Mars
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The High Resolution Stereo Camera on board ESA's Mars Express imaged the Eumenides Dorsum mountains on the Red Planet. Eumenides Dorsum is located in to the west of the Tharsis Region, and forms part of the Medusae-Fossae Region, at approximately 2° south and 206° east. The images, taken on 26 December 2007, have a ground resolution of about 13 m/pixel and cover an area of about 12 000 square km. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Perspective view of Euminedes Dorsum
The High Resolution Stereo Camera on board ESA's Mars Express imaged the Eumenides Dorsum mountains on the Red Planet. Eumenides Dorsum is located in to the west of the Tharsis Region, and forms part of the Medusae-Fossae Region, at approximately 2° south and 206° east. The images, taken on 26 December 2007, have a ground resolution of about 13 m/pixel and cover an area of about 12 000 square km. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Perspective view of Euminedes Dorsum
The High Resolution Stereo Camera on board ESA's Mars Express imaged the Eumenides Dorsum mountains on the Red Planet. Eumenides Dorsum is located in to the west of the Tharsis Region, and forms part of the Medusae-Fossae Region, at approximately 2° south and 206° east. The images, taken on 26 December 2007, have a ground resolution of about 13 m/pixel and cover an area of about 12 000 square km. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Euminedes Dorsum
This image was obtained by the High Resolution Stereo Camera (HRSC) on board ESA's Mars Express on 28 July 2008 (orbit 5870), at a distance of 351 km from the moon's centre. The image was taken using the camera's nadir channel, at a resolution of 14 m/pixel. The origin of Phobos is debated. While its density, lower than the density of the Martian surface rocks, make it appear to belong to D-class asteroids, the moon appears to share many surface characteristics with the class of carbonaceous C-type asteroids, which suggests it might have been captured from this population. However, it is difficult to explain either the capture mechanism or the following evolution of its orbit into the equatorial plane of Mars. An alternative hypothesis is that it formed in its present position, and is therefore a remnant from the planetary formation period. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Phobos
The Mangala Fossae trough is a system of outflow channels on Mars that bears evidence of lava deposition and catastrophic floods. The HRSC on board Mars Express obtained images of this region centred at 17° south and 213° east on 21 March 2007. Mangala Fossae is approximately 1000 km long, located south-west of the volcanic region Tharsis, where the highest known volcano in the Solar System, Olympus Mons, is located. The western part of the region is remarkably smooth and exhibits just a few small impact craters, larger craters being absent. Since the crater count relates directly to the age of the region (the more the number of craters, the older the uppermost layer of material), and only few small craters are seen in the area, this indicates that the uppermost surface layer is young and that the basaltic lava was put in place relatively recently. The lava flows most likely originated in the Tharsis Region. Sharp edges of the 100-m thick lava blanket are visible in some places. This perspective view has been calculated from the digital terrain model derived from the stereo channels. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Perspective view of Mangala Fossae
The Mangala Fossae trough is a system of outflow channels on Mars that bears evidence of lava deposition and catastrophic floods. The HRSC on board Mars Express obtained images of this region centred at 17° south and 213° east on 21 March 2007. Mangala Fossae is approximately 1000 km long, located south-west of the volcanic region Tharsis, where the highest known volcano in the Solar System, Olympus Mons, is located. The western part of the region is remarkably smooth and exhibits just a few small impact craters, larger craters being absent. Since the crater count relates directly to the age of the region (the more the number of craters, the older the uppermost layer of material), and only few small craters are seen in the area, this indicates that the uppermost surface layer is young and that the basaltic lava was put in place relatively recently. This perspective view has been calculated from the digital terrain model derived from the stereo channels. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Perspective view of Mangala Fossae
The Mangala Fossae trough, a system of outflow channels on Mars that bears evidence of lava deposition and catastrophic floods. The HRSC on board Mars Express obtained images of this region centred at 17° south and 213° east on 21 March 2007. Mangala Fossae is approximately 1000 km long, located south-west of the volcanic region Tharsis, where the highest known volcano in the Solar System, Olympus Mons, is located. This colour scene has been derived from the three HRSC-colour channels and the nadir channel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Mangala Fossae
