Mission Viking

<h1>PIA00003: Valles Marineris Hemisphere</h1><div class="PIA00003" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mosaic composed of 102 Viking Orbiter images of Mars, covering nearly a full hemisphere of the planet (approximate latitude -55 to 60 degrees, longitude 30 to 130 degrees). The mosaic is in a point-perspective projection with a scale of about 1 km/pixel. The color variations have been enhanced by a factor of about two, and the large-scale brightness variations (mostly due to sun-angle variations) have been normalized by large-scale filtering. The center of the scene shows the entire Valles Marineris canyon system, over 3,000 km long and up to 8 km deep, extending from Noctis Labyrinthus, the arcuate system of graben to the west, to the chaotic terrain to the east. Bright white layers of material in the eastern canyons may consist of carbonates deposited in ancient lakes. Huge ancient river channels begin from the chaotic terrain and from north-central canyons and run north. Many of the channels flowed into a basin called Acidalia Planitia, which is the dark area in the extreme north of this picture. The Viking 1 landing site (Mutch Memorial Station) is located in Chryse Planitia, south of Acidalia Planitia. The three Tharsis volcanoes (dark red spots), each about 25 km high, are visible to the west. The large crater with two prominent rings located at the bottom of this image is named Lowell, after the Flagstaff astronomer. The images were acquired by Viking Orbiter 1 in 1980 during early northern summer on Mars (Ls = 70 degrees); the atmosphere was relatively dust-free. A variety of clouds appear as bright blue streaks and hazes, and probably consist of water ice. Long, linear clouds north of central Valles Marineris appear to emanate from impact craters.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00003" onclick="window.open(this.href); return false;" title="Voir l'image PIA00003: Valles Marineris Hemisphere sur le site de la NASA">Voir l'image PIA00003: Valles Marineris Hemisphere sur le site de la NASA.</a></div>
PIA00003: Valles Marineris Hemisphere
<h1>PIA00004: Schiaparelli Hemisphere</h1><div class="PIA00004" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This mosaic is composed of about 100 red- and violet- filter Viking Orbiter images, digitally mosaiced in an orthographic projection at a scale of 1 km/pixel. The images were acquired in 1980 during mid northern summer on Mars (Ls = 89 degrees). The center of the image is near the impact crater Schiaparelli (latitude -3 degrees, longitude 343 degrees). The limits of this mosaic are approximately latitude -60 to 60 degrees and longitude 280 to 30 degrees. The color variations have been enhanced by a factor of two, and the large-scale brightness variations (mostly due to sun-angle variations) have been normalized by large-scale filtering. The large circular area with a bright yellow color (in this rendition) is known as Arabia. The boundary between the ancient, heavily-cratered southern highlands and the younger northern plains occurs far to the north (latitude 40 degrees) on this side of the planet, just north of Arabia. The dark streaks with bright margins emanating from craters in the Oxia Palus region (to the left of Arabia) are caused by erosion and/or deposition by the wind. The dark blue area on the far right, called Syrtis Major Planum, is a low-relief volcanic shield of probable basaltic composition. Bright white areas to the south, including the Hellas impact basin at the lower right, are covered by carbon dioxide frost.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00004" onclick="window.open(this.href); return false;" title="Voir l'image PIA00004: Schiaparelli Hemisphere sur le site de la NASA">Voir l'image PIA00004: Schiaparelli Hemisphere sur le site de la NASA.</a></div>
PIA00004: Schiaparelli Hemisphere
<h1>PIA00005: Oblique View of Valles Marineris</h1><div class="PIA00005" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">An oblique, color image of central Valles Marineris, Mars showing relief of Ophir and Candor Chasmata; view toward north. The photograph is a composite of Viking high-resolution images in black and white and low-resolution images in color. Ophir Chasma on the north is approximately 300 km across and as deep as 10 km. The connected chasma or valleys of Valles Marineris may have formed from a combination of erosional collapse and structural activity. Tongues of interior layered deposits on the floor of the chasmata can be observed as well as young landslide material along the base of Ophir Chasma's north wall.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00005" onclick="window.open(this.href); return false;" title="Voir l'image PIA00005: Oblique View of Valles Marineris sur le site de la NASA">Voir l'image PIA00005: Oblique View of Valles Marineris sur le site de la NASA.</a></div>
