Over the course of 10 separate orbits, the High Resolution Stereo Camera (HRSC) on Mars Express captured image data from the central region of Tiu Vallis, which has been compiled into a mosaic with a resolution of 12.5 metres per pixel. The mosaic extends over 379 kilometres from north to south and 298 kilometres from east to west. It covers a total area of around 113,000 square kilometres, larger than that of the five new German Federal states.Tiu Vallis is one of a number of valley systems known in Martian geology as 'outflow channels', which extend from the central Martian highlands for hundreds of kilometres to the plains of the northern lowland. These valley systems are characterised by flow structures and streamlined buttes and craters such as those in the centre, around which the highly energetic masses of water that carved out these valleys once flowed.Digital terrain models have been generated using image data from the HRSC camera system’s nadir and stereo channels, from which the topography of the surface can be derived. In this image, colours have been allocated to the different elevations in the landscape. It is clear that the Tiu Vallis and the masses of water flowing within it have dug to a depth of between 1500 and 2000 metres into the northern runouts of the Martian highlands. Individual impact craters in the valley floor form striking depressions. They occurred at a time when water no longer flowed here – otherwise they would have been filled with the sediment load being carried along with it.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
Credit: ESA/DLR/FU Berlin (G. Neukum).
Over the course of 10 separate orbits, the High Resolution Stereo Camera (HRSC) on Mars Express captured image data for the central region of Tiu Vallis, which has been compiled into a mosaic with a resolution of 12.5 metres per pixel. The mosaic extends over 379 kilometres from north to south and 298 kilometres from east to west. It covers a total area of around 113,000 square kilometres, larger than that of the five new German Federal states.Tiu Vallis is one of a number of valley systems known in Martian geology as 'outflow channels', which extend from the central Martian highlands for hundreds of kilometres to the plains of the northern lowland. These valley systems are characterised by flow structures and streamlined buttes and craters such as those in the centre, around which the highly energetic masses of water that carved out these valleys once flowed. In the centre of the image we can see a striking example of a 2500-metre-high butte in the central Martian highland, around the longer sides of which masses of water have flowed.This makes it clear that Tiu Vallis and the masses of water flowing within it from south (left) to north have dug down to 2000 metres into the northern runouts of the Martian highlands. Individual impact craters in the valley floor form striking depressions. They occurred at a time when water no longer flowed here – otherwise they would have been filled with the sediment load being carried along with it.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
Over the course of 10 separate orbits, the High Resolution Stereo Camera (HRSC) on Mars Express captured image data for the central region of Tiu Vallis, which has been compiled into a mosaic with a resolution of 12.5 metres per pixel. The mosaic extends over 379 kilometres from north to south and 298 kilometres from east to west. It covers a total area of around 113,000 square kilometres, larger than that of the five new German Federal states.Tiu Vallis is one of a number of valley systems known in Martian geology as 'outflow channels', which extend from the central Martian highlands for hundreds of kilometres to the plains of the northern lowland. These valley systems are characterised by flow structures and streamlined buttes and craters such as those in the centre, around which the highly energetic masses of water that carved out these valleys once flowed. In the centre of the image and in the background, impact craters each 60 kilometres wide can be seen. The crater interiors are deeper than the surrounding floor of the Tiu Vallis.This makes it clear that Tiu Vallis and the masses of water flowing within it from south (left) to north have dug down to 2000 metres into the northern runouts of the Martian highlands. Individual impact craters in the valley floor form striking depressions. They occurred at a time when water no longer flowed here – otherwise they would have been filled with the sediment load being carried along with it.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
Over the course of 10 separate orbits, the High Resolution Stereo Camera (HRSC) on Mars Express captured image data from the central region of Tiu Vallis, which has been compiled into a mosaic with a resolution of 12.5 metres per pixel. The mosaic extends over 379 kilometres from north to south and 298 kilometres from east to west. It covers a total area of around 113,000 square kilometres, larger than that of the five new German Federal states.The Tiu Vallis is one of a number of valley systems known in Martian geology as 'outflow channels', which extend from the central Martian highlands for hundreds of kilometres to the plains of the northern lowland. These valley systems are characterised by flow structures and streamlined buttes and craters, around which the highly energetic masses of water that carved out these valleys once flowed.Digital terrain models have been generated using image data from the HRSC camera system's nadir and stereo channels, from which the topography of the surface can be derived. In this image, colours have been allocated to the different elevations in the landscape. It is clear that the Tiu Vallis and the masses of water flowing within it have dug to a depth of between 1500 and 2000 metres into the northern runouts of the Martian highlands.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