HRSC Stereo Channel 1 image of Phobos with a resolution of 3.7 m/pixel at its best. The inset to the right shows the potential landing region and sites for the Russia’s Phobos-Grunt sample return mission, due for launch in 2009. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Potential Phobos-Grunt landing site
On 23 July 2008, the High Resolution Stereo Camera on board the ESA's Mars Express took the highest-resolution full-disc image yet of the surface of the moon Phobos. The image data was acquired from a distance of 97 km with a spatial resolution of about 3.7 m/pixel in orbit 5851. These images have surpassed all previous images from other missions in continuous coverage of the illuminated surface at the highest spatial resolution of 3.7 m/pixel. This image has been geometrically corrected and exhibits the original illumination and photometric conditions. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Phobos
The High-Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Echus Chasma, one of the largest water source regions on the Red Planet. Echus Chasma is the source region of Kasei Valles which extends 3000 km to the north. The data was acquired on 25 September 2005. The pictures are centred at about 1° north and 278° east and have a ground resolution of approximately 17 m/pixel. An impressive cliff, up to 4000 m high, is located in the eastern part of Echus Chasma. Gigantic water falls may once have plunged over these cliffs on to the valley floor. The remarkably smooth valley floor was later flooded by basaltic lava. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Perspective view of Echus Chasma
The High-Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Echus Chasma, one of the largest water source regions on the Red Planet. Echus Chasma is the source region of Kasei Valles which extends 3000 km to the north. The data was acquired on 25 September 2005. The pictures are centred at about 1° north and 278° east and have a ground resolution of approximately 17 m/pixel. The dark material shows a network of light-coloured, incised valleys that look similar to drainage networks known on Earth. It is still debated whether the valleys originate from precipitation, groundwater springs or liquid or magma flows on the surface. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Perspective view of Echus Chasma
The High-Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Echus Chasma, one of the largest water source regions on the Red Planet. Echus Chasma is the source region of Kasei Valles which extends 3000 km to the north. The data was acquired on 25 September 2005. The pictures are centred at about 1° north and 278° east and have a ground resolution of approximately 17 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Perspective view of Echus Chasma
The High-Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Echus Chasma, one of the largest water source regions on the Red Planet. Echus Chasma is the source region of Kasei Valles which extends 3000 km to the north. The data was acquired on 25 September 2005. The pictures are centred at about 1° north and 278° east and have a ground resolution of approximately 17 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Echus Chasma, nadir view
The High-Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39° north and 17° east on the planet. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Mamers Valles Perspective View
The High-Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39° north and 17° east on the planet. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Mamers Valles Perspective View
The High-Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39° north and 17° east on the planet. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Crater in Mamers Valles
The High Resolution Stereo Camera on board ESA's Mars Express orbiter imaged Nepenthes Mensae, a river delta on Mars, on 22 January 2008. The data was acquired in the region lying at approximately 3° north and 121° east with a ground resolution of 15 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Perspective View of Nepenthes Mensae
The High Resolution Stereo Camera on board ESA's Mars Express orbiter imaged Nepenthes Mensae, a river delta on Mars, on 22 January 2008. The data was acquired in the region lying at approximately 3° north and 121° east with a ground resolution of 15 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Nepenthes Mensae, Perspective View
The High Resolution Stereo Camera on board ESA's Mars Express orbiter imaged Nepenthes Mensae, a river delta on Mars, on 22 January 2008. The data was acquired in the region lying at approximately 3° north and 121° east with a ground resolution of 15 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Nepenthes Mensae False-Colour Nadir View
The High Resolution Stereo Camera on board ESA's Mars Express orbiter imaged Nepenthes Mensae, a river delta on Mars, on 22 January 2008. The data was acquired in the region lying at approximately 3° north and 121° east with a ground resolution of 15 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Nepenthes Mensae