PIA00005: Oblique View of Valles Marineris
<h1>PIA00006: Oblique View with Altimetry of Valles Marineris</h1><div class="PIA00006" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">An oblique, color image of central Valles Marineris, Mars showing relief of Ophir and Candor Chasmata; view toward east. The photograph is a composite of Viking high-resolution images in black and white and low-resolution images in color. Ophir Chasma on the north (left side) is approximately 300 km across and as deep as 10 km. The connected chasma or valleys of Valles Marineris may have formed from a combination of erosional collapse and structural activity. Tongues of interior layered deposits on the floor of the chasmata can be observed as well as young landslide material along the base of Ophir Chasma's north wall.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00006" onclick="window.open(this.href); return false;" title="Voir l'image PIA00006: Oblique View with Altimetry of Valles Marineris sur le site de la NASA">Voir l'image PIA00006: Oblique View with Altimetry of Valles Marineris sur le site de la NASA.</a></div>
PIA00006: Oblique View with Altimetry of Valles Marineris
<h1>PIA00009: North Polar Ice Cap</h1><div class="PIA00009" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">North polar ice cap of Mars, as seen during mid summer in the northern hemisphere. The reddish areas consist of eolian dust, bright white areas consist of a mixture of water ice and dust, and the dark blue areas consist of sand dunes forming a huge 'collar' around the polar ice cap. (The colors have been enhanced with a decorrelation stretch to better show the color variability.) Shown here is an oblique view of the polar region, as seen with the Viking 1 spacecraft orbiting Mars over latitude 39 degrees north. The spiral bands consist of valleys which form by a combination of the Coriolis forces, wind erosion, and differential sublimation and condensation. In high-resolution images the polar caps are seen to consist of thick sequences of layered deposits, suggesting that cyclical climate changes have occurred on Mars. Cyclical climate changes are readily explained by quasi-periodic changes in the amount and distribution of solar heating resulting from perturbations in orbital and axial elements. Variations in the Earth's orbit have also been linked to the terrestrial climate changes during the ice ages.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00009" onclick="window.open(this.href); return false;" title="Voir l'image PIA00009: North Polar Ice Cap sur le site de la NASA">Voir l'image PIA00009: North Polar Ice Cap sur le site de la NASA.</a></div>
PIA00009: North Polar Ice Cap
<h1>PIA00091: Cerberus Hemisphere</h1><div class="PIA00091" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This mosaic is composed of 104 Viking Orbiter images acquired on February 11, 1980. At that time, it was early northern summer on Mars (Ls = 65 degrees). The center of the image is at latitude 3 degrees, longitude 185 degrees, and the latitude limits are approximately 60 degrees N. and S. This image is in an orthographic projection with a scale of 1 km/pixel. The color variations have been enhanced by a factor of 2, and the large-scale brightness variations (mostly due to sun-angle variations) have been normalized by large-scale filtering. A major geologic boundary extends across this mosaic, with the lower third of the image showing ancient cratered highlands; north of this boundary are the lowland northern plains. A series of poorly-indurated sedimentary deposits occur just north of the highland-lowland boundary; some workers believe that these are explosive volcanic deposits (ignimbrites) whereas others have postulated that they are paleo-polar deposits. Other prominent features in this image include the large dark area left of the image center (named Cerberus), and the Elysium volcanic region (bright yellowish area north of Cerberus). The crater 'Mie' is located near the top left, and has a dark spot near its center. The Viking 2 Lander is located about 400 km west of the center of this crater, or about 1 1/2 crater diameter left of the left edge of the crater. Thin white clouds are dispersed over the northern hemisphere, and the opaque cloud in the upper right overlies the Olympus Mons Aureole. The arcuate markings west of the Aureole are thought to be extended drifts of windblown material. The bright blue area at the bottom of the picture shows the extent of the seasonal carbon dioxide polar cap (these frosts are actually white).<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00091" onclick="window.open(this.href); return false;" title="Voir l'image PIA00091: Cerberus Hemisphere sur le site de la NASA">Voir l'image PIA00091: Cerberus Hemisphere sur le site de la NASA.</a></div>
