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Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. Close-up of a large impact crater measuring 20 km in diameter. The image was obtained by the Mars Express probe on December 28, 2007. This image of Hephaestus Fossae was obtained by Esa's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21* North and 126* East on the Red Planet. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region. The image shows a large impact crater measuring 20 km in diameter. It shows a blanket of ejecta with flow forms surrounding the rim

Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. Close-up of a large impact crater measuring 20 km in diameter. The image was obtained by the Mars Express probe on December 28, 2007. This image of Hephaestus Fossae was obtained by Esa's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21* North and 126* East on the Red Planet. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region. The image shows a large impact crater measuring 20 km in diameter. It shows a blanket of ejecta with flow forms surrounding the rim

PIX4616168

Mars - Phobos satellite - Martian moon Phobos - View of the Phobos satellite above the Mars blade obtained by the Mars Express probe on 22 January 2007. An image of Phobos by the High - Resolution Stereo Camera on board Mars Express on 22 January 2007. The larger and inner of the two martian moons is seen here floating just above the martian limb. The image has been enhanced slightly to bring out the detail on the moon

Mars - Phobos satellite - Martian moon Phobos - View of the Phobos satellite above the Mars blade obtained by the Mars Express probe on 22 January 2007. An image of Phobos by the High - Resolution Stereo Camera on board Mars Express on 22 January 2007. The larger and inner of the two martian moons is seen here floating just above the martian limb. The image has been enhanced slightly to bring out the detail on the moon

PIX4616246

Mars: shadow of Phobos - Shadow of moon Phobos on martian surface - View of the shadow of Phobos satellite on Mars. Image obtained by the Mars Express probe on November 10, 2005. Recolorated image. On 10 November 2005, the camera experiment on Mars Express, the High Resolution Stereo Camera, obtained images of the shadow of the Martian moon Phobos as it moved across the surface. The shadow of Phobos has an elliptical shape on the Martian surface, because the shadow's cone hits the surface under an oblique angle

Mars: shadow of Phobos - Shadow of moon Phobos on martian surface - View of the shadow of Phobos satellite on Mars. Image obtained by the Mars Express probe on November 10, 2005. Recolorated image. On 10 November 2005, the camera experiment on Mars Express, the High Resolution Stereo Camera, obtained images of the shadow of the Martian moon Phobos as it moved across the surface. The shadow of Phobos has an elliptical shape on the Martian surface, because the shadow's cone hits the surface under an oblique angle

PIX4616032

Mars: Noctis Labyrinthus - Mars: Noctis Labyrinthus - Perspective view of Noctis Labyrinthus, located in the western part of the great Martian canyon Valles Marineris. This heavily eroded canyon is here 5000 meters deep. Image obtained by the Mars Express probe on June 25, 2006. On 25 June 2006 the High - Resolution Stereo Camera (HRSC), onboard the ESA spacecraft Mars Express obtained image data with a ground resolution of approximately 16 meters per pixel. The data were acquired in the region of Noctis Labyrinthus at approximately 6.5* southern latitude and 260* eastern longitude. The region Noctis Labyrinthus, the Labyrinth of the Night”” is located directly on the western edge of Valles Marineris, the “Grand Canyon of Mars””. It is part of the complex graben system which is associated with the up - arching of Tharsis. Eye - catching is the high density of deeply incised, smaller, maze - like fractures. The scene exhibits parts of those graben structures which are incised up to 5000

Mars: Noctis Labyrinthus - Mars: Noctis Labyrinthus - Perspective view of Noctis Labyrinthus, located in the western part of the great Martian canyon Valles Marineris. This heavily eroded canyon is here 5000 meters deep. Image obtained by the Mars Express probe on June 25, 2006. On 25 June 2006 the High - Resolution Stereo Camera (HRSC), onboard the ESA spacecraft Mars Express obtained image data with a ground resolution of approximately 16 meters per pixel. The data were acquired in the region of Noctis Labyrinthus at approximately 6.5* southern latitude and 260* eastern longitude. The region Noctis Labyrinthus, the Labyrinth of the Night”” is located directly on the western edge of Valles Marineris, the “Grand Canyon of Mars””. It is part of the complex graben system which is associated with the up - arching of Tharsis. Eye - catching is the high density of deeply incised, smaller, maze - like fractures. The scene exhibits parts of those graben structures which are incised up to 5000

