet, meteor) hit the surface.This image is a composite of Viking medium-resolution images in black and white and low-resolution images in color. The image extends from latitude 60 degrees S. to 20 degrees S. and from longitude 250 degrees to 320 degrees. Mercator projection is used between latitudes 20 degrees S. and 30 degrees S.; Lambert projection is used below latitude 30 degrees S.The exact diameter of the ancient Hellas basin is difficult to determine because large portions of the rim are missing to the northeast and southwest. In addition several large patera or low volcanoes (Tyrrhena, Hadriaca, Amphitrites) occur along or near the rim and their flows have partially buried the older impact deposits. Outside the rim are several large, arcuate, inward-facing escarpments which could be remnants of multiple rings. The plains of Hellas are very complex; fluvial channels drain into the basin and the plains have been described as being a mixture of fluvial, lacustrine, glacial, eolian, and volcanic deposits. Frequent dust storms occur within the basin. | |
NASA's Mars Global Surveyor shows the north polar cap of Mars surrounded by fields of dark sand dunes. | 26 May 2004The north polar cap of Mars is surrounded by fields of dark sand dunes. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows several dunes in the north polar region. The winds responsible for them blow from the lower left toward the upper right. The picture is located near 78.6°N, 243.9°W. Sunlight illuminates the scene from the lower left, and the picture covers an area about 3 km (1.9 mi) across. | |
NASA's Ingenuity Mars Helicopter's fifth flight was captured on May 7, 2021, by one of the navigation cameras aboard the agency's Perseverance rover. This was the first time it flew to a new landing site. | NASA's Ingenuity Mars Helicopter's fifth flight was captured on May 7, 2021, by one of the navigation cameras aboard the agency's Perseverance rover. The helicopter ascended to a new height record of 33 feet (10 meters) flew 424 feet (129 meters) to a new landing site. This was the first time the helicopter made a one-way flight. It was airborne a total of 108 seconds.The Ingenuity Mars Helicopter was built by JPL, which also manages the technology demonstration project for NASA Headquarters. It is supported by NASA's Science, Aeronautics Research, and Space Technology mission directorates. NASA's Ames Research Center in California's Silicon Valley, and NASA's Langley Research Center in Hampton, Virginia, provided significant flight performance analysis and technical assistance during Ingenuity_x0092_s development. AeroVironment Inc., Qualcomm, and SolAero also provided design assistance and major vehicle components. Lockheed Martin Space designed and manufactured the Mars Helicopter Delivery System. | |
This image shows the tracks left by NASA's Curiosity rover on Aug. 22, 2012, as it completed its first test drive on Mars. This image was taken by a front Hazard-Avoidance camera, which has a fisheye lens. | This image shows the tracks left by NASA's Curiosity rover on Aug. 22, 2012, as it completed its first test drive on Mars. The rover went forward 15 feet (4.5 meters), rotated 120 degrees and then reversed 8.2 feet (2.5 meters). Curiosity is now 20 feet (6 meters) from its landing site, named Bradbury Landing.This image was taken by a front Hazard-Avoidance camera, which has a fisheye lens.
JPL manages the Mars Science Laboratory/Curiosity for NASA's Science Mission Directorate in Washington. The rover was designed, developed and assembled at JPL, a division of the California Institute of Technology
in Pasadena.
For more about NASA's Curiosity mission, visit: http://www.jpl.nasa.gov/msl, http://www.nasa.gov/mars, and
http://marsprogram.jpl.nasa.gov/msl. | |
NASA's Mars Global Surveyor shows streamlined landforms carved by catastrophic floods in the Athabasca Valles system of the Cerberus region of Mars. | 11 May 2005This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows streamlined landforms carved by catastrophic floods in the Athabasca Valles system of the Cerberus region of Mars. Location near: 7.9°N, 205.7°W Image width: ~3 km (~1.9 mi) Illumination from: lower left Season: Northern Autumn | |
This image from NASA's Mars Reconnaissance Orbiter shows a number of unusual, quasi-circular structures that apparently formed within bright flows in Meridiani Planum. | This image shows a number of unusual, quasi-circular structures from 300 to 600 meters in diameter that apparently formed within bright flows in Meridiani Planum. The strange structures were observed earlier in MOC image E12-01295. They are located near the equator, about 300 kilometers West of the MER rover Opportunity.New details can be seen in the HiRISE image that yield clues to the origin of these mysterious features. The dark rings seen within the concentric structures appear rougher than their surroundings. The bright material in which they formed is densely fractured, suggesting that it is quite brittle. Several small impact craters found within the bright unit produced sprays of dark ejecta, suggesting that the bright surface layer may be only a few meters thick. A compositional and morphological boundary separates the contorted central region of the unit from the smooth margins.A full interpretation awaits detailed analysis, but these observations suggest that the lobate bright unit may have been produced by an ancient flow of water-saturated fluvial sediments. The circular structures within the flow could have formed by desiccation, as the sediments dried out and contracted, similar to mud cracks but on a much larger scale. Or they may have formed by a process of diapirism, if a solid crust formed on the surface of the drying sediments that was denser than the water-saturated slurry below. On Earth, slurries of sand and water that are pressurized by the weight of the overburden can rise to the surface to form "injectites," eruptions of sand and water that can reach heights of hundreds of meters. Whether they were formed by desiccation or injection, these unusual features record a unique moment in the distant past of Mars.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, 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 & Technologies Corp., Boulder, Colo.Originally released October 27, 2010 | |
Mars digital-image mosaic merged with color of the MC-21 quadrangle, Iapygia region of Mars. This image is from NASA's Viking Orbiter 1. | Mars digital-image mosaic merged with color of the MC-21 quadrangle, Iapygia region of Mars. Heavily cratered and in places dissected highlands dominate the Iapygia quadrangle. The west-central part is marked by a large impact crater, Huygens. Huygens is an ancient remnant of the many large impact events that occurred during the period of heavy bombardment. The southern one-third is characterized by mountainous and knobby terrain of the northern rim of the enormous Hellas impact basin. Latitude range -30 to 0 degrees, longitude range -90 to -45 degrees. | |
This image acquired on October 5, 2018 by NASA's Mars Reconnaissance Orbiter, shows a new impact crater that formed between July and September 2018. | Map Projected Browse ImageClick on image for larger versionThis image shows a new impact crater that formed between July and September 2018. It's notable because it occurred in the seasonal southern ice cap, and has apparently punched through it, creating a two-toned blast pattern. The impact hit on the ice layer, and the tones of the blast pattern tell us the sequence. When an impactor hits the ground, there is a tremendous amount of force like an explosion. The larger, lighter-colored blast pattern could be the result of scouring by winds from the impact shockwave. The darker-colored inner blast pattern is because the impactor penetrated the thin ice layer, excavated the dark sand underneath, and threw it out in all directions on top of the layer.The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 24.8 centimeters (9.8 inches) per pixel (with 1 x 1 binning); objects on the order of 74 centimeters (29.1 inches) across are resolved.] North is up.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
This image from NASA's Mars Odyssey spacecraft shows part of Zephyria Planum. | Context image for PIA09443Changing WindsThis infrared image shows part of Zephyria Planum. This region is well named, Zephyria is one of the winged mares of Selene (the moon goddess of Greek mythology), and this region has been subject to intense wind activity. Each level of surface in this image records a different wind direction. Note the small double-circle opening in the thumbnail which reveals a surface etched in a NW/SE direction beneath one etched by the wind in a NNW/SSE direction.Image information: IR instrument. Latitude -0.1N, Longitude 151.6E. 98 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
Taken by NASA's 2001 Mars Odyssey spacecraft, this image of the northeastern flank of Ascraeus Mons shows several volcanic channels. | Context imageThis VIS image of the northeastern flank of Ascraeus Mons shows several volcanic channels.Orbit Number: 42609 Latitude: 11.9702 Longitude: 258.164 Instrument: VIS Captured: 2011-07-23 18:21Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Global Surveyor shows a dust devil making a streak in Mars' Promethei Terra. Dust devils are spinning, columnar vortices of wind that move across the landscape, pick up dust, and look somewhat like miniature tornadoes. | In December 1999, the MOC team finally had an answer! A dust devil, shown in the above left figure, was caught in the act of creating a swirly, dark streak! An eerie sensation washed over the first team members who saw this picture -- here was an event on Mars "caught in the act" just hours before the picture was played back to Earth. A "smoking gun."The first dust devil seen making a streak -- located in Promethei Terra (above, left) -- was traveling from right (east) to left (west). A columnar shadow was cast by sunlight coming from the upper left. This shadow indicates the true shape of the dust devil. The bright dust devil itself does not look like a column because the picture was taken from a camera looking straight down on it. The dust devil is less than 100 meters (less than 100 yards) wide and the picture covers an area approximately 1.5 by 1.7 kilometers (about 1 by 1 mile).Dust devils are spinning, columnar vortices of wind that move across the landscape, pick up dust, and look somewhat like miniature tornadoes. Dust devils are a common occurrence in dry and desert landscapes on Earth as well as Mars. They form when the ground heats up during the day, warming the air immediately above the surface. As the warmed air nearest the surface begins to rise, it spins. The spinning column begins to move across the surface and picks up loose dust (if any is present). The dust makes the vortex visible and gives it the "dust devil" or tornado-like appearance. On Earth, dust devils typically last for only a few minutes.The fourth picture (above, right) shows a surface in southwestern Terra Sirenum near 63°S, 168°W, that has seen the activity of so many dust devils that it looks like a plate of dark gray spaghetti. This image, taken in early summer during February 2000, covers an area 3 km wide and 30 km long (1.9 by 19 miles). In fact, a dust devil can be seen in the upper right of this image. Like the other pictures shown here, the Terra Sirenum image is illuminated by sunlight from the upper left. | |
Water-Signature Mineral Found by Spirit | This spectrum, taken by the Mars Exploration Rover Spirit's Moessbauer spectrometer, shows the presence of an iron-bearing mineral called goethite in a rock called "Clovis" in the "Columbia Hills" of Mars. Goethite contains water in the form of hydroxyl as a part of its structure. By identifying this mineral, the examination of Clovis produced strong evidence for past water activity in the area that Spirit is exploring. | |
Numerous channels dissect the rim of Lohse Crater, as shown in this image captured by NASA's 2001 Mars Odyssey spacecraft. | Context imageNumerous channels dissect the rim of Lohse Crater.Orbit Number: 56734 Latitude: -44.1847 Longitude: 342.358 Instrument: VIS Captured: 2014-09-28 05:15Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image taken by the navigation camera on NASA's Mars Exploration Rover Opportunity shows the layers of bedrock that line the walls of 'Endurance Crater' on Mars. | Figure 1
Chlorine Goes Deep
This image taken by the navigation camera on the Mars Exploration Rover
Opportunity shows the layers of bedrock that line the walls of "Endurance Crater."