PIA00091: Cerberus Hemisphere
<h1>PIA00092: Syrtis Major Hemisphere</h1><div class="PIA00092" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This mosaic is composed of about 100 red- and violet- filter Viking Orbiter images, digitally mosaiced in an orthographic projection at a scale of 1 km/pixel. The images were acquired in 1980 during early northern summer on Mars (Ls = 75 degrees). The center of this image is near latitude 0 degree, longitude 310 degree, and the limits of this mosaic are approximately latitude -60 to 60 degrees and longitude 260 to 350 degrees. The color variations have been enhanced by a factor of two, and the large-scale brightness variations (mostly due to sun-angle variations) have been normalized by large-scale filtering. The large circular area with a bright yellow color (in this rendition) located in the upper left area of the image is known as Arabia. The boundary between the ancient, heavily-cratered southern highlands and the younger northern plains occurs far to the north (latitude 40 degrees) on this side of the planet, just north of Arabia. The dark blue area to the right of Arabia, called Syrtis Major Planum, is a low-relief volcanic shield of probable basaltic composition. The bright yellow area to the right of Syrtis Major Isidis Planitia, an ancient impact basin. Bright white areas to the south, including the Hellas impact basin at lower right, are covered by carbon dioxide frost.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00092" onclick="window.open(this.href); return false;" title="Voir l'image PIA00092: Syrtis Major Hemisphere sur le site de la NASA">Voir l'image PIA00092: Syrtis Major Hemisphere sur le site de la NASA.</a></div>
PIA00092: Syrtis Major Hemisphere
<h1>PIA00145: Surface Sampler Arm Acquiring Sample</h1><div class="PIA00145" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Operation of the surface sampler in obtaining Martian soil for Viking 2's molecular analysis experiment last Saturday (September 25) was closely monitored by one of the Lander cameras because of the precision required in trenching the small area--8 by 9 inches-surrounded by rocks. Dubbed 'Bonneville Salt Flats,' the exposure of thin crust appeared unique in contrast with surrounding materials and became a prime target for organic analysis in spite of potential hazards. Large rock in foreground is 8 inches high. At left, the sampler scoop has touched the surface, missing the rock at upper left by a comfortable 6 inches, and the backhoe has penetrated the surface about one-half inch. The scoop was then pulled back to sample the desired point and (second photo) the backhoe furrowed the surface pulling a piece of thin crust toward the spacecraft. The initial touchdown and retraction sequence was used to avoid a collision between a rock in the shadow of the arm and a plate joining the arm and scoop. The rock was cleared by 2 to 3 inches. The third picture was taken 8 minutes after the scoop touched the surface and shows that the collector head has acquired a quantity of soil. With surface sampler withdrawn (right), the foot-long trench is seen between the rocks. The trench is three inches wide and about 1 1/2 to 2 inches deep. The scoop reached to within 3 inches of the rock at far end of trench. Penetration appears to have left a cavernous opening roofed by the crust and only about one inch of undisturbed crust separates the deformed surface and the rock.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00145" onclick="window.open(this.href); return false;" title="Voir l'image PIA00145: Surface Sampler Arm Acquiring Sample sur le site de la NASA">Voir l'image PIA00145: Surface Sampler Arm Acquiring Sample sur le site de la NASA.</a></div>
PIA00145: Surface Sampler Arm Acquiring Sample
<h1>PIA00151: Memnonia Fossae (Enhanced Color)</h1><div class="PIA00151" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Tharsis-centered volcanic and tectonic activity resulted in the formation of radial grabens of Memnonia Fossae, which cut materials of the ancient cratered highlands and the relatively young, highland-embaying lava flows from the Tharsis volcanoes. Center of picture is at latitude 16 degrees S., longitude 142 degrees W. The enhanced color version (following decorrelation stretch) reveals a diversity of subtle color variations; many of the color variations may be due to different lava flow units and variable amounts of weathering, possible alteration by water, and eolian redistributions. Viking Orbiter Picture Numbers 41B52 (green) 41B54 (red), and 41B56 (blue) at 198 m/pixel resolution. Picture width is 206 km. North is 119 degrees counter-clockwise from top.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00151" onclick="window.open(this.href); return false;" title="Voir l'image PIA00151: Memnonia Fossae (Enhanced Color) sur le site de la NASA">Voir l'image PIA00151: Memnonia Fossae (Enhanced Color) sur le site de la NASA.</a></div>