PIX4616056

March: Hebes Chasma - Hebes Chasma is a basin of almost 8000 m deep located in the northern part of Valles Marineris, the great Martian canyon. At the centre of this depression is a stratified plateau that constitutes sedimentary deposits. Perspective image obtained by the Mars Express probe in 2005. Perspective view of Hebes Chasma obtained by the High Resolution Stereo Camera (HRSC) on ESA's Mars Express spacecraft. 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. 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

March: Hebes Chasma - Hebes Chasma is a basin of almost 8000 m deep located in the northern part of Valles Marineris, the great Martian canyon. At the centre of this depression is a stratified plateau that constitutes sedimentary deposits. Perspective image obtained by the Mars Express probe in 2005. Perspective view of Hebes Chasma obtained by the High Resolution Stereo Camera (HRSC) on ESA's Mars Express spacecraft. 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. 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

PIX4616076

Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The darker area could be caused by local erosion or wind-driven material. 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. The valley of Mamers Valles is approximately

Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The darker area could be caused by local erosion or wind-driven material. 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. The valley of Mamers Valles is approximately

PIX4616090

March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible to the right (north). It is partially covered with ice. In the center of the image, structures formed by lava flows; on the left of the image, ice, which is an extension of the southern polar cap. 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 interio

March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible to the right (north). It is partially covered with ice. In the center of the image, structures formed by lava flows; on the left of the image, ice, which is an extension of the southern polar cap. 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 interio

PIX4616118

March: Echus Chasma - Mars: Echus Chasma - Echus Chasma is a valley located north of Valles Marineris. It is about 100 km long and 10 km wide. Detail obtained by the Mars Express probe in September 2005. The High - Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Etus 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

March: Echus Chasma - Mars: Echus Chasma - Echus Chasma is a valley located north of Valles Marineris. It is about 100 km long and 10 km wide. Detail obtained by the Mars Express probe in September 2005. The High - Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Etus 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

PIX4616128

March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this perspective image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible at the bottom of the image. It is partially covered with ice. On top, structures formed by lava flows; at the top of the picture, ice, which is an extension of the southern polar cap. 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 bottom of the image. The crater's interior is par

March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this perspective image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible at the bottom of the image. It is partially covered with ice. On top, structures formed by lava flows; at the top of the picture, ice, which is an extension of the southern polar cap. 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 bottom of the image. The crater's interior is par

PIX4616138

Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater at the top of the picture is 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. This image of Hephaestus Fossae was obtained by Esa's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21* North and 126* East on the Red Planet. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region. The surface is mostly smooth, and is covered by several small impact craters measuring 800 to 2800 m in diameter. Smaller craters are scattered across the entire region. A larger impact crater measuring 20 km in diameter is a prominent f

Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater at the top of the picture is 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. This image of Hephaestus Fossae was obtained by Esa's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21* North and 126* East on the Red Planet. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region. The surface is mostly smooth, and is covered by several small impact craters measuring 800 to 2800 m in diameter. Smaller craters are scattered across the entire region. A larger impact crater measuring 20 km in diameter is a prominent f

PIX4616151

Mars - Satellite Phobos - Martian moon Phobos - View of the satellite Phobos obtained by the Mars Express probe on January 9, 2011, at a distance of 100 km from the satellite. The south pole is indicated. Mars Express took this image of the surface of the moon Phobos on January 9, 2011. Mars Express passed Mars' largest moon at a distance of 100 km. South pole is indicated