Over the course of 10 separate orbits, the High Resolution Stereo Camera (HRSC) on Mars Express captured image data from the central region of Tiu Vallis, which has been compiled into a mosaic with a resolution of 12.5 metres per pixel. The mosaic extends over 379 kilometres from north to south and 298 kilometres from east to west. It covers a total area of around 113,000 square kilometres, larger than that of the five new German Federal states.The Tiu Vallis is one of a number of valley systems known in Martian geology as 'outflow channels', which extend from the central Martian highlands for hundreds of kilometres to the plains of the northern lowland. These valley systems are characterised by flow structures and streamlined buttes and craters, around which the highly energetic masses of water that carved out these valleys once flowed.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
The High Resolution Stereo Camera (HRSC), on board ESA's Mars Express spacecraft, operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR), captured image data from the Martian valleys Dao and Niger Valles over the course of eight separate orbits. This was then compiled into a vertical overview mosaic with a resolution of 25 metres per pixel. The mosaic extends over 755 kilometres north to south and 770 kilometres east to west, covering a total area of 581,350 square kilometres, roughly the size of the Iberian Peninsula. The valleys are close to the Hesperia Planum volcanic region at latitude 32 degrees south and longitude 93 degrees east, on the imposing edge of the 2000-kilometre-wide Hellas impact basin. In Martian geology, such valley systems are known as ‘outflow channels’. The valleys are up to 40 kilometres wide in some places. The valley heads to the northeast are around 200 metres deeper than the valley outflows shown here. While the northern Dao Vallis is 2400 metres deep at its centre, the southern Niger Vallis has dug almost 1000 metres less into its surroundings. For this reason, the floor of the Niger Vallis exhibits a significantly more chaotic structure. The Niger Vallis is mostly dominated by terraced basin and rupture structures. In the Dao Vallis, a level valley floor with numerous, heavily eroded buttes in the valley interior is visible. The valleys are cut into a region that is still part of the southern slope of the Hadriaca Patera volcano, at the topmost edge of the image. Traces of numerous lava flows and possibly outflow channels can be made out on the surface. The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
The High Resolution Stereo Camera (HRSC), on board ESA's Mars Express spacecraft, operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR), captured image data from the Martian valleys Dao and Niger Valles over the course of eight separate orbits. This was then compiled into a vertical overview mosaic with a resolution of 25 metres per pixel. The mosaic extends over 755 kilometres north to south and 770 kilometres east to west covering a total area of 581,350 square kilometres, roughly the size of the Iberian Peninsula. A digital terrain model showing a perspective view of the region was generated using stereo image data. The valleys are close to the Hesperia Planum volcanic region at latitude 32 degrees south and longitude 93 degrees east, on the imposing edge of the 2000 kilometre-wide Hellas impact basin. In Martian geology, such valley systems are known as 'outflow channels'. The valleys are up to 40 kilometres wide in some places. The valley heads to the northeast are around 200 metres deeper than the valley outflows shown here. While the northern Dao Vallis is 2400 metres deep at its centre, the southern Niger Vallis has dug almost 1000 metres less into its surroundings. For this reason, the floor of the Niger Vallis exhibits a significantly more chaotic structure. The Niger Vallis is mostly dominated by terraced basin and rupture structures. In the Dao Vallis, a level valley floor with numerous, heavily eroded buttes in the valley interior is visible. The valleys are cut into a region that is still part of the southern slope of the Hadriaca Patera volcano, at the topmost edge of the image. Traces of numerous lava flows and possibly outflow channels can be made out on the surface. The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