Opportunity has been inching down the crater walls, investigating distinct layers of
rock for clues to Mars' buried past. The various layers are labeled here as "A"
through "F." Targets within these layers, including millstone, are also indicated.
Using its alpha particle X-ray spectrometer, Opportunity has discovered that the
element chlorine increases in concentration dramatically with deepening layers.
Opportunity will continue to roll deeper into Endurance to see if this puzzling trend
continues. Scientists hope the new data will help them figure out how the presence
of chlorine fits into the history of water at Endurance Crater. This image was taken
on sol 134 (June 9, 2004). | |
This view from Spirit's panoramic camera is assembled from frames acquired on Nov. 23 and 24, 2005 from the rover's position near an outcrop called 'Seminole.' The marscape shows an abundance of rocks upon red soil. | This view from Spirit's panoramic camera is assembled from frames acquired on Martian days, or sols, 672 and 673 (Nov. 23 and 24, 2005) from the rover's position near an outcrop called "Seminole." The view is a southward-looking portion of a larger panorama still being completed. This is a false-color version to emphasize geological differences. It is a composite of images shot through three different filters, admitting light of wavelengths 750 nanometers, 530 nanometers and 430 nanometers. | |
This image from NASA's Mars Odyssey shows a small section of Shalbatana Vallis. | Context imageToday's VIS image shows a small section of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is an outflow channel carved by massive floods of escaping groundwater whose source lies far to the south of this image. This channel, and all others in this region, drain into Chryse Planitia.Orbit Number: 80550 Latitude: 5.84335 Longitude: 316.746 Instrument: VIS Captured: 2020-02-10 19:21Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
Many gullies dissect the inner rim of this unnamed crater in Noachis Terra, as shown in this image captured by NASA's 2001 Mars Odyssey spacecraft. | Context image Many gullies dissect the inner rim of this unnamed crater in Noachis Terra.Orbit Number: 67270 Latitude: -40.2335 Longitude: 357.921 Instrument: VIS Captured: 2017-02-11 22:06Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
Silica-Rich Soil in Gusev Crater | NASA's Mars Exploration Rover Spirit has found a patch of bright-toned soil so rich in silica that scientists propose water must have been involved in concentrating it. The silica-rich patch, informally named "Gertrude Weise" after a player in the All-American Girls Professional Baseball League, was exposed when Spirit drove over it during the 1,150th Martian day, or sol, of Spirit's Mars surface mission (March 29, 2007). One of Spirit's six wheels no longer rotates, so it leaves a deep track as it drags through soil. Most patches of disturbed, bright soil that Spirit had investigated previously are rich in sulfur, but this one has very little sulfur and is about 90 percent silica.Spirit's panoramic camera imaged the bright patch through various filters on Sol 1,158 (April 6). This approximately true-color image combines images taken through three different filters. The track of disturbed soil is roughly 20 centimeters (8 inches) wide. Spirit's miniature thermal emission spectrometer, which can assess a target's mineral composition from a distance, examined the Gertrude Weise patch on Sol 1,172 (April 20). The indications it found for silica in the overturned soil prompted a decision to drive Spirit close enough to touch the soil with the alpha particle X-ray spectrometer, a chemical analyzer at the end of Spirit's robotic arm. The alpha particle X-ray spectrometer collected data about this target on sols 1,189 and 1,190 (May 8 and May 9) and produced the finding of approximately 90 percent silica.Silica is silicon dioxide. On Earth, it commonly occurs as the crystalline mineral quartz and is the main ingredient in window glass. The Martian silica at Gertrude Weise is non-crystalline, with no detectable quartz.In most cases, water is required to produce such a concentrated deposit of silica, according to members of the rover science team. One possible origin for the silica could have been interaction of soil with acidic steam produced by volcanic activity. Another could have been from water in a hot spring environment. | |
The movement pathways of molten rock, or lava, is demonstrated in this image from NASA's Mars Odyssey spacecraft of a portion of Olympus Mons, the largest volcano in our solar system. | (Released 4 June 2002)The ScienceThe movement pathways of molten rock, or lava, is demonstrated in this image of a portion of Olympus Mons, the largest volcano in our solar system. These now-solid lava flows all show nearly the same orientation, having flowed from northeast to southwest, down the slope of the volcano's southeastern flank. Throughout the image, narrow pairs of lineaments can be observed ? these are called levees, and are essentially channel walls formed by the solidification and buildup of the edges of the lava flows. We can determine that the high-standing mountains must be older than the flows because they blocked their passage, causing the flows to change direction and go around the taller mountains. As in other THEMIS images, the lack of bright-dark contrast in this image indicates that a layer of dust covers these surfaces. The surfaces of the lava flows are virtually uncratered, attesting to the relatively recent formation of the flows, where ?recent? is within the last 500 million years or so. Several meteorites found on Earth appear to have come from volcanic regions on Mars ? their ages are as young as 180 million years, leading many scientists to suggest that volcanoes of the Tharsis region, including Olympus Mons, may be the source regions of these meteorites. A prominent pear-shaped bowl is apparent on a hill in the lower right third of the image ? the collapse and mass movement of material down slope, which also formed a debris pile below and southeast of the bowl, likely formed this feature.The StoryMillions and millions of years ago, a huge impact blasted a crater into the surface of Mars, sending particles of the Martian surface scattering into space at great speeds, where they spent millions and millions of years calmly in space before encountering a nearby orbiting planet: our own planet Earth. Hurtling down through Earth's atmosphere, these pieces of Mars landed in various regions of our world and were discovered by modern-day meteorite hunters. When scientists analyzed the ages and chemical composition of several meteorites, they were able to determine that these ancient space rocks came from Mars, were volcanic in origin, and were around 180 million years old.So, where on Mars did they come from? Geologists had to turn the Martian globe, looking for volcanic areas that were relatively recent in their formation. Believe it or not, "recent" in geological terms can actually mean "180 million years young." So, where did their fingers point? To the Tharsis region, home to Olympus Mons, the largest volcano in our solar system.The above THEMIS image hints at the young age of the lava flows around Olympus Mons. Since the surfaces of the lava flows are virtually uncratered, that means these lava flows were "relatively recent," forming within the last 500 million years or so. While no one knows for sure if the Mars meteorites came from this area, this lava-rich region seems likely as a possibility.Always in search of relative ages of geological happenings on the red planet, geologists can also tell that the high-standing mountains in the area are older than the lava flows. You can follow the evidence too. Take a look at the mountains and the lava flows near them. The narrow, flowing lava lines throughout the image are called levees, and outline the supple contours of the channel walls that formed as the lava flows became solid and built up at the edges. Now solid, cool, and still, these lava flows once moved dramatically down the slope of the volcano's southeastern flank. It couldn't have been an entirely free flow: the mountains must have stood in their way, because it's clear that the layered flows of molten rock had to change direction and move around them.That's not the only dramatic movement that took place here. Look also for the pear-shaped bowl on a hill in the lower right third of the image. It was formed when a huge mass of material collapsed and moved downslope, forming a debris pile below and southeast of the bowl.Not everything that's happened in this region is ferocious, however. Because this image does not have severe black-and-white contrasts of landforms on the Martian surface, it's likely that a layer of dust has blanketed the region over time, giving it a calm uniform look that belies its angrier past. | |
This pair of images color images from NASA's Mars Global Surveyor shows early autumn clouds over the Arsia Mons volcano, plus the shadow of the innermost of the two martain moons, Phobos. | Annotated View of Arsia and Phobos6 February 2006This pair of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) color images shows early autumn clouds over the Arsia Mons volcano, plus the shadow of the innermost of the two martain moons, Phobos. The picture on the left is taken from the MOC daily global map acquired at 7.5 km (~4.7 mi) per pixel on 28 January 2006, about a week after the start of southern autumn. The picture on the right was taken at the same time, but at a higher resolution of 489 m (1604 ft) per pixel. Both pictures are composites of MOC red and blue wide angle images, and both are oriented such that north is up and east is to the right. Arsia Mons and the other large Tharsis volcanoes commonly develop afternoon orographic (i.e., topographically-controlled) water ice clouds at this time of year. The equatorial Tharsis volcano, Pavonis Mons, is also under a deck of water ice clouds; it is located toward the upper right corner of the left, lower-resolution image. Sunlight glints off the dusty surface and the clouds and aerosols in the atmosphere, producing the bright diagonal streak located just southeast (lower right) of Arsia Mons. A water ice haze is seen on the left side of the lower-resolution image. The dark oval to the northeast of Arsia Mons, as noted above, is the shadow of Phobos.Location near: 9°S, 121°W Image width: 100 km scale bar = ~62 mi; 300 km bar = ~186 mi Illumination from: upper left Season: Southern Autumn | |
This cylindrical mosaic taken by NASA's Mars Exploration Rover Spirit shows the view south of the large crater dubbed 'Bonneville.' The rock dubbed 'Mazatzal' and the hole the rover drilled in to it can be seen at the lower left. | This cylindrical mosaic taken by the navigation camera on the Mars Exploration Rover Spirit on sol 82 shows the view south of the large crater dubbed "Bonneville." The rover will travel toward the Columbia Hills, seen here at the upper left. The rock dubbed "Mazatzal" and the hole the rover drilled in to it can be seen at the lower left. The rover's position is referred to as "Site 22, Position 32." This image was geometrically corrected to make the horizon appear flat. | |
NASA's Mars Global Surveyor shows dark-gray or blue-black sand shaded with light-toned frosted dunes in Kaiser Crater on Mars. | As the Mars Global Surveyor Primary Mission draws to an end, the southern hemisphere of Mars is in the depths of winter. At high latitudes, it is dark most, if not all, of the day. Even at middle latitudes, the sun shines only thinly through a veil of water and carbon dioxide ice clouds, and the ground is so cold that carbon dioxide frosts have formed. Kaiser Crater (47°S, 340°W) is one such place. At a latitude comparable to Seattle, Washington, Duluth, Minnesota, or Helena, Montana, Kaiser Crater is studied primarily because of the sand dune field found within the confines of its walls (lower center of the Mars Orbiter Camera image, above). The normally dark-gray or blue-black sand can be seen in this image to be shaded with light-toned frost. Other parts of the crater are also frosted. Kaiser Crater and its dunes were the subject of an earlier presentation of results. Close-up pictures of these and other dunes in the region show details of their snow-cover, including small avalanches. The two Mars Global Surveyor Mars Orbiter Camera images that comprise this color view (M23-01751 and M23-01752) were acquired on January 26, 2001. | |