Mars - Satellite Phobos - Martian moon Phobos - View of the satellite Phobos obtained by the Mars Express probe on January 9, 2011, at a distance of 100 km from the satellite. The south pole is indicated. Mars Express took this image of the surface of the moon Phobos on January 9, 2011. Mars Express passed Mars' largest moon at a distance of 100 km. South pole is indicated

PIX4616339

March: Rull Vallis Canal. - Rull Vallis Canal east of Hellas Basin. We think water was flowing there once. The area photographed is 100 km wide. Image obtained by the Mars Express probe on 15 January 2004 at an altitude of 273 km

March: Rull Vallis Canal. - Rull Vallis Canal east of Hellas Basin. We think water was flowing there once. The area photographed is 100 km wide. Image obtained by the Mars Express probe on 15 January 2004 at an altitude of 273 km

PIX4615872

March: Olympus Mons Volcano Summit - This volcano has a diameter of 600 km and rises to 27 km. Its caldera view here has a depth of 3000m. Image obtained by the Mars Express probe at an altitude of 273 km on January 21, 2004

March: Olympus Mons Volcano Summit - This volcano has a diameter of 600 km and rises to 27 km. Its caldera view here has a depth of 3000m. Image obtained by the Mars Express probe at an altitude of 273 km on January 21, 2004

PIX4615905

Mars: Cratere Nicholson by Mars Express - Perspective view of a hill 55 km long by 37 km wide and 3500 m high located in the centre of an impact crater

Mars: Cratere Nicholson by Mars Express - Perspective view of a hill 55 km long by 37 km wide and 3500 m high located in the centre of an impact crater

PIX4615961

March: Caldera of the volcano Apollinaris Patera - This Martian volcano is 180 to 280 km from its base and rises at about 5000 m altitude. Its caldera seen here by the Mars Express probe on October 26, 2004 measures 80 km in diameter and a depth of 1 km. Faux Color Image

March: Caldera of the volcano Apollinaris Patera - This Martian volcano is 180 to 280 km from its base and rises at about 5000 m altitude. Its caldera seen here by the Mars Express probe on October 26, 2004 measures 80 km in diameter and a depth of 1 km. Faux Color Image

PIX4615989

Mars: Martian face in the region of Cydonia - Perspective view of the massif obtained by the Mars Express probe on July 22, 2006

Mars: Martian face in the region of Cydonia - Perspective view of the massif obtained by the Mars Express probe on July 22, 2006

PIX4616025

March: Iani Chaos - Mars: Iani Chaos - The region of Iani Chaos on Mars. Image obtained by the Mars Express probe. Iani Chaos on Mars, an area where Light Toned Deposits, or LTD, are known to be present. An analysis of data and images from Mars Express suggests that several LTD, some of the least understood structures on Mars, were formed when large amounts of groundwater burst on to the surface. Scientists propose that groundwater had a greater role in shaping the martian surface than previously believed, and may have sheltered primitive life forms as the planet started drying up. This image was obtained with the High Resolution Stereo Camera on board ESA's Mars Express spacecraft

March: Iani Chaos - Mars: Iani Chaos - The region of Iani Chaos on Mars. Image obtained by the Mars Express probe. Iani Chaos on Mars, an area where Light Toned Deposits, or LTD, are known to be present. An analysis of data and images from Mars Express suggests that several LTD, some of the least understood structures on Mars, were formed when large amounts of groundwater burst on to the surface. Scientists propose that groundwater had a greater role in shaping the martian surface than previously believed, and may have sheltered primitive life forms as the planet started drying up. This image was obtained with the High Resolution Stereo Camera on board ESA's Mars Express spacecraft

PIX4616054

March: chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles and Sacra Fossae. To the north, the large impact crater is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The image shows an old 35 km - diameter impact crater in the north. The crater's southwestern rim is eroded strongly, mostly by flowing water. The source of the water was located in Etus Chasma, which lies about 850 km to the southwest. The crater floor and the northwestern part are remarkably flat, formed by sediments and basaltic lava fl

