Possible Volcanic Vent Near Discovery Rupes

The Caloris basin contains a complex mix of impact, tectonic, and volcanic features. At center-right, the elongate depression may be a volcanic vent within the basin. This feature highlights the ambiguity that sometimes arises in discerning whether a depression is due to an impact or a volcanic event, as both can leave elongate depressions. One clue that might point to volcanism is the depression's slightly irregular shape; another is the apparent lack of a rim of impact ejecta that is raised above the baseline level of the surrounding terrain.

This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.

Date acquired: June 30, 2013
Image Mission Elapsed Time (MET): 14936140
Image ID: 4355811
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 24.18°
Center Longitude: 148.1° E
Resolution: 48 meters/pixel
Scale: The proposed vent is 17.9 km (11.1 mi.) across
Incidence Angle: 66.0°
Emission Angle: 50.3°
Phase Angle: 115.4°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Alvin Rupes

Lobate scarps are one of the most common types of landform on Mercury, and frequently cross-cut impact craters of all sizes. However, the example in this image, termed Alvin Rupes, is one of only a very small subset of scarps that are accompanied by thin, linear depressions on their upper surfaces. One possibility is that these features are graben -- fault-bounded troughs that form when rock is extended -- like those seen in Caloris basin, for example. If so, then these graben are among the only such structures known to occur outside of volcanically flooded impact basins and craters.

This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.

Date acquired: July 3, 2013
Image Mission Elapsed Time (MET): 15167012
Image ID: 4372157
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 7.8°
Center Longitude: 151.1° E
Resolution: 54 meters/pixel
Scale: The crater in the center of the image is about 12 km (7.5 mi.) across
Incidence Angle: 75.6°
Emission Angle: 12.6°
Phase Angle: 88.2°
North is up in this image.

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

1000 Downloaded Images Mosaic

On August 3, 2004 the MESSENGER spacecraft blasted off into space from Florida's Cape Canaveral Air Force Station, entering orbit around the innermost planet some six and a half years later, on March 18, 2011.

Over the course of the mission, the MESSENGER team has been posting Featured Images at regular intervals. The first image was posted in August 2005 -- and today we've hit 1,000 Featured Images!

This mosaic celebrates the incredible range of images, maps, and other scientific data shared by the MESSENGER team in more than eight years of web postings, but of course contains just a small percentage of the total collection of images now available online. Although we can't list them all, see if you can spot some highlights like the MESSENGER stamp, Mercury's dark and mysterious north pole, the Caloris basin in full color, lava channels, Pantheon Fossae, images of Earth and Venus, and the Cookie Monster!

Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Unnamed Crater in Shadow

In this dramatic scene, an unnamed crater in Mercury's northern volcanic plains is bathed in darkness as the sun sits low on the horizon. Rising from the floor of the crater is its central peak, a small mountain resulting from the crater's formation. A central peak is a type of crater morphology that lies between "simple" and "peak ring" in the range of crater morphology on Mercury.

This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.

Date acquired: July 07, 2013
Image Mission Elapsed Time (MET): 15510763
Image ID: 4396614
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 69.67°
Center Longitude: 1.51° E
Resolution: 16 meters/pixel
Scale: The image is about 23 km (14.3 mi.) from top to bottom
Incidence Angle: 80.3°
Emission Angle: 49.8°
Phase Angle: 130.1°
North is to the bottom right of the image.

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Different Views of Erte Crater

Presented here are nine views of the same colorful section of Mercury's surface. The first two rows are eight individual images taken through narrowband color filters with center wavelengths of 433, 480, 559, 629, 748, 829, 898, and 996 nanometers (nm). The color composite on the bottom is shown with the 996, 748, and 433 nm WAC filters for red, green, and blue. Color differences on Mercury are subtle, and no prominent features stand out in examination of the eight individual grey-scale images. However, the bluish nature of the crater rays on the left and the reddish cast of the material surrounding the impact crater Erte at right become apparent when the images are co-registered.

Erte was seen recently in a three-dimensional close-up!

This image was acquired as part of MDIS's 8-color base map. The 8-color base map is composed of WAC images taken through eight different narrow-band color filters and covers more than 99% of Mercury's surface with an average resolution of 1 kilometer/pixel. The highest-quality color images are obtained for Mercury's surface when both the spacecraft and the Sun are overhead, so these images typically are taken with viewing conditions of low incidence and emission angles.