NASA's Mars Global Surveyor shows mesas and pits formed by sublimation of carbon dioxide of the martian south polar cap. | 17 March 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows mesas and pits formed by sublimation of carbon dioxide of the south polar cap.Location near: 85.8°S, 351.5°W Image width: ~2 km (~1.2 mi) Illumination from: upper left Season: Southern Summer | |
The crater shown in this image from NASA's Mars Reconnaissance Orbiter has very few craters superposed on it, which attests to its youth. It also has very steep slopes and a sharp rim; more evidence of its young age. | This observation shows a fresh, approximately 7.5 kilometer diameter crater that resides in a larger crater in the Southern hemisphere.The crater shown here has very few craters superposed on it, which attests to its youth. It also has very steep slopes and a sharp rim; more evidence of its young age. Young, fresh craters are of interest on Mars because they help place constraints on the rate at which new impact craters and other young features have formed in recent times.This fresh crater is particularly interesting because it contains gullies. Gullies are slope features that are proposed to require some amount of liquid water to form. The gullies must have formed after the crater did, which means that if liquid water was involved in the formation of these gullies, then it existed on the surface of Mars more recently. The existence of recent liquid water is especially important in terms of the search for life on Mars and its future exploration.Several of the gullies show features such as terraces, discontinuous channels, and abandoned channels (see subimage); all of which imply that more than one flow event occurred. It is unknown whether or not such multiple flows would have been closely spaced in time.Terraces are thought to indicate past flow levels. Discontinuous channels may represent some subsurface flow in addition to surface flow, or they may be channels that were once continuous that have since been filled in with wind-blown sediment and dust. The latter is the most likely in the subimage. For example, see the discontinuous channel near the center; it appears to have sediment infilling it. Abandoned channels are paths that fluid flowed through in the past before another flow took a different direction.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, 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 & Technologies Corp., Boulder, Colo.Originally released June 20, 2007 | |
NASA's Mars Global Surveyor shows kidney bean-shaped pits, and other pits, formed by erosion in a landscape of frozen carbon dioxide in the martian south polar residual cap. | 17 August 2005This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows kidney bean-shaped pits, and other pits, formed by erosion in a landscape of frozen carbon dioxide. This images shows one of about a dozen different patterns that are common in various locations across the martian south polar residual cap, an area that has been receiving intense scrutiny by the MGS MOC this year, because it is visible on every orbit and in daylight for most of 2005.Location near: 86.9°S, 6.9°W Image width: width: ~3 km (~1.9 mi) Illumination from: upper left Season: Southern Spring | |
The Cerberus feature, imaged here by NASA's Mars Odyssey, is a dark region at the southeastern edge of the huge Elysium Mons volcanic complex that was visible to early astronomers because it was a distinctive dark spot on a large bright region of Mars. | (Released 24 April 2002)The ScienceThe Cerberus feature is a relatively dark region at the southeastern edge of the huge Elysium Mons volcanic complex. It was visible to early astronomers of Mars because it was a distinctive dark spot on a large bright region of the planet. Today we recognize that the Cerberus region encompasses a range of geologic terrains from relatively young and smooth lava flows to the very rugged, ancient eroded landscape seen in this THEMIS image. The Cerberus feature has also proven to be ephemeral. Compared to just 20 years ago when the Viking orbiter instruments viewed the planet, the Cerberus feature has shrunk down from its original length of roughly 1000 kilometers to just a few isolated dark splotches of just a few 100 kilometers. This is testament to the active eolian environment on Mars where global dust storms can lift and then later deposit significant amounts of dust, brightening formerly dark surfaces. The THEMIS image occurs in a portion of Cerberus that remains relatively dark and dust-free although in the bottommost portion of the image are faint, criss-crossing lines that likely are dust devil tracks. The abundant dune-like features covering many of the low, smooth surfaces are similar to those found in many places across the planet. They are evidence of the interaction of wind and movable particles at the surface but not necessarily in today's environment. In many other places on Mars they are clearly inactive; relicts of a different climate.The StoryHellhound of Greek mythology, Cerberus was the three-headed, dragon-tailed dog that stood guard at the opening to the underworld. This rough-and-tumble Mars terrain looks just as fierce and foreboding. At the edge of the huge Elysium Mons volcano complex, the Cerberus area appeared as a dark spot to early Mars astronomers in an otherwise bright region of the planet. If this dark area seems somewhat hellish to your imagination too, you'll be glad to know that the Martian wind has been brightening up the area.Just twenty years ago, the Viking orbiters reached Mars for the first long-term studies of Mars up close. The Cerberus feature was then almost 600 miles long, but has now been vanquished down to few small splotches about 60 miles long. Call that a triumph of lightness upon the surface, but don't think that the force bringing back the light is gentle and kind. The Martian wind can kick up a fierce global dust storm that lifts up the bright Martian dust into the air and then blankets the surface with the brighter material as it settles down again.The ancient, eroded terrain in this image is still rather dark and dust free, so you might say it's one area where a mythical Cerberus still guards its shrinking territory. The wind teases it, however, by kicking up small, whirling dust devils that leave long, dark, scratchy tracks upon the land. Fields of dunes wrinkle the surface in places as well, but they may be permanently cemented upon the surface now, no longer able to blow and drift as they did in their younger days. | |
Engineers for NASA's Mars Exploration Rover Mission are completing assembly and testing for the twin robotic geologists at JPL. | February 10, 2003Engineers for NASA's Mars Exploration Rover Mission are completing assembly and testing for the twin robotic geologists at JPL. This week the twin rovers are sharing floor space in JPL's Spacecraft Assembly Facility for the last time before they are shipped to the Kennedy Space Center in Florida.In the image above, engineers are installing the rover's solar panels. The rovers will be launched separately in May and June. | |
This graph based on data from the RAD instrument onboard NASA's Mars Science Laboratory spacecraft shows the flux of energetic particles (vertical axis) as a function of the estimated energy deposited in water (horizontal axis). | The relationship between charged-particle radiation dose measured with silicon sensors and the dose that biological tissue would receive in the same setting is assessed as a function of how much energy the charged particles would deposit in water (which serves as a proxy for biological tissue). This graph shows the flux of energetic particles (vertical axis) as a function of the estimated energy deposited in water (horizontal axis). The term "dose equivalent," which is used to discuss health risk from radiation exposure, takes this relationship into account. A quality factor, Q, is used to convert measured dose to dose equivalent. The green line on this graph indicates the biological weighting function of how Q is related to how charged-particle radiation deposits energy in water.These factors have been used in the process of interpreting the ramifications for future human interplanetary missions from the measurements made by the Radiation Assessment Detector inside NASA's Mars Science Laboratory spacecraft during the spacecraft's travel from Earth to Mars in 2011 and 2012.Southwest Research Institute, in San Antonio, Texas, and Boulder, Colo., supplied and operates the RAD instrument in collaboration with Germany's national aerospace research center, Deutsches Zentrum für Luft- und Raumfahrt. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Science Laboratory Project and the mission's Curiosity rover for NASA's Science Mission Directorate in Washington. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the rover.For more information about Curiosity and its mission, visit: http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl. | |
The extensive volcanic flows in this image captured by NASA's 2001 Mars Odyssey spacecraft are part of Daedalia Planum. | Context imageThe extensive volcanic flows in this VIS image are part of Daedalia Planum.Orbit Number: 50613 Latitude: -21.1694 Longitude: 240.671 Instrument: VIS Captured: 2013-05-12 11:00Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image shows the rocky road NASA's Mars Exploration Rover Spirit traveled to reach its ultimate destination the Columbia Hills. | Figure 1 (labels)This image shows the rocky road the Mars Exploration Rover Spirit will travel to reach its ultimate destination - the Columbia Hills. The hills, seen here in the background, are located 2.3 kilometers (1.4 miles) away in the southeast direction. Rover planners estimate the journey will take about two months, or 60 sols, including stops at interesting targets along the way. As of sol 81 (March 26, 2004), Spirit has traveled 492 meters (1614 feet). | |
The many small channels dissecting the top part of this image are drainage valleys on Mars. Most are draining downhill to the top of the image as seen by NASA's 2001 Mars Odyssey. | Context image for PIA02916Surface DrainageThe many small channels dissecting the top part of this image are drainage valleys. Most are draining downhill to the top [north] of the image.Image information: VIS instrument. Latitude -1.6N, Longitude 301.1E. 18 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows the northern part of Terby Crater. | Context imageThe THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows the northern part of Terby Crater. This image shows the layered deposits that fill the crater.Orbit Number: 42741 Latitude: -27.348 Longitude: 74.2507 Instrument: VIS Captured: 2011-08-03 13:23Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Curiosity looks back down at Marker Band Valley, where the rover's tracks are visible in the distance, after climbing a steep slope. This mosaic was captured by the rover's Mastcam on June 21, 2023. | Figure ANASA's Curiosity Mars rover looks back down at "Marker Band Valley" after climbing a steep slope. This mosaic, made of five images that were stitched together after being sent to Earth, was captured by the rover's Mastcam on June 21, 2023, the 3,865th Martian day, or sol, of the mission. The color has been adjusted to match lighting conditions as the human eye would see them on Earth.Figure A is the same image annotated to point out rover tracks in the gray terrain of the Marker Band.Curiosity struggled to climb a 23-degree slope that had slippery sand and wheel-size boulders. These three factors – the incline, the sand, and the large boulders – combined to make this Curiosity's toughest climb yet.Curiosity was built by NASA's Jet Propulsion Laboratory, which is managed by Caltech in Pasadena, California. JPL leads the mission on behalf of NASA's Science Mission Directorate in Washington. Malin Space Science Systems in San Diego built and operates Mastcam.For more about Curiosity, visit: http://mars.nasa.gov/msl or https://www.nasa.gov/mission_pages/msl/index.html. | |
These lava flows are part of the Arsia Mons complex on Mars as seen by NASA's 2001 Mars Odyssey spacecraft. | Context image for PIA02299Lava FlowsThese lava flows are part of the Arsia Mons complex.Image information: VIS instrument. Latitude -18.2N, Longitude 235.6E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Global Surveyor shows the cratered uplands located between the Amenthes Fossae and Hesperia Planum with windblown dunes and ripples. | This is a Mars Orbiter Camera view of the cratered uplands located between the Amenthes Fossae and Hesperia Planum. This ancient, cratered surface sports a covering of windblown dunes and ripples oriented in somewhat different directions. The dunes are bigger and their crests generally run east-west across the image. The ripples are smaller and their crests run in a more north-south direction. The pattern they create together makes some of the dunes almost appear as if they are giant millipedes!This picture covers an area only 3 kilometers (1.9 miles) wide. Illumination is from the top.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. | |