March: chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles and Sacra Fossae. To the north, the large impact crater is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The image shows an old 35 km - diameter impact crater in the north. The crater's southwestern rim is eroded strongly, mostly by flowing water. The source of the water was located in Etus Chasma, which lies about 850 km to the southwest. The crater floor and the northwestern part are remarkably flat, formed by sediments and basaltic lava fl

PIX4616176

March: Volcano Olympus Mons - False colors - Mars: volcano Olympus Mons - Altimetric data obtained by the Mars Express probe. The Olympus Mons volcano is 600 km in diameter and 26 km above the plains. This is a mosaic of Olympus Mons, the highest volcano on Mars, which towers 26 km above the surrounding plains. The image covers an area of approximately 600,000 sq km and is color - coded according to height

March: Volcano Olympus Mons - False colors - Mars: volcano Olympus Mons - Altimetric data obtained by the Mars Express probe. The Olympus Mons volcano is 600 km in diameter and 26 km above the plains. This is a mosaic of Olympus Mons, the highest volcano on Mars, which towers 26 km above the surrounding plains. The image covers an area of approximately 600,000 sq km and is color - coded according to height

PIX4615892

March: Summit of Hecates Tholus Volcano - This volcano north of Elysium rises at 5300m. Its caldera view here has a depth of 600m. Image obtained by the Mars Express probe at an altitude of 275 km on January 19, 2004

March: Summit of Hecates Tholus Volcano - This volcano north of Elysium rises at 5300m. Its caldera view here has a depth of 600m. Image obtained by the Mars Express probe at an altitude of 275 km on January 19, 2004

PIX4615898

March: Impact crater and dunes - View of a 12 km by 7 km dune field at the bottom of an impact crater located in Argyre Planitia

March: Impact crater and dunes - View of a 12 km by 7 km dune field at the bottom of an impact crater located in Argyre Planitia

PIX4615918

March: Faults and impact crater in Acheron Fossae. - Fracture system around a 55 km diametre and 2000m deep impact crater. Image obtained by the Mars Express probe in 2004

March: Faults and impact crater in Acheron Fossae. - Fracture system around a 55 km diametre and 2000m deep impact crater. Image obtained by the Mars Express probe in 2004

PIX4615921

March: Cratere Nicholson - Mars: Cratere Nicholson - View of a hill 55 km long by 37 km wide and 3500 m high located in the centre of an impact crater. The Nicholson crater is 100 km in diameter and is located south of Amazonis Planitia. Image obtained by the Mars Express probe on November 27, 2004

March: Cratere Nicholson - Mars: Cratere Nicholson - View of a hill 55 km long by 37 km wide and 3500 m high located in the centre of an impact crater. The Nicholson crater is 100 km in diameter and is located south of Amazonis Planitia. Image obtained by the Mars Express probe on November 27, 2004

PIX4615953

March: impact crater Maunder - Mars: Maunder crater - Perspective view of an impact crater located between Argyre Planitia and Hellas Planitia. The Maunder crater is 90 km in diameter and 900 m deep. The dark areas at the bottom of the crater are dunes. Image obtained by the Mars Express probe in 2005. On 29 November and 14 December 2005 the High - Resolution Stereo Camera (HRSC), onboard the ESA spacecraft Mars Express obtained image data with a ground resolution of approximately 15 meters per pixel. The data were acquired in the region of Noachis Terra at approximately 50* southern latitude and 2* eastern longitude. The Maunder Crater, located halfway between Argyre Planitia and Hellas Planitia on the southern Highlands of Mars, has a diameter of 90 kilometers and a current depth of barely 900 meters. In the east, the crater floor is bounded by an approximately 700 meters deep trough. It may be associated with the landslide on the western edge of the crater. Some gullies formed on th