Date acquired: April 22, 2011
Image Mission Elapsed Time (MET): 211937370, 211937378, 211937372
Image ID: 161451, 161456, 161452
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 30.04°
Center Longitude: 239.9° E
Resolution: 798 meters/pixel
Scale: The scene is about 420 km (261 mi.) across
Incidence Angle: 59.5°
Emission Angle: 0.1°
Phase Angle: 59.4°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Rude Impact Crater

This view from MESSENGER's Narrow Angle Camera shows the impact crater Rude under morning illumination. The crater has small remnant central peaks that are slightly off-center. A sizable impact crater formed on Rude's floor, possibly causing slumping of Rude's northern rim. Francois Rude was a French sculptor who lived from 1784-1855. His statue of "Mercury Fastening his Sandals" is in the Louvre.

This image was acquired as part of MDIS's high-resolution surface morphology base map. The surface morphology base map covers more than 99% of Mercury's surface with an average resolution of 200 meters/pixel. Images acquired for the surface morphology base map typically are obtained at off-vertical Sun angles (i.e., high incidence angles) and have visible shadows so as to reveal clearly the topographic form of geologic features.

Date acquired: March 04, 2012
Image Mission Elapsed Time (MET): 239375379
Image ID: 1474113
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -33.50°
Center Longitude: 280.4° E
Resolution: 180 meters/pixel
Scale: Rude crater is about 67 km (42 mi.) in diameter
Incidence Angle: 81.8°
Emission Angle: 18.4°
Phase Angle: 100.3°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

V-Shaped Wrinkle Ridges

This view of a location within Mercury's northern volcanic plains includes a set of wrinkle ridges that form a "V" shape.

This image was acquired as part of MDIS's high-resolution surface morphology base map. The surface morphology base map covers more than 99% of Mercury's surface with an average resolution of 200 meters/pixel. Images acquired for the surface morphology base map typically are obtained at off-vertical Sun angles (i.e., high incidence angles) and have visible shadows so as to reveal clearly the topographic form of geologic features.

Date acquired: October 14, 2011
Image Mission Elapsed Time (MET): 227092494
Image ID: 884412
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 79.09°
Center Longitude: 352.7° E
Resolution: 140 meters/pixel
Scale: The "V" is about 59 km (37 mi.) long
Incidence Angle: 84.1°
Emission Angle: 28.2°
Phase Angle: 112.3°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Rayed Impact Crater

Fresh and bright, this unnamed, elongated crater appears to have been formed by an impactor that struck the surface at an oblique angle, causing most of the ejecta to be thrown out unevenly around the crater (notice the bright rays above, below, and to the right of the crater). The marginally bright material in the bottom left corner is actually part of a ray from Hokusai, over 1380 km (about 860 mi.) away!

This image was acquired as a high-resolution targeted color observation. Targeted color observations are images of a small area on Mercury's surface at resolutions higher than the 1-kilometer/pixel 8-color base map. During MESSENGER's one-year primary mission, hundreds of targeted color observations were obtained. During MESSENGER's extended mission, high-resolution targeted color observations are more rare, as the 3-color base map covered Mercury's northern hemisphere with the highest-resolution color images that are possible.

Date acquired: August 19, 2011
Image Mission Elapsed Time (MET): 222275999, 222275995, 222275991
Image ID: 652862, 652861, 652860
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 27.84°
Center Longitude: 30.73° E
Resolution: 116 meters/pixel
Scale: The small bright crater measures about 13 km (8 mi.) in long dimension.
Incidence Angle: 31.1°
Emission Angle: 37.2°
Phase Angle: 68.3°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Impact Craters and a Contractional Ridge Inside Copland Crater

Located in Copland crater, this image consists of three small unnamed impact craters and a contractional ridge that was partly destroyed by the two superimposed impact craters at the center. At one point extensive volcanic eruptions took place within Copland, forming a smooth surface. As the lava cooled it contracted, causing fractures and ridges to form. Images such as this give scientists a better understanding of the processes that accompany flood volcanism on Mercury and other planetary bodies.

This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.