Perspective view of Hebes Chasma obtained by the High Resolution Stereo Camera (HRSC) on ESA's Mars Express spacecraft. Hebes Chasma is located at approximately 1° south and 282° east. The HRSC obtained image data on 16 September 2005 with a ground resolution of approximately 15 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Hebes Chasma, Perspective View
Perspective view of Hebes Chasma obtained by the High Resolution Stereo Camera (HRSC) on ESA's Mars Express spacecraft. Hebes Chasma is located at approximately 1° south and 282° east. The HRSC obtained image data on 16 September 2005 with a ground resolution of approximately 15 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Hebes Chasma, Perspective View
Perspective view of Hebes Chasma obtained by the High Resolution Stereo Camera (HRSC) on ESA's Mars Express spacecraft. Hebes Chasma is located at approximately 1° south and 282° east. The HRSC obtained image data on 16 September 2005 with a ground resolution of approximately 15 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Hebes Chasma, Perspective View
This is an ortho-image of Hebes Chasma, a trough in the Grand Canyon of Mars. The image is overlaid with elevation data from an HRSC-derived high-resolution digital terrain model (DTM). In an ortho-image, the projecting rays are perpendicular to the plane of projection. This corrects any deformations introduced by an imaging camera. Such an image can be fitted directly on to a map. Hebes Chasma is located at approximately 1° south and 282° east. Image data was obtained on 16 September 2005 with a ground resolution of approximately 15 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Hebes Chasma, Colour-Coded Elevation Model
Hebes Chasma is an enclosed trough, almost 8000 m deep, in Valles Marineris, the Grand Canyon of Mars, where water is believed to have flowed. The High Resolution Stereo Camera (HRSC) on ESA's Mars Express studied the area providing new pictorial clues to its history. Hebes Chasma is located at approximately 1° south and 282° east. Image data was obtained on 16 September 2005 with a ground resolution of approximately 15 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Hebes Chasma
This is an image of Daedalia Planum, located 1000 km south of Arsia Mons, a southern volcano of the Tharsis Montes. The image was taken on 19 July 2005, from a distance of 302 km from the surface. The image is centred at 235.4° east and 26.2° south. The scene spans a width of 100 km and the ground resolution is 25 m/pixel. Credit: ESA/DLR/FU Berlin (G. Neukum).
 
 
Daedalia Planum
Promethei Planum, an area seasonally covered with a layer of ice more than 3500-m thick layer of ice in the martian south polar region, was the subject of the High Resolution Stereo Camera’s (HRSC) focus on 22 September 2005 as Mars Express was in orbit above the Red Planet. Promethei Planum lies at approximately 76° south and 105° east. Credits: ESA/ DLR/ FU Berlin (G. Neukum)
 
 
Promethei Planum Perspective View
Promethei Planum, an area seasonally covered with a layer of ice more than 3500-m thick layer of ice in the martian south polar region, was the subject of the High Resolution Stereo Camera’s (HRSC) focus on 22 September 2005 as Mars Express was in orbit above the Red Planet. Promethei Planum lies at approximately 76° south and 105° east. Credits: ESA/ DLR/ FU Berlin (G. Neukum)
 
 
Promethei Planum Perspective View
Promethei Planum, an area seasonally covered with layer of ice more than 3500 m thick layer of ice in the martian south polar region, was the subject of the High Resolution Stereo Camera’s focus on 22 September 2005 as Mars Express was in orbit above the Red Planet. Promethei Planum lies at approximately 76° south and 105° east. An approximately 100 km-large and 800 m-deep impact crater is visible in the northern part of the image. The crater’s interior is partly covered in ice. In the centre of the image are structures that may have been created by basaltic lava flow from a volcano. This area is covered in ice. The dark dunes towards the bottom of the image are most likely made up of dust originating from this lava flow or volcanic ash. A broad sheet of ice, which is an extension of the south polar ice cap is located south of the lava flow, to the left in the (nadir) image. The steep flanks clearly show white, clean ice. The thickness of the ice is between 900 and 1100 m. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Promethei Planum
Mars Express took snapshots of Candor Chasma, a valley in the northern part of Valles Marineris, as it was in orbit above the region on 6 July 2006. The High Resolution Stereo Camera on the orbiter obtained the data in orbit number 3195, with a ground resolution of approximately 20 m/pixel. Candor Chasma lies at approximately 6° south and 290° east. Credits: ESA/DLR/FU Berlin (G. Neukum).
 
 
Perspective view of Candor Chasma
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