March: impact crater Maunder - Mars: Maunder crater - Perspective view of an impact crater located between Argyre Planitia and Hellas Planitia. The Maunder crater is 90 km in diameter and 900 m deep. The dark areas at the bottom of the crater are dunes. Image obtained by the Mars Express probe in 2005. On 29 November and 14 December 2005 the High - Resolution Stereo Camera (HRSC), onboard the ESA spacecraft Mars Express obtained image data with a ground resolution of approximately 15 meters per pixel. The data were acquired in the region of Noachis Terra at approximately 50* southern latitude and 2* eastern longitude. The Maunder Crater, located halfway between Argyre Planitia and Hellas Planitia on the southern Highlands of Mars, has a diameter of 90 kilometers and a current depth of barely 900 meters. In the east, the crater floor is bounded by an approximately 700 meters deep trough. It may be associated with the landslide on the western edge of the crater. Some gullies formed on th

PIX4615975

Mars: Martian face in the region of Cydonia - The “face” is visible in the center of the image. Image obtained by the Mars Express probe on July 22, 2006. The resolution is 13.7m per pixel

Mars: Martian face in the region of Cydonia - The “face” is visible in the center of the image. Image obtained by the Mars Express probe on July 22, 2006. The resolution is 13.7m per pixel

PIX4615998

March: Caldera of the volcano Apollinaris Patera - This Martian volcano is 180 to 280 km from its base and rises at about 5000 m altitude. Its caldera seen here by the Mars Express probe on October 26, 2004 measures 80 km in diameter and a depth of 1 km

March: Caldera of the volcano Apollinaris Patera - This Martian volcano is 180 to 280 km from its base and rises at about 5000 m altitude. Its caldera seen here by the Mars Express probe on October 26, 2004 measures 80 km in diameter and a depth of 1 km

PIX4616015

March: the region of Cydonia - Perspective view of the “pyramids””. Image obtained by the Mars Express probe on July 22, 2006. The resolution is 13.7m per pixel

March: the region of Cydonia - Perspective view of the “pyramids””. Image obtained by the Mars Express probe on July 22, 2006. The resolution is 13.7m per pixel

PIX4616030

Mars: faults in Claritas Fossae. - Mars: fractures in Claritas Fossae - Fracture system in Claritas Fossae, a region south of the Tharsis volcanoes. These fractures, ranging from a few kilometres to a hundred kilometres, are probably associated with the tectonic activity that led to elevation of the Tharsis plateau. Perspective image obtained by the Mars Express probe in 2004. On 29 June 2004 the High Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained image data in orbit 563 with a ground resolution of approximately 62 metres per pixel. The images cover Claritas Fossae at approximately 25* southern latitude and 253* eastern longitude. Claritas Fossae is located on the Tharsis rise, south of the three large volcanoes known as the Tharsis Montes, and extends roughly north to south for approximately 1800 km. Claritas Fossae, which is composed of a series of linear fractures with widths ranging from a few kilometres to 100 km, is roughly 150 km wide in the nor

Mars: faults in Claritas Fossae. - Mars: fractures in Claritas Fossae - Fracture system in Claritas Fossae, a region south of the Tharsis volcanoes. These fractures, ranging from a few kilometres to a hundred kilometres, are probably associated with the tectonic activity that led to elevation of the Tharsis plateau. Perspective image obtained by the Mars Express probe in 2004. On 29 June 2004 the High Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained image data in orbit 563 with a ground resolution of approximately 62 metres per pixel. The images cover Claritas Fossae at approximately 25* southern latitude and 253* eastern longitude. Claritas Fossae is located on the Tharsis rise, south of the three large volcanoes known as the Tharsis Montes, and extends roughly north to south for approximately 1800 km. Claritas Fossae, which is composed of a series of linear fractures with widths ranging from a few kilometres to 100 km, is roughly 150 km wide in the nor