Interpreting Radar View near Mars' North Pole, Orbit 1512 | A radargram from the Shallow Subsurface Radar instrument (SHARAD) on NASA's Mars Reconnaissance Orbiter is shown in the upper-right panel and reveals detailed structure in the polar layered deposits of the north pole of Mars (with blowups shown in the upper-left panels). The sounding radar collected the data presented here during orbit 1512 of the mission, on Nov. 22, 2006. The horizontal scale in the radargram is distance along the ground track. It can be referenced to the ground track map shown in the lower right. The radar traversed from about 83.5 degrees to 80.5 degrees north latitude, or about 180 kilometers (110 miles). The ground track map shows elevation measured by the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor orbiter. Green indicates low elevation; reddish-white indicates higher elevation. The traverse is from the high elevation of the plateau formed by the layers to the lowlands below.The vertical scale on the radargram is time delay of the radar signals reflected back to Mars Reconnaissance Orbiter from the surface and subsurface. For reference, using an assumed velocity of the radar waves in the subsurface, time is converted to depth below the surface in two places: about 600 meters (2,000 feet) to the lowest of an upper series of bright reflectors and about 2,000 meters (6,500 feet) to the base of the polar layered deposits. The color scale of the radargram varies from black for weak reflections to bright yellow for strong reflections. The lower-left panel is a image from the Mars Orbiter Camera on Mars Global Surveyor showing exposed polar layering in the walls of a canyon near the north pole. The layering is divided into a finely structured upper unit (labeled "Upper PLD") and less-well-defined stratigraphy in the lower unit (labeled "Lower PLD"). The radargram clearly reveals the complexity of the layering in the upper unit, additional reflections from the lower unit, and the base of the entire stack of layered deposits. The layering manifests the recent climate history of Mars, recorded by the deposition and removal of ice and dust.The Shallow Subsurface Radar was provided by the Italian Space Agency (ASI). Its operations are led by the University of Rome and its data are analyzed by a joint U.S.-Italian science team. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Reconnaissance Orbiter for the NASA Science Mission Directorate, Washington. | |
This image from NASA's Mars Odyssey spacecraft shows the southern rim of Melas Chasma. A fault is seen as a small ridge feature entering the upper lobe of the gully. | Context image for PIA10030Follow The FaultThis image of the southern rim of Melas Chasma is unique in showing the trace of one of the many faults associated with Valles Marineris. The fault is seen as a small ridge feature entering the upper lobe of the gully. It continues as the brighter line crossing diagonally across the gully and then as a darker line down along the slope to the floor of Melas Chasma.Image information: VIS instrument. Latitude -10.3N, Longitude 283.7E. 35 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey spacecraft shows Aeolis Planum and the long term effect of wind on soft/poorly cemented material. Stretching from just south of Olympus Mons to Aeolis Planum is a region called the Medusa Fossae Formation. | Context image for PIA09440Wind EtchingThis image of Aeolis Planum shows the long term effect of wind on soft/poorly cemented material. Stretching from just south of Olympus Mons to Aeolis Planum is a region called the Medusa Fossae Formation. MFF is materials that are completely sculpted by the wind.Image information: VIS instrument. Latitude 0.7N, Longitude 144.8E. 18 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Exploration Rover Spirit panoramic camera shows the view acquired on the martian afternoon Apr. 3, 2004 in the direction of the rover's future drive destination. In the distance are the eastern-lying 'Columbia Hills.' | This mosaic image from the Mars Exploration Rover Spirit panoramic camera shows the view acquired after the rover drove 50.2 meters (165 feet) on the martian afternoon of sol 89 (April 3, 2004). The view shows the direction of the rover's future drive destination. In the distance are the eastern-lying "Columbia Hills." This image was assembled from images in the panoramic camera's green (530 nanometer) filter.Anatolia was named after the Anatolian fault system in Turkey. | |
The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the floor of Galle Crater. | Context imageThe THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of the floor of Galle Crater. Dark dunes are visible in the center of the image. The dark blue color typically indicates basaltic sand.Orbit Number: 58800 Latitude: -51.5789 Longitude: 328.788 Instrument: VIS Captured: 2015-03-17 07:20Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
The dust devil tracks seen in this image from NASA's 2001 Mars Odyssey spacecraft are located in Argyre Planitia. | Context imageThe dust devil tracks in today's VIS image are located in Argyre Planitia.Orbit Number: 42349 Latitude: -10.9922 Longitude: 223.593 Instrument: VIS Captured: 2011-07-02 06:46Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This set of images compares the 'Link' outcrop of rocks on Mars (left) with similar rocks seen on Earth (right). The 'Link' outcrop shows rounded gravel fragments, or clasts, up to a couple inches (few centimeters), within the rock outcrop. | Figure 1Click on the image for larger versionThis set of images compares the Link outcrop of rocks on Mars (left) with similar rocks seen on Earth (right). The image of Link, obtained by NASA's Curiosity rover, shows rounded gravel fragments, or clasts, up to a couple inches (few centimeters), within the rock outcrop. Erosion of the outcrop results in gravel clasts that fall onto the ground, creating the gravel pile at left. The outcrop characteristics are consistent with a sedimentary conglomerate, or a rock that was formed by the deposition of water and is composed of many smaller rounded rocks cemented together. A typical Earth example of sedimentary conglomerate formed of gravel fragments in a stream is shown on the right.An annotated version of the image highlights a piece of gravel that is about 0.4 inches (1 centimeter) across. It was selected as an example of coarse size and rounded shape. Rounded grains (of any size) occur by abrasion in sediment transport, by wind or water, when the grains bounce against each other. Gravel fragments are too large to be transported by wind. At this size, scientists know the rounding occurred in water transport in a stream.The name Link is derived from a significant rock formation in the Northwest Territories of Canada, where there is also a lake with the same name.Scientists enhanced the color in the Mars image to show the scene as it would appear under the lighting conditions we have on Earth, which helps in analyzing the terrain. The Link outcrop was imaged with the 100-millimeter Mast Camera on Sept. 2, 2012, which was the 27th sol, or Martian day of operations. JPL manages the Mars Science Laboratory/Curiosity for NASA's Science Mission Directorate in Washington. The rover was designed, developed and assembled at JPL, a division of the California Institute of Technology in Pasadena.For more about NASA's Curiosity mission, visit: http://www.jpl.nasa.gov/msl, http://www.nasa.gov/mars, and http://marsprogram.jpl.nasa.gov/msl. | |
This image from NASA's Mars Odyssey shows small, dark dunes and dust devil tracks located on the floor of Wirtz Crater on Mars. | Context image for PIA10258Wirtz CraterThese small, dark dunes and dust devil tracks are located on the floor of Wirtz Crater.Image information: VIS instrument. Latitude -48.6N, Longitude 334.8E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey spacecraft shows lava flows located between Syria Planum and Solis Planum and probably originated from volcanic vents in Syria Planum. | Context image for PIA09436Lava FlowsThese lava flows are located between Syria Planum and Solis Planum and probably originated from volcanic vents in Syria Planum.Image information: VIS instrument. Latitude -20.1N, Longitude 258.6E. 17 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of the plains of Terra Sirenum. | Context imageThe THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of the plains of Terra Sirenum.Orbit Number: 36434 Latitude: -38.7176 Longitude: 220.775 Instrument: VIS Captured: 2010-03-02 06:07Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Global Surveyor shows a young impact crater that formed in Arabia Terra on Mars. | Figure AAnnotated ImageNo AnnotationFigure BAnnotated ImageNo AnnotationThese Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) images show a young impact crater that formed in Arabia Terra near 22.2°N, 345.5°W, some time between 2 April 2001 and 11 December 2003. This image and figure A are sub-frames of MOC image S16-01199, acquired on 13 March 2006. This image has been colorized using a look-up table derived from color data acquired by the Mars Reconnaissance Orbiter's High Resolution Stereo Camera (HRSC). The site features a crater about 24.0 ± 3.0 meters (about 79 feet) across. In other words, one can compare a 100 yard U.S. style football field with this 26 yards wide crater. The "blast zone" around the crater is much larger and includes combination of rays and chains of small secondary impacts. Figure B: This picture shows how the timing of the impact event was constrained. The first picture is a sub-frame of MOC red wide angle image E03-00127, obtained on 2 April 2001. The white circle indicates the impact site. The second picture, obtained after the impact occurred, is MOC red wide angle camera image R12-01350, acquired on 11 December 2003. The Mars Global Surveyor mission is managed for NASA's Office of Space Science, Washington, by the Jet Propulsion Laboratory, a division of the California Institute of Technology, 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. | |
The prominent rock in this image from NASA's rover Curiosity, informally named 'East Bull Rock,' is about 20 inches (half a meter) high. The rock-studded local rise dominating the image is called 'Elsie Mountain'. | NASA's Mars rover Curiosity used the Navigation Camera (Navcam) on its mast to record this westward look on the 347th Martian day, or sol, of the rover's work on Mars (July 28, 2013). The rover had completed a southwestward drive of 60.1 meters on that sol. The prominent rock in the right foreground, informally named "East Bull Rock," is about 20 inches (half a meter) high. The rock-studded local rise dominating the image is called "Elsie Mountain." A distant portion of the rim of Gale Crater is visible in the upper portion of the view. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the project's Curiosity rover.More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