PIA00151: Memnonia Fossae (Enhanced Color)
<h1>PIA00152: North Polar Cap Margin (natural color (top) and enhanced color (bottom))</h1><div class="PIA00152" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Water ice mixed with dust form the residual north polar ice cap (brown color). Seasonal frost of relatively pure ice (white color) partly blankets the polar deposits. A large trough, which is occupied by linear sand dunes (dark band), exposes polar layered deposits. The layered deposits hold a partial record of the history of atmospheric activity and climate of Mars. Center of picture is at latitude 82 degrees N., longitude 84 degrees W. Viking Orbiter Picture Numbers 82B11-12 (violet), 82B15-16 (green), and 82B17-18 (red) at 53 m/pixel resolution. Picture width is 106 km. North is 6 degrees counter-clockwise from top.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00152" onclick="window.open(this.href); return false;" title="Voir l'image PIA00152: North Polar Cap Margin (natural color (top) and enhanced color (bottom)) sur le site de la NASA">Voir l'image PIA00152: North Polar Cap Margin (natural color (top) and enhanced color (bottom)) sur le site de la NASA.</a></div>
PIA00152: North Polar Cap Margin (natural color (top) and enhanced color (bottom))
<h1>PIA00153: Reull Valles (Enhanced Color)</h1><div class="PIA00153" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">A conspicuous fretted channel, Reull Valles, which dissects wall deposits of the large Hellas impact basin, trends southeast towards the basin floor. Center of picture is at latitude 42 degrees S., longitude 258 degrees W. Fretted channels are wide, flat-floored channels with steep walls, which may be runoff channels that have been modified and enlarged by masswasting. Many nearby hills and mountains are surrounded by lobate debris aprons, which may have formed by slow creep of rock deposits aided by the presence of near-surface ice. Layering is exposed in the channel and crater walls. The color variations of the surface are very bland in this region; most of the variations seen are due to atmospheric scattering. Viking Orbiter Picture Numbers 126A08 (violet), 126A16 (green), and 126A24 (red) at 157 m/pixel resolution. Picture width is 161 km. North is 112 degrees clockwise from top.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00153" onclick="window.open(this.href); return false;" title="Voir l'image PIA00153: Reull Valles (Enhanced Color) sur le site de la NASA">Voir l'image PIA00153: Reull Valles (Enhanced Color) sur le site de la NASA.</a></div>
PIA00153: Reull Valles (Enhanced Color)
<h1>PIA00154: Claritas Fossae (Enhanced Color)</h1><div class="PIA00154" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;"><p>Syria Planum-centered volcanism and tectonism produced fractures, narrow to broad grabens, large scarps, and broad fold and thrust ridges that deformed a basement complex. Picture is centered at latitude 29 degrees S., longitude 101 degrees W. The region appears to have been mantled by materials of unknown origin. Colors seen are due to variable proportions of dust and sand and possibly to different kinds of weathering or alterations. Viking Orbiter Picture Numbers 421A42 (violet), 421A48 (green), and 421A50 (red) at 106 m/pixel resolution. Picture width is 117 km. North is 101 degrees clockwise from top.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00154" onclick="window.open(this.href); return false;" title="Voir l'image PIA00154: Claritas Fossae (Enhanced Color) sur le site de la NASA">Voir l'image PIA00154: Claritas Fossae (Enhanced Color) sur le site de la NASA.</a></div>
PIA00154: Claritas Fossae (Enhanced Color)