PIX4616037

Mars: Valles Marineris - Mosaic of 20 images obtained by the European probe Mars Express. This image shows the eastern part of Valles Marineris, a canyon about 4500 km long and 8 km deep. This mosaic image of eastern part of Valles Marineris - colored to resemble the martian surface - comes from Esa's Mars Express spacecraft, which repeatedly crosses the Martian equator from north to south or south to north. The High Resolution Stereo Camera (HRSC) on board Mars Express, has been taking image strips of the valley system since 2004 as it passes overhead. The individual HRSC image strips are each between 50 and 200 kilometers wide, depending on Mars Express' orbit, so this view of Valles Marineris has only been made possible by creating a mosaic using 20 separate images. To improve the presentation here, the altitudes have been exaggerated fourfold, so that the slopes and mountainsides appear steeper than they are in reality. The colours in this image are slightly false as well. By incre

Mars: Valles Marineris - Mosaic of 20 images obtained by the European probe Mars Express. This image shows the eastern part of Valles Marineris, a canyon about 4500 km long and 8 km deep. This mosaic image of eastern part of Valles Marineris - colored to resemble the martian surface - comes from Esa's Mars Express spacecraft, which repeatedly crosses the Martian equator from north to south or south to north. The High Resolution Stereo Camera (HRSC) on board Mars Express, has been taking image strips of the valley system since 2004 as it passes overhead. The individual HRSC image strips are each between 50 and 200 kilometers wide, depending on Mars Express' orbit, so this view of Valles Marineris has only been made possible by creating a mosaic using 20 separate images. To improve the presentation here, the altitudes have been exaggerated fourfold, so that the slopes and mountainsides appear steeper than they are in reality. The colours in this image are slightly false as well. By incre

PIX4616253

Mars - Phobos Satellite - Martian moon Phobos - View of the Phobos satellite obtained by the Mars Express probe in March 2010. The north pole is indicated. Mars Express took this image of the surface of the moon Phobos in March 2010. The resolution is about 9 m/pixel

Mars - Phobos Satellite - Martian moon Phobos - View of the Phobos satellite obtained by the Mars Express probe in March 2010. The north pole is indicated. Mars Express took this image of the surface of the moon Phobos in March 2010. The resolution is about 9 m/pixel

PIX4616274

Mars - Phobos Satellite - Martian moon Phobos - View of the Phobos satellite obtained by the Mars Express probe on March 7, 2010. The resolution is 4.4 meters per pixel. Mars Express took this image of the surface of the moon Phobos on 7 March 2010. The resolution is about 4.4 m/pixel

Mars - Phobos Satellite - Martian moon Phobos - View of the Phobos satellite obtained by the Mars Express probe on March 7, 2010. The resolution is 4.4 meters per pixel. Mars Express took this image of the surface of the moon Phobos on 7 March 2010. The resolution is about 4.4 m/pixel

PIX4616280

March: Echus Chasma - Mars: Echus Chasma - Echus Chasma is a valley located north of Valles Marineris. It is about 100 km long and 10 km wide. Image obtained by the Mars Express probe in September 2005. The High - Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Etus Chasma, one of the largest water source regions on the Red Planet. Echus Chasma is an approximately 100 km long and 10 km wide incision in the Lunae Planum high plateau north of Valles Marineris, the 'Grand Canyon' of Mars. Etus Chasma is the water source region of Kasei Valles, which extends thousands of kilometres to the north, and its southern - most part. 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

March: Echus Chasma - Mars: Echus Chasma - Echus Chasma is a valley located north of Valles Marineris. It is about 100 km long and 10 km wide. Image obtained by the Mars Express probe in September 2005. The High - Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Etus Chasma, one of the largest water source regions on the Red Planet. Echus Chasma is an approximately 100 km long and 10 km wide incision in the Lunae Planum high plateau north of Valles Marineris, the 'Grand Canyon' of Mars. Etus Chasma is the water source region of Kasei Valles, which extends thousands of kilometres to the north, and its southern - most part. 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