This image taken by the HiRISE camera on NASA's Mars Reconnaissance Orbiter, captures Opportunity traversing south (at the end of the white arrow) to new science targets and a winter haven at 'Solander Point,' another portion of the Endeavour rim. | Figure 1Figure 2Figure 3Click on an individual image for full resolution imageNASA's Mars Exploration Rover Opportunity has been on the western rim of Endeavour Crater in Meridiani Planum for about two years. Until May 2013, it was investigating sedimentary layers that are three to four billion years old on a portion of the rim called "Cape York." This image taken by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter on July 8, 2013, captures Opportunity traversing south (at the end of the white arrow) to new science targets and a winter haven at "Solander Point," another portion of the Endeavour rim. The relatively level ground between Cape York and Solander Point is called "Botany Bay." The image was taken 10 years after Opportunity was launched from Florida on July 7, 2013, EDT and PDT (July 8, Universal Time).Opportunity's destination at Solander Point is thought to have clay-bearing rocks (as detected from orbit) as part of well-exposed geological layers that could provide clues to Mars' watery past. In addition, north-facing slopes on Solander Point will increase the amount of solar energy the rover can collect during the upcoming Mars southern-hemisphere winter, allowing an active winter science campaign.Opportunity investigated younger sedimentary units exposed in the smaller craters of Eagle, Endurance, and Victoria from early 2004 to mid-2009. By driving across Meridiani from Victoria to Endeavour Crater, and now from point-to-point on Endeavour's rim, Opportunity has set a new U.S. space program record for distance traversed on another planetary body, at greater than 22 miles or 36 kilometers.Figure 1, an oblique, northward-looking view based on stereo orbital imaging, shows the location of Opportunity on its journey from Cape York to Solander Point when HiRISE took the new color image. Endeavour Crater is about 14 miles (22 kilometers) in diameter. The distance from Cape York to Solander Point is about 1.2 miles (2 kilometers). The red line indicates the path the rover has driven.Figure 2 shows the location of the rover-containing section of new color image in relation to Solander Point. North is up. The scale bar is 250 meters (820 feet).Figure 3 is an unannotated version of a section of the new color image including the rover.This new image, HiRISE digital terrain modeling and cameras on Opportunity aid rover drivers in identifying safe routes. Additionally, they assist NASA geologists in finding attractive science targets for future investigation. The new image is one product from HiRISE observation ESP_032573_1775. Other products from the observation are at http://uahirise.org/ESP_032573_1775.HiRISE is one of six instruments on NASA's Mars Reconnaissance Orbiter. The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter and Mars Exploration Rover projects for NASA's Science Mission Directorate, Washington. | |
NASA's Mars Global Surveyor acquired this image on July 4, 1998. Shown here is Elysium Mons, one of three large volcanoes that occur on the Elysium Rise. | On July 4, 1998--the first anniversary of the Mars Pathfinder landing--Mars Global Surveyor's latest images were radioed to Earth with little fanfare. The images received on July 4, 1998, however, were very exciting because they included a rare crossing of the summit caldera of a major martian volcano. Elysium Mons is located at 25°N, 213°W, in the martian eastern hemisphere. Elysium Mons is one of three large volcanoes that occur on the Elysium Rise-- the others are Hecates Tholus (northeast of Elysium Mons) and Albor Tholus (southeast of Elysium Mons). The volcano rises about 12.5 kilometers (7.8 miles) above the surrounding plain, or about 16 kilometers (9.9 miles) above the martian datum-- the "zero" elevation defined by average martian atmospheric pressure and the planet's radius.Elysium Mons was discovered by Mariner 9 in 1972. It differs in a number of ways from the familiar Olympus Mons and other large volcanoes in the Tharsis region. In particular, there are no obvious lava flows visible on the volcano's flanks. The lack of lava flows was apparent from the Mariner 9 images, but the new MOC high resolution image--obtained at 5.24 meters (17.2 feet) per pixel--illustrates that this is true even when viewed at higher spatial resolution.Elysium Mons has many craters on its surface. Some of these probably formed by meteor impact, but many show no ejecta pattern characteristic of meteor impact. Some of the craters are aligned in linear patterns that are radial to the summit caldera--these most likely formed by collapse as lava was withdrawn from beneath the surface, rather than by meteor impact. Other craters may have formed by explosive volcanism. Evidence for explosive volcanism on Mars has been very difficult to identify from previous Mars spacecraft images. This and other MOC data are being examined closely to better understand the nature and origin of volcanic features on Mars.The three MOC images, 40301 (red wide angle), 40302 (blue wide angle), and 40303 (high resolution, narrow angle) were obtained on Mars Global Surveyor's 403rd orbit around the planet around 9:58 - 10:05 p.m. PDT on July 2, 1998. The images were received and processed at Malin Space Science Systems (MSSS) around 4:00 p.m. PDT on July 4, 1998.This image: MOC image 40303 subframe of the Elysium Mons' southern caldera wall and floor shown at full resolution (5.24 meters (17.2 feet) per pixel). Illumination is from the right, north is approximately up.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. | |
NASA's Mars Global Surveyor shows the southern rim of the summit crater, or caldera, of the intermediate-sized martian volcano, Ulysses Patera on Mars. | Zoom View AnimationBroad View AnimationFigure 1: Small crater with dark,rayed ejecta was not present in 1976; rate at which ejecta faded from 1999to 2005 suggests mid-1980s age.Figure 2: Comparison of MOC wide angleviews with Viking 2 viewFigure 3: Context view, Ulysses Patera volcanoin U.S. Geological Survey mosaic ofViking Orbiter imagesScientists using the Mars Orbiter Camera on NASA's Mars Global Surveyor spacecraft have discovered a crater that appears to have formed on Mars in the past 20 or so Earth years, and have used it and several other similar craters to estimate the present cratering rate on Mars.One of the basic tenets of planetary geology is that impact craters have accumulated on planetary surfaces at roughly a constant rate since the early history of the solar system. This appears to have been the case for small craters on the surface of the Moon, as shown by measurements of the length of time that lunar rocks created by small impacts have been exposed to cosmic rays, as determined by laboratory measurements of samples returned to Earth by the Apollo astronauts. This principle should permit the number of craters found on a planetary surface to be used to determine the age of that surface, if the rate at which new craters form is known. Scientists have previously estimated the cratering rate of Mars by scaling the lunar cratering rate based on the proximity of Mars to the asteroid belt, and by performing calculations based on orbital mechanics. Another way to establish the cratering rate of Mars would be to use long-term observations, say, from orbiting spacecraft, to actually locate new craters. The new crater is located on the southern rim of the summit crater, or caldera, of the intermediate-sized martian volcano, Ulysses Patera. The site was imaged by the Viking 2 orbiter in 1976 (left, an enlarged portion of the image) and in narrow-angle views by the Mars Orbiter Camera in 1999 (center) and 2005 (right). The new crater, about 25 meters (82 feet) across, is marked by a distinct dark, rayed pattern of ejected material, or ejecta, which is seen to have faded somewhat between 1999 and 2005. Ulysses Patera, a volcanic shield about 100 kilometers (62 miles) in diameter volcanic shield, located near 2.5 degrees north latitude, 121.3 degrees west longitude, is one of the Tharsis volcanoes and is partly buried by younger lava flows. The summit caldera is about 55 kilometers (34 miles) in diameter.The amount that the crater's rays faded between 1999 and 2005 can be used to help estimate how many years ago the crater formed. The actual contrast between the ejecta and the undisturbed volcano summit materials is actually much less than it appears to be in these processed images, and the amount of fading is also much less. Images of disturbed surfaces from various parts of Mars, such as dust devil tracks, dark slope streaks and rover tracks, indicate that disturbed surfaces on Mars are dark and that they lighten with time. Using these other examples to estimate how dark the ejecta from the Ulysses crater was originally, and how much it has faded in six years, suggests the crater formed in the early to mid 1980s. The rate at which dark surfaces lighten on Mars is not uniform over the whole planet, but scientists using the Mars Orbiter Camera have found a number of other craters with dark ejecta that have faded during the Mars Global Surveyor mission. The scientists estimate that these craters probably formed within the past 100 years. Although the sample is very small (the Mars Orbiter Camera narrow angle camera has imaged barely 4 percent of Mars), it appears that the recent cratering rate for craters on Mars 25 to 100 meters (82 to 328 feet) in diameter is about 0.000000003 to 0.000000006 craters per square kilometer (0.39 square mile) per Earth year, which is about five times lower than previous estimates. The site of the new crater is shown in wider context in a comparison of the 1976 Viking image with wide-angle views taken by the Mars Orbiter Camera in 1999 and 2005 (figure 2), and in even wider context in a regional mosaic of Viking images (figure 3). The Mars Orbiter Camera was built and is operated by Malin Space Science Systems, San Diego, Calif. Mars Global Surveyor left Earth on Nov. 7, 1996, and began orbiting Mars on Sept. 12, 1997. JPL, a division of the California Institute of Technology, Pasadena, manages Mars Global Surveyor for NASA's Science Mission Directorate, Washington. | |
Starburst Spider | Mars' seasonal cap of carbon dioxide ice has eroded many beautiful terrains as it sublimates (goes directly from ice to vapor) every spring. In the region where the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter took this image, we see troughs that form a starburst pattern. In other areas these radial troughs have been refered to as spiders, simply because of their shape. In this region the pattern looks more dendritic as channels branch out numerous times as they get further from the center. The troughs are believed to be formed by gas flowing beneath the seasonal ice to openings where the gas escapes, carrying along dust from the surface below. The dust falls to the surface of the ice in fan-shaped deposits. This image, covering an area about 1 kilometer (0.6 mile) across, is a portion of the HiRISE observation cataloguedas ESP_011842_0980, taken on Feb. 4, 2009. The observation is centered at 81.8 degrees south latitude, 76.2 degrees east longitude. The image was taken at a local Mars time of 4:56 PM and the scene is illuminated from the west with a solar incidence angle of 78 degrees, thus the sun was about 12 degrees above the horizon. At a solar longitude of 203.6 degrees, the season on Mars is 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 & Technologies Corp., Boulder, Colo. | |
This image from NASA's Mars Odyssey shows a large sand sheet with surface dune forms located on the complex floor of Rabe Crater. | Context imageThe large sand sheet with surface dune forms seen in this VIS image is located on the complex floor of Rabe Crater. The sand is likely derived by erosion into the deposit that fills most of the crater floor, creating a pit which hosts the dunes. This crater morphology is unique to Rabe Crater. Rabe Crater is located in Noachis Terra and is 108km in diameter (67 miles).Orbit Number: 84884 Latitude: -43.4896 Longitude: 34.4426 Instrument: VIS Captured: 2021-02-01 15:04Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows linear depressions, part of Sirenum Fossae. | Context imageThe linear depressions in this VIS image are part of Sirenum Fossae. These depressions are called graben, which form by the down drop of material between two parallel faults. The faults are caused by extensional tectonic stresses in the region. The fossae are 2735km long (1700 miles).Orbit Number: 83767 Latitude: -25.1526 Longitude: 220.709 Instrument: VIS Captured: 2020-11-01 15:42Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Exploration Rover Opportunity captured this view of a portion of Endeavour crater's rim after a drive on Aug. 4, 2011 to reach 'Spirit Point,' the chosen arrival site. | NASA's Mars Exploration Rover Opportunity used its panoramic camera (Pancam) to capture this view of a portion of Endeavour crater's rim after a drive during the rover's 2,676th Martian day, or sol, of working on Mars (Aug. 4, 2011). The drive covered 396 feet (120.7 meters) and put the rover with about that much distance to go before reaching the chosen arrival site at the rim, called "Spirit Point."Endeavour crater has been the rover team's destination for Opportunity since the rover finished exploring Victoria crater in August 2008. Endeavour, with a diameter of about 14 miles (22 kilometers), offers access to older geological deposits than any Opportunity has seen before.This view looks toward a portion of the rim south of Spirit Point, including terrain that Opportunity may explore in the future. | |