The High Resolution Stereo Camera (HRSC), on board ESA's Mars Express spacecraft, operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR), captured image data from the Martian valleys Dao and Niger Valles over the course of eight separate orbits. This was then compiled into a vertical overview mosaic with a resolution of 25 metres per pixel. The mosaic extends over 755 kilometres north to south and 770 kilometres east to west covering a total area of 581,350 square kilometres, roughly the size of the Iberian peninsula. This digital terrain model has been derived from stereo image data in which different colours have been allocated to the elevation values.The valleys are close to the Hesperia Planum volcanic region at latitude 32 degrees south and longitude 93 degrees east, on the imposing edge of the 2000 kilometre-wide Hellas impact basin. In Martian geology, such valley systems are known as 'outflow channels'. The valleys are up to 40 kilometres wide in some places. The valley heads to the northeast are around 200 metres deeper than the valley outflows shown here. While the northern Dao Vallis is 2400 metres deep at its centre, the southern Niger Vallis has dug almost 1000 metres less into its surroundings. For this reason, the floor of the Niger Vallis exhibits a significantly more chaotic structure. The Niger Vallis is mostly dominated by terraced basin and rupture structures. In the Dao Vallis, a level valley floor with numerous, heavily eroded buttes in the valley interior is visible. The valleys are cut into a region that is still part of the southern slope of the Hadriaca Patera volcano, at the topmost edge of the image. Traces of numerous lava flows and possibly outflow channels can be made out on the surface. The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
The image shows a vertical (orthographic) view of a 162 kilometre-wide section of the northern slopes of Coprates Chasma, the eastern part of the Valles Marineris canyon system. The vertical relief from the valley floor to the top edge of the terrain is 9.92 kilometres.The image data used for this view was captured during three Mars Express orbits - 2028, 2039 and 3195. The resolution of the image data in the nadir channel – the highest resolution the HRSC camera system can deliver – is 12.5 metres per pixel. The digital terrain model derived from the stereo image data has a resolution of 50 metres per second. The image output shown here was created at the Department of Planetary Sciences and Remote Sensing, Institute for Geological Sciences, at the Freie Universität Berlin. The image and DTM processing were carried out by B. Schreiner, A. Dumke and D. Neu.Coprates Chasma is the name of the eastern section (over 1000 kilometres long) of the main central valley of the Valles Marineris, the largest canyon system on Mars. The vast structure is thought to have resulted from the Tharsis bulge – several thousand metres high and about four thousand kilometres long to the west of the Valles Marineris – which created such great stress in the Martian highland that the Martian crust ended up rupturing. Another theory is that large volumes of water or ice melt water may have removed rocky material from the substrata, causing the surface to cave in. It is possible that both processes were at work.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This perspective colour anaglyph provides an unusual view of the northern slopes of Coprates Chasma in the eastern part of the Valles Marineris canyon system. The region shown here extends over 162 kilometres and has a vertical relief of 9.92 kilometres. Besides the digital terrain model (DTM) with a resolution of 50 metres, a section of the larger Valles Marineris HRSC DGM with a resolution of 100 metres per pixel was used for the oblique view. The image output shown here was created at the Department of Planetary Sciences and Remote Sensing, Institute for Geological Sciences, at the Freie Universität Berlin. The image and DTM processing were carried out by B. Schreiner, A. Dumke and D. Neu.Coprates Chasma is the name of the eastern section (over 1000 kilometres long) of the main central valley of the Valles Marineris, the largest canyon system on Mars. The vast structure is thought to have resulted from the Tharsis bulge – several thousand metres high and about four thousand kilometres long to the west of the Valles Marineris – which created such great stress in the Martian highland that the Martian crust ended up rupturing. Another theory is that large volumes of water or ice melt water may have removed rocky material from the substrata, causing the surface to cave in. It is possible that both processes were at work.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This image shows a section approximately 240 by 100 kilometres wide of the Aeolis Mensae region, located at the transition from the southern highlands to the northern lowlands. Due to the sharp contrast in the shapes of the landscapes, this transition is also known as the 'dichotomy boundary'. Tectonic structures, isolated buttes and floe-like, fissured massifs can be seen in the image. The landscape has been sculpted by wind activity. Several yardangs – rocky ridges streamlined to several kilometres in length and separated from each other by ‘wind channels’ – have been created by wind erosion. The yardangs are mostly visible in the northwest (top right), but also occur in isolation in the region of intensive tectonic stress in the left half of the image.The image data was captured on 2 August 2010 by the HRSC camera system on board ESA's Mars Express spacecraft during orbit 8425. The centre of the image is at latitude 7 degrees south and longitude 152 degrees east. The resolution is about 21 metres per pixel.