PIX4616094

March: Echus Chasma - Mars: Echus Chasma - Echus Chasma is a valley located north of Valles Marineris. It is about 100 km long and 10 km wide. Detail obtained by the Mars Express probe in September 2005. The High - Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Etus 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

March: Echus Chasma - Mars: Echus Chasma - Echus Chasma is a valley located north of Valles Marineris. It is about 100 km long and 10 km wide. Detail obtained by the Mars Express probe in September 2005. The High - Resolution Stereo Camera (HRSC) on board ESA's Mars Express has returned images of Etus 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

PIX4616125

March: Chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles (top) and Sacra Fossae (bottom). Kasei Valles is one of the largest Martian canal systems. The large impact crater on the right is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The upper portion of the image swath shows the eastern margin of Kasei Valles and the western margin of the Lunae Planum plateau and the adjoining Sacra Fossae. Kasei Valles is one of the largest outflow channels on Mars, spanning 3000 km, from the Chryse Planitia basi

March: Chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles (top) and Sacra Fossae (bottom). Kasei Valles is one of the largest Martian canal systems. The large impact crater on the right is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The upper portion of the image swath shows the eastern margin of Kasei Valles and the western margin of the Lunae Planum plateau and the adjoining Sacra Fossae. Kasei Valles is one of the largest outflow channels on Mars, spanning 3000 km, from the Chryse Planitia basi

PIX4616154

Mars: crateres and canals in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater on the left is 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. This image of Hephaestus Fossae was obtained by Esa's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21* North and 126* East on the Red Planet. This image covering an area of approximately 150 km exhibits a large impact crater measuring 20 kilometers in diameter. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region

Mars: crateres and canals in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater on the left is 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. This image of Hephaestus Fossae was obtained by Esa's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21* North and 126* East on the Red Planet. This image covering an area of approximately 150 km exhibits a large impact crater measuring 20 kilometers in diameter. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region

PIX4616155

Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater on the left of the image measures 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. This image of Hephaestus Fossae was obtained by Esa's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21* North and 126* East on the Red Planet. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region. The surface is mostly smooth, and is covered by several small impact craters measuring 800 to 2800 m in diameter. Smaller craters are scattered across the entire region. The left side of the image shows a large impact crater measuri

Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater on the left of the image measures 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. This image of Hephaestus Fossae was obtained by Esa's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21* North and 126* East on the Red Planet. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region. The surface is mostly smooth, and is covered by several small impact craters measuring 800 to 2800 m in diameter. Smaller craters are scattered across the entire region. The left side of the image shows a large impact crater measuri

PIX4616156

March: chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles and Sacra Fossae. The large impact crater is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The image shows an old 35 km - diameter impact crater in the north. The crater's southwestern rim is eroded strongly, mostly by flowing water. The source of the water was located in Echo Chasma, which lies about 850 km to the southwest

March: chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles and Sacra Fossae. The large impact crater is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The image shows an old 35 km - diameter impact crater in the north. The crater's southwestern rim is eroded strongly, mostly by flowing water. The source of the water was located in Echo Chasma, which lies about 850 km to the southwest

PIX4616171

Astrolabe, c.1570 (gilt brass)

Astrolabe, c.1570 (gilt brass)

Flemish School, (16th century)

CH3057865

Landscape, 1617 (ink and colour on silk)

Landscape, 1617 (ink and colour on silk)

Zhao Zuo (17th Century)

IMA1557337

Landscape, 1617 (ink and colour on silk)

Landscape, 1617 (ink and colour on silk)

Zhao Zuo (17th Century)

IMA1557338

Suffering, 1907 (bronze)

Suffering, 1907 (bronze)

Brancusi, Constantin (1876-1957)

INC2970810

Calligraphy (ink on paper)

Calligraphy (ink on paper)

Qichang, Dong (1555-1636)

IMA1557339

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