NASA's Mars Global Surveyor shows | 13 February 2004 This pair of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) narrow angle images shows the landing site of the Mars Exploration Rover (MER-B), Opportunity, before and after the landing. The first image was acquired on 24 August 2003, five months prior to the 25 January 2004 landing. The second picture, obtained on 1 February 2004, shows the lander--located within a ~20 meter (~66 feet) diameter crater--and other features that resulted from the landing. The Opportunity landing site is located in Meridiani Planum near 2.0°S, 5.6°W. Both images are simple cylindrical map projections with north up and east to the right; the lower image is about 1.4 kilometers (0.9 miles) wide. The dark area on the right side of the upper picture was not imaged by MOC until after the landing. Sunlight illuminates each scene from the lower left. | |
This image from NASA's Mars Exploration Rover Opportunity shows 'Bounce Rock.' There appears to be a dusty coating on the top of parts of the rock, which may have been broken when it was struck by the airbags while rolling to a stop. | Figure 1This Mars Exploration Rover Opportunity panoramic camera image shows "Bounce Rock," a rock the airbag-packaged rover struck while rolling to a stop on January 24, 2004. This is the largest rock for as far as the eye can see, approximately 35 centimeters (14 inches) long and 10 centimeters (4 inches) high. There appears to be a dusty coating on the top of parts of the rock, which may have been broken when it was struck by the airbags. The rock was about 5 meters (16 feet) from the rover when this image was obtained. This is an enhanced color composite image from sol 36 of the rover's journey, generated using the camera's L2 (750 nanometer), L5 (530 nanometer), and L6 (480 nanometer) filters.Bounce Rock SpectraFigure 1 above is a plot of panoramic camera spectra extracted from three different regions on the rock dubbed "Bounce." The yellow spectrum is from the yellow box in the image on the left, from the dusty top part of the rock. The spectrum is dominated by the signature of oxidized "ferric" iron (Fe3+) like that seen in the classic Martian dust. The red spectrum is from the darker Meridiani Planum soils that were disturbed by the airbag when it bounced near the rock. That spectrum is also dominated by ferric iron, though the reflectivity is lower. Scientists speculate that this may be because the grains are coarser in these soils compared to the dust. The green spectrum, which is from the right side of the rock, shows a strong drop in the infrared reflectance that is unlike any other rock yet seen at Meridiani Planum or Gusev Crater. This spectral signature is typical of un-oxidized "ferrous" iron (Fe2+) in the rock, perhaps related to the presence of volcanic minerals like olivine or pyroxene. The possibility that this may be a basaltic rock that is distinctly different from the rocks seen in the Eagle Crater outcrop is being intensively explored using the rover's other instruments. | |
This image shows inclined beds characteristic of delta deposits where a stream entered a lake, but at a higher elevation and farther south than other delta deposits north of Mount Sharp. | Figure 1Click on the image for larger versionThis image from the Mast Camera (Mastcam) on NASA's Curiosity Mars rover shows inclined strata at "Zabriskie Plateau," about a third of a mile (half a kilometer) northeast of the "Pahrump Hills" outcrop at the base of Mount Sharp. The view looks to the west. These sedimentary rocks, like those at "Kimberley," (see PIA19070) are inclined toward the south and are also interpreted as the deposits of small deltas building out into a lake. Remarkably, these inclined beds occur at an elevation about 80 feet (about 25 meters) higher than at Kimberley. This suggests that they represent a younger cycle of delta growth than those observed at Kimberley, and importantly in a more basinward location. There were likely multiple episodes of delta growth into a Gale Crater lake as sediment accumulated in the basin, with the deltas encroaching further southward over time.The Mastcam's left-eye camera recorded the component frames of this mosaic on July 22, 2014, during the 696th Martian day, or sol, of Curiosity's work on Mars. The color has been approximately white-balanced to resemble how the scene would appear under daytime lighting conditions on Earth. Figure 1 is a version with a superimposed scale bar of 1.5 meters (about 5 feet).NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. JPL designed and built the project's Curiosity rover. Malin Space Science Systems, San Diego, built and operates the rover's Mastcam.More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
Aurorae Chaos is located at the eastern end of the chasmata forming Vallis Marineris. This image from NASA's 2001 Mars Odyssey spacecraft is very close to the chasmata and at a higher elevation than the floor of the chasmata. | Context imageAurorae Chaos is located at the eastern end of the chasmata forming Vallis Marineris. This image is very close to the chasmata and at a higher elevation than the floor of the chasmata.Orbit Number: 42171 Latitude: -11.4809 Longitude: 319.348 Instrument: VIS Captured: 2011-06-17 15:03Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
Shown in this image from NASA's Mars Reconnaissance Orbiter are fan-shaped deposits emerging from regions of steep topography called alluvial fans. Alluvial fans on Mars are thought to be ancient and record past episodes of flowing water. | Map Projected Browse ImageClick on the image for larger versionThis image from NASA's Mars Reconnaissance Orbiter (MRO) was originally meant to track the movement of sand dunes near the North Pole of Mars, but what's on the ground in between the dunes is just as interesting!The ground has parallel dark and light stripes from upper left to lower right in this area. In the dark stripes, we see piles of boulders at regular intervals.What organized these boulders into neatly-spaced piles? In the Arctic back on Earth, rocks can be organized by a process called "frost heave." With frost heave, repeatedly freezing and thawing of the ground can bring rocks to the surface and organize them into piles, stripes, or even circles. On Earth, one of these temperature cycles takes a year, but on Mars it might be connected to changes in the planet's orbit around the Sun that take much longer.The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 32 centimeters (12.6 inches) per pixel (with 1 x 1 binning); objects on the order of 96 centimeters (37.8 inches) across are resolved.] North is up.This is a stereo pair with ESP_053937_2550.The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows depressions in the surface of southern Noachis Terra. | Context imageThe THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows depressions in the surface of southern Noachis Terra.Orbit Number: 6317 Latitude: -74.0813 Longitude: 351.861 Instrument: VIS Captured: 2003-05-18 13:25Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This is a map of lower Mount Sharp on Mars, showing the major geologic units identified from orbit. The rocks of the 'Murray Formation,' mapped in green, likely represent the oldest layers of Mount Sharp that NASA's Curiosity rover will explore. | This is a map of lower Mount Sharp on Mars, showing the major geologic units identified from orbit. The rocks of the "Murray Formation," mapped in green, likely represent the oldest layers of Mount Sharp that NASA's Curiosity rover will explore. The Murray formation is in contact with two other major units: The sedimentary rocks of the crater floor that Curiosity has been exploring for the past two years, and the hematite ridge, a feature on Mount Sharp that shows a very distinct mineral composition from orbit. The segment A to A' corresponds to the geologic cross-section presented in PIA18782. This image was made using the data from the High Resolution Imaging Science Experiment (HiRISE) camera, one of six instruments on NASA's Mars Reconnaissance Orbiter. The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter and Mars Science Laboratory projects for NASA's Science Mission Directorate, Washington.More information about Curiosity is online at http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl/. | |
This image from NASA's Mars Odyssey shows part of the eastern flank of Arsia Mons, including part of Oti Fossae. | Context imageToday's VIS image shows part of the eastern flank of Arsia Mons, including part of Oti Fossae (bottom of image). Arsia Mons is the southernmost and youngest of the three large, aligned Tharsis volcanoes. Oti Fossae - linear graben - follow the major northeast/southwest trend of the volcanoes.Orbit Number: 81526 Latitude: -9.5484 Longitude: 242.037 Instrument: VIS Captured: 2020-05-01 03:58Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Exploration Rover Opportunity's view shows the rover's tracks visible at the original spot where the rover attempted unsuccessfully to exit its landing site crater in 2004. | This image shows the Mars Exploration Rover Opportunity's view on its 56th sol on Mars, before it left its landing-site crater. To the right, the rover tracks are visible at the original spot where the rover attempted unsuccessfully to exit the crater. After a one-sol delay, Opportunity took another route to the plains of Meridiani Planum. This image was taken by the rover's navigation camera. | |
This image from NASA's Mars Reconnaissance Orbiter shows the central peak in Porter Crater. Southward on the slopes below the peak is a large dune field. | Map Projected Browse ImageClick on the image for larger versionThe extended-mission status of the Mars Reconnaissance Orbiter and the HiRISE camera has greatly increased our understanding of numerous active processes occurring on Mars. By taking carefully planned repeat images of surface, we now have an important record of how the surface evolves for a maximum of 5 Mars years.This image shows the central peak in Porter Crater. Although there are no repeat images here we can infer several active geologic processes, based on morphologic evidence and lessons learned from past well-monitored sites.Shallow gullies are located on the south and east facing slopes of the central peak. These features might have been carved by volatiles, such as carbon dioxide frost, sometime in the recent geologic past.Meanwhile on the northern slopes are several smaller slope features that have a morphology hinting at recurring slope lineae (RSL). Alternatively, these features could be the remnants of past active gullies. Several more HiRISE images would be needed to characterize their behavior and confirm their status as RSL (see "Recurring Slope Lineae in Equatorial Regions of Mars").Southward on the slopes below the peak is a large dune field. Dunes show sharp crests with prominent ripples, both signs of actively migrating dunes. Also, we can see dust devil tracks crossing the nearby dusty surfaces and clear evidence for ongoing modification by swirling winds that persistently remove surface dust.Ongoing operations by HiRISE are dedicated to studying all of the active surface and atmospheric processes operating on Mars. The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project and Mars Science Laboratory Project for NASA's Science Mission Directorate, Washington. | |
The jumble of eroded ridges and mesas seen in this NASA Mars Odyssey image occurs within Ares Vallis, one of the largest catastrophic outflow channels on the planet. Floods raged through this channel, pouring out into the Chryse Basin to the north. | This jumble of eroded ridges and mesas occurs within Ares Vallis, one of the largest catastrophic outflow channels on the planet. Floods raged through this channel, portions of which are up to 25 km wide, pouring out into the Chryse Basin to the north. Close inspection of the THEMIS image reveals polygonal shapes on the floor of the channel system. Polygonal terrain on Mars is fairly common although the variety of forms and scales of the polygons suggests multiple modes of origin. Those in Ares Vallis resemble giant desiccation polygons that form in soils on Earth when a moist layer at depth drys out. While polygons can form in icy soils (permafrost) and even lava flows, their presence in a channel thought to have been carved by flowing water is at least consistent with a mode of origin that involved liquid water.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image, acquired on July 30, 2019 by NASA's Mars Reconnaissance Orbiter, shows Alga Crater, located in the southern highlands near a large flood-channel called Ladon Valles. | Map Projected Browse ImageClick on image for larger versionThe most habitable places on Mars now and in the past are underground, where water is or was much more stable than at the surface and protected from energetic particle radiation. Large impact craters have central rebounds that uplift buried strata from miles below the surface. Often these central uplifts reveal colorful rocks with diverse minerals, including ones altered by prolonged contact with water. Alga Crater is located in the southern highlands near a large flood-channel called Ladon Valles. The image cutout shows enhanced (infrared-shifted) color.The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. (The original image scale is 25.8 centimeters [10.2 inches] per pixel [with 1 x 1 binning]; objects on the order of 77 centimeters [30.3 inches] across are resolved.) North is up.The University of Arizona, in Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., in Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