<h1>PIA00155: West Candor Chasm (Enhanced Color)</h1><div class="PIA00155" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This picture (centered at latitude 4 degrees S., longitude 76 degrees W.) shows areas of central Valles Marineris, including Candor Chasm (lower left), Ophir Chasm (lower right), and Hebes Chasm (upper right). Complex layered deposits in the canyons may have been deposited in lakes, and if so, are of great interest for future searches for fossil life on Mars. The pinkish deposits in Candor Chasm may be due to hydrothermal alterations and the production of crystalline ferric oxides (Geissler et al., 1993, Icarus 106,380). Viking Orbiter Picture Numbers 279B02 (violet), 279B10 (green), and 279B12 (red) at 240 m/pixel resolution. Picture width is 231 km. North is 47 degrees clockwise from top.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00155" onclick="window.open(this.href); return false;" title="Voir l'image PIA00155: West Candor Chasm (Enhanced Color) sur le site de la NASA">Voir l'image PIA00155: West Candor Chasm (Enhanced Color) sur le site de la NASA.</a></div>
PIA00155: West Candor Chasm (Enhanced Color)
<h1>PIA00156: Melas Chasm (Enhanced Color)</h1><div class="PIA00156" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">This picture (centered at latitude 10 degrees S., longitude 74 degrees W.) shows much of Melas Chasm and a portion of Candor Chasm (upper right) in central Valles Marineris. Several interesting compositional units can be seen in the image: white materials (center-right) may consist of carbonates or some other evaporite deposit, pinkish materials (upper right) may be relatively rich in crystalline iron oxides, and greenish materials (lower left) correspond to dark sand dunes. Viking Orbiter Picture Numbers 279B41 (violet), 279B49 (green), and 279B51 (red) at 257 m/pixel resolution. Picture width is 261 km. North is 50 degrees clockwise from top.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00156" onclick="window.open(this.href); return false;" title="Voir l'image PIA00156: Melas Chasm (Enhanced Color) sur le site de la NASA">Voir l'image PIA00156: Melas Chasm (Enhanced Color) sur le site de la NASA.</a></div>
PIA00156: Melas Chasm (Enhanced Color)
<h1>PIA00161: MC-1 Mare Boreum Region</h1><div class="PIA00161" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-1 quadrangle, Mare Boreum region of Mars. The central part is covered by a residual ice cap that is cut by spiral-patterned troughs exposing layered terrain. The cap is surrounded by broad flat plains and large dune fields. Latitude range 65 to 90, longitude range -180 to 180.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00161" onclick="window.open(this.href); return false;" title="Voir l'image PIA00161: MC-1 Mare Boreum Region sur le site de la NASA">Voir l'image PIA00161: MC-1 Mare Boreum Region sur le site de la NASA.</a></div>
PIA00161: MC-1 Mare Boreum Region
<h1>PIA00162: MC-2 Diacria Region</h1><div class="PIA00162" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-2 quadrangle, Diacria region of Mars. The northern two-thirds is dominated by relatively smooth plains. The southeastern part is marked by aureole deposits of the largest known volcano in the solar system, Olympus Mons. Latitude range 30 to 65 degrees, longitude range 120 to 180.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00162" onclick="window.open(this.href); return false;" title="Voir l'image PIA00162: MC-2 Diacria Region sur le site de la NASA">Voir l'image PIA00162: MC-2 Diacria Region sur le site de la NASA.</a></div>
PIA00162: MC-2 Diacria Region
<h1>PIA00163: MC-3 Arcadia Region</h1><div class="PIA00163" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-3 quadrangle, Arcadia region of Mars. The southern part contains the large shield volcano, Alba Patera, and the highly faulted Tempe Terra province, which includes many small volcanoes. The northern part is dominated by relatively smooth plains. Latitude range 30 to 65 degrees, longitude range 60 to 120 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00163" onclick="window.open(this.href); return false;" title="Voir l'image PIA00163: MC-3 Arcadia Region sur le site de la NASA">Voir l'image PIA00163: MC-3 Arcadia Region sur le site de la NASA.</a></div>
PIA00163: MC-3 Arcadia Region
<h1>PIA00164: MC-4 Mare Acidalium Region</h1><div class="PIA00164" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-4 quadrangle, Mare Acidalium region of Mars. The central part is characterized by dark depression--the northern Chryse basin, which contains relatively smooth plains where several large outflow channels terminate. The depression is partly bounded to the southwest by the highly faulted and heavily cratered Tempe Terra province, to the southeast by the heavily cratered Arabia Terra province, and to the north by relatively smooth plains of Vastitas Borealis. Latitude range 30 to 65 degrees, longitude range 0 to 60 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00164" onclick="window.open(this.href); return false;" title="Voir l'image PIA00164: MC-4 Mare Acidalium Region sur le site de la NASA">Voir l'image PIA00164: MC-4 Mare Acidalium Region sur le site de la NASA.</a></div>