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This image shows a section approximately 240 by 100 kilometres wide of the Aeolis Mensae region, located at the transition from the southern highlands to the northern lowlands. Due to the sharp contrast in the shapes of the landscapes, this transition is also known as the 'dichotomy boundary'. This digital terrain model is based on stereo image data. The legend on the top right associates colours with elevation. Tectonic structures, isolated buttes and floe-like, fissured massifs can be seen in the image. The landscape has been sculpted by wind activity. Several yardangs – rocky ridges streamlined to several kilometres in length and separated from each other by 'wind channels' – have been created by wind erosion. The yardangs are mostly visible in the northwest (top right), but also occur in isolation in the region of intensive tectonic stress in the left half of the image.The image data was captured on 2 August 2010 by the HRSC camera system on board the ESA Mars Express spacecraft during orbit 8425. The centre of the image is at latitude 7 degrees south and longitude 152 degrees east. The resolution is about 21 metres per pixel.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This image from the High Resolution Stereo Camera (HRSC), carried on board ESA's Mars Express spacecraft and operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR) shows Gale Crater, situated at latitude 5.4 degrees south and longitude 137.9 degrees east. NASA's Mars Science Laboratory (MSL), with its rover Curiosity, which was launched on 26 November 2011, is scheduled to land in the northern part of Gale Crater in August 2012. The aim of the MSL mission, besides geological and mineralogical research, is to search for possible forms of life or habitats on Mars.Gale Crater has a diameter of 154 kilometres. The conspicuous central peak in the crater stands 5.5 kilometres above the crater floor and consists, in part, of sedimentary layers. Hydrated sulphates such as gypsum or kieserite and phyllosilicates (clays) can be identified from orbit using the spectrometers on board Mars Express. They are evidence that standing water might once have been found in Gale Crater. This crater was selected due to the abundance of different minerals and the relatively good accessibility of the outcrops.Images from orbits 5273 and 1916 were combined to create this image mosaic. It has a resolution of 22 metres per pixel. The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This image from the High Resolution Stereo Camera (HRSC), carried on board ESA's Mars Express spacecraft and operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR) shows Gale Crater, situated at latitude 5.4 degrees south and longitude 137.9 degrees east. This image is a colour-coded illustrated map based on a digital terrain model derived from stereo image data. Different colours are used for the elevation information; the legend in the upper right can be used to see the elevations to which the colours have been allocated.NASA's Mars Science Laboratory (MSL), with its rover Curiosity, which was launched on 26 November 2011, is scheduled to land in the northern part of Gale Crater – in the depression shown in blue in the right third of the image – in August 2012. The aim of the MSL mission, besides geological and mineralogical research, is to search for possible forms of life or habitats on Mars.Gale Crater has a diameter of 154 kilometres. The conspicuous central peak in the crater stands 5.5 kilometres above the crater floor and consists, in part, of sedimentary layers. Hydrated sulphates such as gypsum or kieserite and phyllosilicates (clays) can be identified from orbit using the spectrometers on board Mars Express. They are evidence that standing water might once have been found in Gale Crater. This crater was selected due to the abundance of different minerals and the relatively good accessibility of the outcrops.Images from orbits 5273 and 1916 were combined to create this image mosaic. It has a resolution of 100 metres per pixel.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This image from the High Resolution Stereo Camera (HRSC), carried on board ESA's Mars Express spacecraft and operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR) shows a view from the northeast of Gale Crater, situated at latitude 5.4 degrees south and longitude 137.9 degrees east. This image is a colour-coded perspective view based on a digital terrain model derived from stereo image data. Different colours are used for the elevation information; the legend in the upper right can be used to see the elevations to which the colours have been allocated.NASA's Mars Science Laboratory (MSL), with its rover Curiosity, which was launched on 26 November 2011, is scheduled to land in the northern part of Gale Crater – in the depression shown in blue in the right third of the image – in August 2012. The aim of the MSL mission, besides geological and mineralogical research, is to search for possible forms of life or habitats on Mars.Gale Crater has a diameter of 154 kilometres. The conspicuous central peak in the crater stands 5.5 kilometres above the crater floor and consists, in part, of sedimentary layers. Hydrated sulphates such as gypsum or kieserite and phyllosilicates (clays) can be identified from orbit using the spectrometers on board Mars Express. They are evidence that standing water might once have been found in Gale Crater. This crater was selected due to the abundance of different minerals and the relatively good accessibility of the outcrops.Images from orbits 5273 and 1916 were combined to create this image mosaic. It has a resolution of 100 metres per pixel.