NASA's Mars Global Surveyor shows part of a network of ancient valleys in northern Arabia Terra near Moreux Crater on Mars. The valleys may have originally been carved by a liquid such as water. | 19 January 2004Covered by an eroded mantle of--perhaps--cemented dust, this Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows part of a network of ancient valleys in northern Arabia Terra near Moreux Crater. The valleys may have originally been carved by a liquid such as water. The scene is located near 40.6°N, 316.4°W. The rugged surface of this mantled scene is a common feature at middle latitudes in both hemispheres of Mars. Some science investigators in the past several years have speculated that ice was once present in such mantles, and that the ice must have sublimed away to create the texture. The image covers an area about 3 km (1.9 mi) wide and is illuminated by sunlight from the lower left. | |
This image shows the summit of Hecates Tholus on Mars. The summit caldera is located in the top of the image as seen by NASA's 2001 Mars Odyssey. | Context image for PIA02683Tholus SummitThis image shows the summit of Hecates Tholus. The summit caldera is located in the top of the image.Image information: VIS instrument. Latitude 31.6N, Longitude 150.0E. 19 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
Impact craters can be created anywhere on the surface of Mars at any time. This image taken by NASA's 2001 Mars Odyssey shows a crater located on the floor of Coprates Chasma. | Context imageImpact craters can be created anywhere on the surface of Mars at any time. This crater is located on the floor of Coprates Chasma.Orbit Number: 36469 Latitude: -12.1165 Longitude: 294.981 Instrument: VIS Captured: 2010-03-05 03:08Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey spacecraft shows a portion of the floor of Ophir Chasma on Mars. At top is a landslide deposit. In the center is a wind and perhaps water eroded highland. At bottom wind appears to be the main agent of erosion. | Context image for PIA10057Ophis ChasmaThis VIS image shows a portion of the floor of Ophir Chasma. At the top of the frame is a landslide deposit. In the center is a wind and perhaps water eroded highland. At the bottom part of the image wind appears to be the main agent of erosion.Image information: VIS instrument. Latitude -3.7N, Longitude 287.0E. 18 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's 2001 Mars Odyssey spacecraft shows a portion of the floor of Antoniadi Crater. The faint, dark marks may be dust devil tracks. | Context imageThis VIS image shows a portion of the floor of Antoniadi Crater. The faint, dark marks may be dust devil tracks.Orbit Number: 53141 Latitude: 19.8044 Longitude: 61.0929 Instrument: VIS Captured: 2013-12-06 13:16Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows central Acidalia Planitia. The crater just off the edge at the bottom part of the image is Bonestell Crater. | Context imageThis VIS image is located in central Acidalia Planitia. The crater just off the edge at the bottom part of the image is Bonestell Crater. The crater towards the top of the image is unnamed. Blue tones in false color images indicated basaltic sand.The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image.Orbit Number: 61938 Latitude: 42.3825 Longitude: 329.019 Instrument: VIS Captured: 2015-11-30 17:59Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
NASA's Mars Exploration Rover Opportunity shows the rover's rock abrasion tool before and after it ground into a rock at Meridiani Planum, Mars. The red dust coating on the instrument is thought to be a form of the mineral hematite. | This image taken by the Mars Exploration Rover Opportunity's panoramic camera shows the rover's rock abrasion tool before and after it ground into a rock at Meridiani Planum, Mars. The red dust coating on the instrument is thought to be a form of the mineral hematite. The image on the left was taken on the 29th martian day, or sol, of the rover's mission, and the image on the right on the 31st sol. | |
These dunes occur in the Syrtis Major volcanic complex, near Meroe Patera on Mars as seen by NASA's 2001 Mars Odyssey spacecraft. | Context image for PIA08597Meroe DunesThese dunes occur in the Syrtis Major volcanic complex, near Meroe Patera.Image information: VIS instrument. Latitude 6.3N, Longitude 68.3E. 18 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images. Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows a section of Scamander Vallis. Scamander Vallis is located in northern Terra Sabaea. The channel is 269km (167 miles) long. | Context imageToday's VIS image shows a section of Scamander Vallis. Scamander Vallis is located in northern Terra Sabaea. The channel is 269km (167 miles) long.Orbit Number: 94873 Latitude: 15.4254 Longitude: 28.7992 Instrument: VIS Captured: 2023-05-05 03:35Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This sprawling look at the martian landscape surrounding the Mars Exploration Rover Spirit is the first 3-D stereo image from the rover's navigation camera. 'Sleepy Hollow' can be seen to center left of the image. 3D glasses are necessary. | This sprawling look at the martian landscape surrounding the Mars Exploration Rover Spirit is the first 3-D stereo image from the rover's navigation camera. A surface depression nicknamed "Sleepy Hollow" can be seen to center left of the image. Scientists theorize that this topographic feature, measuring about 10 meters (30 feet) in diameter and located approximately 10 to 20 meters (30 to 60 feet) away from Spirit, is either an impact crater or a product of wind erosion. | |
At the bottom of this image of Daedalia Planum is the uppermost rim of an impact crater. This image was captured by NASA's 2001 Mars Odyssey spacecraft. | Context image At the bottom of this VIS image of Daedalia Planum is the uppermost rim of an impact crater. The unnamed crater has been almost completely filled by lava flows originating from Arsia Mons.Orbit Number: 71346 Latitude: -21.6885 Longitude: 229.536 Instrument: VIS Captured: 2018-01-13 18:33Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
On Nov. 26, 2018, MarCO-B, one of NASA's Mars Cube One (MarCO) CubeSats, took this image of Mars from about 10,900 miles (17,500 kilometers) away just after NASA's InSight spacecraft landed on Mars. | MarCO-B, one of the experimental Mars Cube One (MarCO) CubeSats, took this image of Mars from about 10,900 miles (17,500 kilometers) away just after NASA's InSight spacecraft landed on Mars on Nov. 26, 2018. MarCO-B flew by Mars with its twin, MarCO-A, to serve as communications relays for InSight as it touched down on the Red Planet around noon PST (3 p.m. EST). This image was taken at 1 p.m. PST (4 p.m. EST).Mars' south pole is facing the viewer in this image. MarCO-B's antenna reflector is on the right and antenna feed (white rectangle with gold square) is on the left. The Sun at upper right overexposed part of the image. This image was taken after PIA22833 and shortly before PIA22834.The MarCO and InSight projects are managed for NASA's Science Mission Directorate, Washington, by JPL, a division of the California Institute of Technology, Pasadena. | |
This image from an animation shows wind blowing sand underneath NASA's Curiosity Mars rover on a non-driving day for the rover. | Figure 1AnimationClick on images for full resolutionThe pair of images in this animation shows effects of one Martian day of wind blowing sand underneath NASA's Curiosity Mars rover on a non-driving day for the rover. Each image was taken just after sundown by the rover's downward-looking Mars Descent Imager (MARDI). The area of ground shown in the images spans about 3 feet (about 1 meter) left-to-right.The first image was taken on Jan. 23, 2017, during the 1,587th Martian day, or sol, of Curiosity's work on Mars. Figure 1 above is the image with a scale bar in centimeters. The second was taken on Jan. 24, 2017 (Sol 1588). The day-apart images by MARDI were taken as a part of investigation of wind's effects during Martian summer, the windiest time of year in Gale Crater. When Curiosity landed inside Gale Crater in August 2012, MARDI recorded the descent from the rover's point of view. Malin Space Science Systems, San Diego, built and operates MARDI.NASA's Jet Propulsion Laboratory, a division of the Caltech in Pasadena, California, manages the Mars Science Laboratory Project for the NASA Science Mission Directorate, Washington, and built the project's Curiosity rover.For more information about Curiosity, visit http://www.nasa.gov/msl and http://mars.jpl.nasa.gov/msl. | |
On Sol 32 (Sept. 7, 2012) the Curiosity rover used a camera located on its arm to obtain this self portrait. The MAHLI cover was in the closed position in order to inspect the dust cover. | On Sol 32 (Sept. 7, 2012) the Curiosity rover used the Mars Hand Lens Imager (MAHLI) located on its arm to obtain this self-portrait. The image shows the top of Curiosity's Remote Sensing Mast including the ChemCam, two Mast cameras and four Navigation cameras. The angle of the frame reflects the position of the MAHLI camera on the arm when the image was taken. The image was acquired while MAHLI's clear dust cover was closed.The image was taken on a day when MAHLI and other instruments and tools on the turret were being inspected using the rover's Mastcams and Navcams. The MAHLI cover was in the closed position in order to inspect the dust cover to esure that the cover, its hinge, and the volume it sweeps when it opens are clear of debris. | |
The two linear depressions in this image from NASA's Mars Reconnaissance Orbiter spacecraft form part of the Elysium Fossae complex, a group of troughs located in the Elysium quadrangle of Mars. | Map Projected Browse ImageClick on the image for larger versionThe two linear depressions in this image form part of the Elysium Fossae complex, a group of troughs located in the Elysium quadrangle of Mars.These troughs are tectonic features, likely formed by the stretching, tearing and subsequent collapse of the crust resulting from the rise of the nearby Elysium volcanic province. The north and south troughs in this image are roughly 4.8 and 3.7 kilometers across respectively, and around 800 meters deep. Strata, or layering from successive deposition of material (likely ash and lava), are exposed in the upper wall of the trough.Upon closer inspection, another interesting phenomenon becomes visible: slope streaks. Observable on the slopes of both troughs, these dark features (also known as dust avalanches) are the result of a mass movement of loose, fine-grained material exposing darker material. Over time, these features superpose and cross-cut one another, manifesting as light-toned angular features on either side of the slope streak. Slope streaks have also been known to form as the result of an impact on or near the slope which shakes loose dust, triggering an avalanche. The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colo. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington. | |