PIA00164: MC-4 Mare Acidalium Region
<h1>PIA00165: MC-5 Ismenius Lacus Region</h1><div class="PIA00165" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-5 quadrangle, Ismenius Lacus region of Mars. Heavily cratered highlands of the southern part are separated from the relatively smooth plains of the northern part by a belt of dissected terrain, containing mesas and buttes. Latitude range 30 to 65 degrees, longitude range -60 to 0 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00165" onclick="window.open(this.href); return false;" title="Voir l'image PIA00165: MC-5 Ismenius Lacus Region sur le site de la NASA">Voir l'image PIA00165: MC-5 Ismenius Lacus Region sur le site de la NASA.</a></div>
PIA00165: MC-5 Ismenius Lacus Region
<h1>PIA00166: MC-6 Casius Region</h1><div class="PIA00166" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-6 quadrangle, Casius region of Mars. Except for the highly dissected southwestern part, which contains faults, mesas, and buttes of Nilosyrtis Mensae, the Casius region is dominated by light-colored and dark, relatively smooth plains. Latitude range 30 to 65 degrees, longitude range -120 to -60 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00166" onclick="window.open(this.href); return false;" title="Voir l'image PIA00166: MC-6 Casius Region sur le site de la NASA">Voir l'image PIA00166: MC-6 Casius Region sur le site de la NASA.</a></div>
PIA00166: MC-6 Casius Region
<h1>PIA00167: MC-7 Cebrenia Region</h1><div class="PIA00167" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-7 quadrangle, Cebrenia region of Mars. The northwestern two-thirds is dominated by light-colored and dark, relatively smooth plains. The southeastern part is marked by one of three prominent Elysium shield volcanoes, Hecates Tholus, and the ridge system of Phlegra Montes. Latitude range 30 to 65 degrees, longitude range -180 to -120 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00167" onclick="window.open(this.href); return false;" title="Voir l'image PIA00167: MC-7 Cebrenia Region sur le site de la NASA">Voir l'image PIA00167: MC-7 Cebrenia Region sur le site de la NASA.</a></div>
PIA00167: MC-7 Cebrenia Region
<h1>PIA00168: MC-8 Amazonis Region</h1><div class="PIA00168" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-8 quadrangle, Amazonis region of Mars. The central part, which is dominated by light-colored, relatively smooth to hummocky plains of Amazonis Planitia, is partly bounded to the east by the western flank of the largest known volcano in the solar system, Olympus Mons, and its associated aureole deposits. Moderately cratered knobby terrain is west of the plains of Amazonis Planitia. Latitude range 0 to 30 degrees, longitude range 135 to 180 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00168" onclick="window.open(this.href); return false;" title="Voir l'image PIA00168: MC-8 Amazonis Region sur le site de la NASA">Voir l'image PIA00168: MC-8 Amazonis Region sur le site de la NASA.</a></div>
PIA00168: MC-8 Amazonis Region
<h1>PIA00169: Mc-9 Tharsis Region</h1><div class="PIA00169" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-9 quadrangle, Tharsis region of Mars. Three of the four largest shield volcanoes on Mars--Olympus, Ascraeus, and Pavonis Montes--lie within the Tharsis quadrangle, together with several smaller shields. The north-central part is marked by highly faulted terrain of Ceraunius Fossae. Latitude range 0 to 30 degrees, longitude range 90 to 135 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00169" onclick="window.open(this.href); return false;" title="Voir l'image PIA00169: Mc-9 Tharsis Region sur le site de la NASA">Voir l'image PIA00169: Mc-9 Tharsis Region sur le site de la NASA.</a></div>
PIA00169: Mc-9 Tharsis Region
<h1>PIA00170: MC-10 Lanae Palus Region</h1><div class="PIA00170" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-10 quadrangle, Lanae Palus region of Mars. The western part is dominated by lava flows of the Tharsis region. The central part includes ridged terrain of Lunae Planum. The west and north borders of Lunae Planum are dissected by the large, relatively young outflow channel, Kasei Vallis, which terminates in Chryse Planitia. Latitude range 0 to 30 degrees, longitude range 45 to 90 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00170" onclick="window.open(this.href); return false;" title="Voir l'image PIA00170: MC-10 Lanae Palus Region sur le site de la NASA">Voir l'image PIA00170: MC-10 Lanae Palus Region sur le site de la NASA.</a></div>
PIA00170: MC-10 Lanae Palus Region