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This image from the High Resolution Stereo Camera (HRSC), carried on board ESA's Mars Express spacecraft and operated by the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt; DLR) shows a view from the northeast of Gale Crater, situated at latitude 5.4 degrees south and longitude 137.9 degrees east. This image is a colour-coded perspective view based on a digital terrain model derived from stereo image data. NASA's Mars Science Laboratory (MSL), with its rover Curiosity, which was launched on 26 November 2011, is scheduled to land in the northern part of Gale Crater – in the depression shown in blue in the right third of the image – in August 2012. The aim of the MSL mission, besides geological and mineralogical research, is to search for possible forms of life or habitats on Mars.Gale Crater has a diameter of 154 kilometres. The conspicuous central peak in the crater stands 5.5 kilometres above the crater floor and consists, in part, of sedimentary layers. Hydrated sulphates such as gypsum or kieserite and phyllosilicates (clays) can be identified from orbit using the spectrometers on board Mars Express. They are evidence that standing water might once have been found in Gale Crater. This crater was selected due to the abundance of different minerals and the relatively good accessibility of the outcrops.Images from orbits 5273 and 1916 were combined to create this image mosaic. It has a resolution of 100 metres per pixel.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This perspective image shows a view of the Elysium volcanic province from the northeast. The picture is based on an image mosaic computed from 12 HRSC nadir images (a channel in the camera system directed vertically onto the surface of Mars and yielding the highest resolution), with a resolution of 25 metres per pixel, and the associated stereo image data for deriving a digital terrain model. The picture is a colour-coded perspective view. Different colours are used for the elevation information; the lowest lying areas are shown in blue and the highest points of the volcano in light beige.Elysium is the second largest volcanic province on Mars. It consists of three volcanic complexes - Elysium Mons (on the right in the background), Albor Tholus (on the left at the back) and Hecates Tholus (in the foreground). The section of the volcanic region shown here extends for about 10 degrees of longitude in an east-west direction and 20 degrees of latitude in a north-south direction. Overall, the volcanic deposits cover an area of around 3.4 million square kilometres - almost 10 times the size of Germany. Elysium Mons is the highest volcano in this region, standing 17.7 kilometres above the western plain. The Elysium volcanic province has been active for over four billion years; elevation in this perspective oblique view is exaggerated by a factor of three.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This perspective image shows a view of the central part of the Elysium volcanic province from the southeast. The picture is based on an image mosaic computed from 12 HRSC nadir images (a channel in the camera system directed vertically onto the surface of Mars and yielding the highest resolution), with a resolution of 25 metres per pixel, and the associated stereo image data for deriving a digital terrain model. The picture is a colour-coded perspective view. Different colours are used for the elevation information: the lowest lying areas are shown in blue and the highest points of the volcano in light beige.Elysium is the second largest volcanic province on Mars. It consists of three volcanic complexes - Elysium Mons (on the right in the background), Albor Tholus (on the left at the back) and Hecates Tholus (in the foreground). Overall, the volcanic deposits cover an area of around 3.4 million square kilometres - almost 10 times the size of Germany. Elysium Mons is the highest volcano in this region, standing 17.7 kilometres above the western plain. The Elysium volcanic province has been active for over four billion years; elevation in this perspective oblique view is exaggerated by a factor of three.The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
This overhead view shows the Elysium volcanic province. The image is a colour-coded perspective view. The picture is based on an image mosaic computed from 12 HRSC nadir images (a channel in the camera system directed vertically onto the surface of Mars and yielding the highest resolution), with a resolution of 25 metres per pixel, and the associated stereo image data for deriving a digital terrain model. The picture is a colour-coded perspective view. Different colours are used for the elevation information: the lowest lying areas are shown in blue and the highest points of the volcano in light beige.Elysium is the second largest volcanic province on Mars. It consists of three volcanic complexes - Elysium Mons (left), Albor Tholus (bottom) and Hecates Tholus (top). The section of the volcanic region shown here extends for about 10 degrees of longitude in an east-west direction and for 20 degrees of latitude in a north-south direction. Overall the volcanic deposits cover an area of around 3.4 million square kilometres - stretching beyond the mosaic shown here. It is almost 10 times the size of Germany. Elysium Mons is the highest volcano in this region, standing 17.7 kilometres above the western plain. The Elysium volcanic province has been active for over four billion years:The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.