This image from NASA's Mars Odyssey spacecraft shows a location close to Mars' equator, near the southern edge of a low, broad volcanic feature called Syrtis Major. | (Released 6 June 2002)The ScienceThis image, located near the equator and 288W (72E), is near the southern edge of a low, broad volcanic feature called Syrtis Major. A close look at this image reveals a wrinkly texture that indicates a very rough surface that is associated with the lava flows that cover this region. On a larger scale, there are numerous bright streaks that trail topographic features such as craters. These bright streaks are in the wind shadows of the craters where dust that settles onto the surface is not as easily scoured away. It is important to note that these streaks are only bright in a relative sense to the surrounding image. Syrtis Major is one of the darkest regions on Mars and it is as dark as fresh basalt flows or dunes are on Earth.The StoryCool! It almost looks as if nature has "painted" comets on the surface of Mars, using craters as comet cores and dust as streaky tails. Of course, that's just an illusion. As in many areas of Mars, the wind is behind the creation of such fantastic landforms. The natural phenomenon seen here gives this particular surface of Mars a very dynamic, fast-moving, almost luminous "cosmic personality."The bright, powdery-looking streaks of dust are in the "wind shadows" of craters, where dust that settles onto the surface is not as easily scoured away. That's because the wind moves across the land in a particular direction, and a raised surface like the rim of a crater "protects" dust from being completely blown away on the other side. The raised landforms basically act as a buffer. From the streaks seen above, you can tell the wind was blowing in a northeast to southwest direction.Why are the streaks so bright? Because they contrast with the really dark underlying terrain in this volcanic area of Mars. Syrtis Major is one of the darkest regions on Mars because it is made of basalt. Basalt is typically dark gray or black, and forms when a certain type of molten lava cools. The meaning of the word basalt has been traced back to an ancient Ethiopian word "basal," which means "a rock from which you can obtain iron." That must have made it a very desired material with ancient Earth civilizations long ago.Basalt is actually one of the most abundant types of rock found on Earth. Most of the volcanic islands in the ocean are made of basalt, including the large shield volcano of Mauna Loa, Hawaii, which is often compared to Martian shield volcanoes. Shield volcanoes don't have high, steep, mountain-like sides, but are instead low and broad humps upon the surface. They're created when highly fluid, molten-basalt flows spread out over wide areas. Over several millennia of basaltic layering upon layering, these volcanoes can reach massive sizes like the ones seen on Mars. You can see the wrinkly texture of dark lava flows (now hard and cool) in the above image beneath the brighter dust. | |
This image from NASA's Mars Odyssey shows part of one of the Elysium Fossae on the western flank of the Elysium volcanic complex. The fossae have both a tectonic and volcanic origin. | Context imageToday's VIS image shows part of one of the Elysium Fossae on the western flank of the Elysium volcanic complex. The fossae have both a tectonic and volcanic origin. The linear fractures, representing tectonic activity, are aligned southeast to northwest (the top of the image is north). The sinuous nature of the channel is due the flow of a liquid, most likely lava in this case.Orbit Number: 72434 Latitude: 28.0172 Longitude: 139.454 Instrument: VIS Captured: 2018-04-13 09:56Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows the floor of Peridier Crater. Small dunes are visible in the image. Dark blue tones indicate basaltic sands. | Context imageThe THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows the floor of Peridier Crater. Small dunes are visible in the image. Dark blue tones indicate basaltic sands. Peridier Crater is 94 km (58 miles) in diameter.Orbit Number: 71276 Latitude: 25.1422 Longitude: 83.61 Instrument: VIS Captured: 2018-01-08 00:25Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows Tombaugh Crater. Dark blue tones are basaltic sands of the floor of the crater. | Context imageTombaugh Crater is in the center of this VIS image. Dark blue tones are basaltic sands of the floor of the crater.The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image.Orbit Number: 60796 Latitude: 3.67604 Longitude: 161.758 Instrument: VIS Captured: 2015-08-28 16:43Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image released on July 25, 2004 from NASA's 2001 Mars Odyssey shows a decorrelation stretch near Cerberus Fossae. Pink/magenta colors usually represent basaltic content, cyan indicates the presence of water ice clouds, while green can represent dust. | Released July 25, 2004On this image you can see two infrared frames of the same area on Mars. One of the images (in black and white) represents a single wavelength or band of the THEMIS IR instrument, while the other image (in false color) represents 3 different bands. The image with the various colors was created with a technique called Decorrelation Stretch (DCS). In this technique individual bands of the THEMIS IR instrument are stretched to better show compositional variations throughout the whole range. After the bands are stretched they are overlayed on one another and colors are assigned to each band. This makes up the colors in the image.As you can see, there is a difference in what is noticable in the single band IR image versus the false-colored one. On the color image the pink/magenta colors usually represent basaltic content, cyan often indicates the presence of water ice clouds, while green can represent dust.The bright purple and pink colors associated with the valley are due to basalt. There may be a thin veneer of dust present in the region (it was a dark colored region during the Viking mission in the 1970's) through which the basaltic material pokes out along the edges of the valley and the nearby knobby terrain.Image information: IR instrument. Latitude 10.7, Longitude 163 East (197 West). 100 meter/pixel resolution.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
The ejecta surrounding this crater in Tempe Terra has an unusual texture that appears to contain small channels and fractures on Mars as seen by NASA's Mars Odyssey spacecraft. | Context image for PIA08748Ejecta TextureThe ejecta surrounding this crater in Tempe Terra has an unusual texture that appears to contain small channels and fractures.Image information: VIS instrument. Latitude 35.7N, Longitude 284.7E. 19 meter/pixel resolution.Please see the THEMIS Data Citation Note for details on crediting THEMIS images.Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
This image from NASA's Mars Odyssey shows numerous gullies dissecting the northern rim of this unnamed crater in Terra Sirenum. | Context imageNumerous gullies dissect the northern rim of this unnamed crater in Terra Sirenum.Orbit Number: 74366 Latitude: -41.1423 Longitude: 188.928 Instrument: VIS Captured: 2018-09-19 13:05Please see the THEMIS Data Citation Note for details on crediting THEMIS images.NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Science Mission Directorate, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena. | |
The beige clouds seen in this global map of Mars are a continent-size dust storm captured on Sept. 29, 2022, by the Mars Color Imager camera aboard NASA's Mars Reconnaissance Orbiter. | The beige clouds seen in this flat global map of Mars are a continent-size dust storm captured on Sept. 29, 2022 by the Mars Color Imager (MARCI) camera aboard NASA's Mars Reconnaissance Orbiter (MRO). As MRO passes over the planet, MARCI takes linear images – essentially strips – of the planet's circumference each day. The images are then stitched together to create a daily global map of the planet, showing atmospheric features across the planet as seen at the same time of day (mid-afternoon). Comparison of daily maps show atmospheric changes over time. Besides providing unique scientific data, MARCI's global maps are useful for monitoring weather changes that could affect NASA's surface missions.The agency's Perseverance, Curiosity, and InSight missions are also labeled, showing the vast distances between them. NASA's Perseverance rover and Ingenuity helicopter, are located at the white dot farthest north, roughly 2,147 miles (3,455 kilometers) from the agency's InSight lander, just above the equator. The Curiosity rover is just below the equator, about 373 miles (600 kilometers) from InSight. Neither Curiosity nor Perseverance and Ingenuity (the helicopter must remain relatively close to Perseverance, which serves as its base station) can travel the distance to the solar-powered InSight lander.The regional dust storm in this map was first observed Sept. 21. By the time these images were taken (Sept. 29), it had expanded considerably. Within the following week, the storm appeared to have entered its decay phase, when it's no longer lifting dust into the atmosphere. At that point, the dust that has already been lofted into the atmosphere and spread far beyond the dust-raising sector can take weeks to settle back to the surface.While this particular storm was roughly 2,175 miles (3,500 kilometers) from InSight, it lofted enough dust to significantly reduce the energy being produced by the lander's solar arrays, which have become covered by dust since the spacecraft landed in November 2018.The lander has long since surpassed its primary mission. With its power steadily declining, it is now close to the end of its extended mission, conducting "bonus science" by measuring marsquakes, which reveal details about the deep interior of the Red Planet.NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages InSight for the agency's Science Mission Directorate in Washington. InSight is part of NASA's Discovery Program, managed by the agency's Marshall Space Flight Center in Huntsville, Alabama. Lockheed Martin Space in Denver built the InSight spacecraft, including its cruise stage and lander, and supports spacecraft operations for the mission.A number of European partners, including France's Centre National d'Études Spatiales (CNES) and the German Aerospace Center (DLR), are supporting the InSight mission. CNES provided the Seismic Experiment for Interior Structure (SEIS) instrument to NASA, with the principal investigator at IPGP (Institut de Physique du Globe de Paris). Significant contributions for SEIS came from IPGP; the Max Planck Institute for Solar System Research (MPS) in Germany; the Swiss Federal Institute of Technology (ETH Zurich) in Switzerland; Imperial College London and Oxford University in the United Kingdom; and JPL. DLR provided the Heat Flow and Physical Properties Package (HP3) instrument, with significant contributions from the Space Research Center (CBK) of the Polish Academy of Sciences and Astronika in Poland. Spain's Centro de Astrobiología (CAB) supplied the temperature and wind sensors.JPL also manages MRO for NASA's Science Mission Directorate in Washington. Lockheed Martin Space built MRO. The Mars Color Imager camera, or MARCI, was built and is managed by Malin Space Science Systems in San Diego. | |
NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this stereo, full-circle view of the rover's surroundings on March 10, 2009. 3D glasses are necessary to view this image. | Left-eye view of a color stereo pair for PIA11973Right-eye view of a color stereo pair for PIA11973NASA's Mars Exploration Rover Spirit used its navigation camera to take the images that have been combined into this stereo, full-circle view of the rover's surroundings during the 1,843rd Martian day, or sol, of Spirit's surface mission (March 10, 2009). South is in the middle. North is at both ends.This view combines images from the left-eye and right-eye sides of the navigation camera. It appears three-dimensional when viewed through red-blue glasses with the red lens on the left. The rover had driven 36 centimeters downhill earlier on Sol 1854, but had not been able to get free of ruts in soft material that had become an obstacle to getting around the northeastern corner of the low plateau called "Home Plate."The Sol 1854 drive, following two others in the preceding four sols that also achieved little progress in the soft ground, prompted the rover team to switch to a plan of getting around Home Plate counterclockwise, instead of clockwise. The drive direction in subsequent sols was westward past the northern edge of Home Plate. This view is presented as a cylindrical-perspective projection with geometric seam correction. | |
NASA's Mars Global Surveyor shows some of the layered, sedimentary rock outcrops exposed on a mound in Gale Crater on Mars. | MGS MOC Release No. MOC2-480, 11 September 2003This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) picture shows some of the layered, sedimentary rock outcrops exposed on a mound in Gale Crater near 5.0°S, 221.8°W. These layers represent a long history of sedimentation that occurred in Gale Crater at some time in the distant martian past. Later, these layers were eroded and exposed. Gale Crater may once have been completely filled by these layered materials. The picture covers an area 3 km (1.9 mi) across and is illuminated by sunlight from the left. |
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