<h1>PIA00171: MC-11 Oxia Palus Region</h1><div class="PIA00171" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-11 quadrangle, Oxia Palus region of Mars. Heavily cratered highlands of the southeastern two-thirds are cut by several large outflow channels. These channels terminate at the dark large depression, Chryse basin, which contain relatively smooth plains in the northwestern part. Latitude range 0 to 30 degrees, longitude range 0 to 45 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00171" onclick="window.open(this.href); return false;" title="Voir l'image PIA00171: MC-11 Oxia Palus Region sur le site de la NASA">Voir l'image PIA00171: MC-11 Oxia Palus Region sur le site de la NASA.</a></div>
PIA00171: MC-11 Oxia Palus Region
<h1>PIA00172: MC-12 Arabia Region</h1><div class="PIA00172" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-12 quadrangle, Arabia region of Mars. Heavily cratered highlands dominate the Arabia quadrangle. The northeastern part is marked by a large impact crater, Cassini. Cassini is an ancient remnant of the many large impact events that occurred during the period of heavy bombardment. Latitude range 0 to 30 degrees, longitude range -45 to 0 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00172" onclick="window.open(this.href); return false;" title="Voir l'image PIA00172: MC-12 Arabia Region sur le site de la NASA">Voir l'image PIA00172: MC-12 Arabia Region sur le site de la NASA.</a></div>
PIA00172: MC-12 Arabia Region
<h1>PIA00173: MC-13 Syrtis Major Region</h1><div class="PIA00173" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-13 quadrangle, Syrtis Major region of Mars. The central part is dominated by dark dust and lava flows of the Syrtis Major Planitia region. These lava flows are partly bounded to the east by a large depression, Isidis basin, which contains smooth plains, and to the west and north by heavily cratered and moderately faulted highlands. Latitude range 0 to 30 degrees, longitude range -90 to -45 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00173" onclick="window.open(this.href); return false;" title="Voir l'image PIA00173: MC-13 Syrtis Major Region sur le site de la NASA">Voir l'image PIA00173: MC-13 Syrtis Major Region sur le site de la NASA.</a></div>
PIA00173: MC-13 Syrtis Major Region
<h1>PIA00174: MC-14 Amenthes Region</h1><div class="PIA00174" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-14 quadrangle, Amenthes region of Mars. The southern part includes heavily cratered highlands. The northern part is dominated by relatively smooth plains of Elysium Planitia and the eastern half of the Isidis basin. Latitude range 0 to 30 degrees, longitude range -135 to -90 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00174" onclick="window.open(this.href); return false;" title="Voir l'image PIA00174: MC-14 Amenthes Region sur le site de la NASA">Voir l'image PIA00174: MC-14 Amenthes Region sur le site de la NASA.</a></div>
PIA00174: MC-14 Amenthes Region
<h1>PIA00175: MC-15 Elysium Region</h1><div class="PIA00175" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-15 quadrangle, Elysium region of Mars. The Elysium quadrangle includes relatively smooth lowland plains immediately north of the more cratered highlands. The plains are interrupted on the northwest by two large shield volcanoes, Elysium Mons and Albor Tholus. The plains are also marked by an elongate crater, Orcus Patera, at the east boundary and a band of knobby terrain that extends northeastward through the eastern part. Latitude range 0 to 30 degrees, longitude range -180 to -135 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00175" onclick="window.open(this.href); return false;" title="Voir l'image PIA00175: MC-15 Elysium Region sur le site de la NASA">Voir l'image PIA00175: MC-15 Elysium Region sur le site de la NASA.</a></div>
PIA00175: MC-15 Elysium Region
<h1>PIA00176: MC-16 Memnonia Region</h1><div class="PIA00176" lang="en" style="width:800px;text-align:left;margin:auto;background-color:#000;padding:10px;max-height:150px;overflow:auto;">Mars digital-image mosaic merged with color of the MC-16 quadrangle, Memnonia region of Mars. Heavily cratered highlands in the southern two-thirds are cut in the northeastern part by a large outflow channel, Mangala Vallis. The highlands are bounded to the north by undulating wind-eroded deposits and to the east by lava flows of the Tharsis region. Latitude range -30 to 0 degrees, longitude range 135 to 180 degrees.<br /><br /><a href="http://photojournal.jpl.nasa.gov/catalog/PIA00176" onclick="window.open(this.href); return false;" title="Voir l'image PIA00176: MC-16 Memnonia Region sur le site de la NASA">Voir l'image PIA00176: MC-16 Memnonia Region sur le site de la NASA.</a></div>
PIA00176: MC-16 Memnonia Region

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