Date acquired: September 13, 2011
Image Mission Elapsed Time (MET): 224423780
Image ID: 755249
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 38.00°
Center Longitude: 72.66° E
Resolution: 35 meters/pixel
Scale: The largest crater is about 9 km (5.5 mi.) in diameter.
Incidence Angle: 75.9°
Emission Angle: 0.2°
Phase Angle: 75.7°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Heine Crater

Heine, detailed here, exhibits Low Reflectance Material (LRM) and high reflectance rays to the west of the crater. The LRM (darker area to the bottom) is likely darker, older material found in some southern areas on Mercury. The bright rays emanate from Degas, located approximately 150 km to the north. Heinrich Heine (1797-1856) is considered one of the most significant German poets of the 19th century. One of Heine's best known poems is "Die Lorelei."

This image was acquired as part of MDIS's high-resolution 3-color imaging campaign. The map produced from this campaign complements the 8-color base map (at an average resolution of 1 km/pixel) acquired during MESSENGER's primary mission by imaging Mercury's surface in a subset of the color filters at the highest resolution possible. The three narrow-band color filters are centered at wavelengths of 430 nm, 750 nm, and 1000 nm, and image resolutions generally range from 100 to 400 meters/pixel in the northern hemisphere.

Date acquired: May 06, 2012
Image Mission Elapsed Time (MET): 244776305, 244776297, 244776301
Image ID: 1773153, 1773151, 1773152
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 32.28°
Center Longitude: 234.5° E
Resolution: 111 meters/pixel
Scale: The diameter of Heine is about 70 km (43 mi.) in diameter.
Incidence Angle: 43.0°
Emission Angle: 0.2°
Phase Angle: 43.1°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Impact Craters

Here multiple generations of craters can be seen. On Mercury, billions of years of impact events can be seen where older craters have younger craters within the interior and on the rim and ejecta. When comparing different terrains on Mercury, the number of craters per unit area can be used to estimate the absolute age of the surfaces, as well as to give insight into the relative ages of the terrains.

This image was acquired as part of MDIS's high-resolution 3-color imaging campaign. The map produced from this campaign complements the 8-color base map (at an average resolution of 1 km/pixel) acquired during MESSENGER's primary mission by imaging Mercury's surface in a subset of the color filters at the highest resolution possible. The three narrow-band color filters are centered at wavelengths of 430 nm, 750 nm, and 1000 nm, and image resolutions generally range from 100 to 400 meters/pixel in the northern hemisphere.

Date acquired: May 23, 2013
Image Mission Elapsed Time (MET): 11621959, 11621954, 11621956
Image ID: 4120141, 4120139, 4120140
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 66.03°
Center Longitude: 243.7° E
Resolution: 183 meters/pixel
Scale: The larger crater is 48 km in diameter (29.5 miles).
Incidence Angle: 79.5°
Emission Angle: 0.2°
Phase Angle: 79.7°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Monteverdi Crater

The large crater seen here, located in Mercury's northern plains, exhibits signs of extensive flooding by lava. Similar to ghost craters that have been completely covered by volcanic flows, much of Monteverde's northern rim and interior have been flooded and filled in by lava. Only the remains of Monteverdi's southern rim jut above the relatively flat interior of the crater. This crater was named after the Italian composer Claudio Monteverdi (1567-1643), whose music marks the transition from the Renaissance style of music to the Baroque style.

This image was acquired as part of MDIS's minimum-phase-angle color campaign. Near the north polar region, the incidence angle (measured from the vertical) is always fairly high because the Sun is low on the horizon. The minimum-phase-angle color campaign acquires images under conditions that minimize the shadows in an image by viewing the surface as nearly as possible from the same direction as the Sun's illumination, which minimizes the phase angle. Images are acquired through five of the WAC's narrow-band color filters, for regions north of 60° N, at an average resolution of 500 meters/pixel. The minimum-phase-angle color campaign began in March 2013.

Date acquired: April 18, 2013
Image Mission Elapsed Time (MET): 8598082, 8598073, 8598079
Image ID: 3905084, 3905081, 3905083
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 63.54°
Center Longitude: 275.7° E
Resolution: 320 meters/pixel
Scale: Monteverdi is 133 km in diameter (83 miles).
Incidence Angle: 76.4°
Emission Angle: 48.3°
Phase Angle: 28.0°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Erte Crater

The crater Erte, the pseudonym of Romain de Tirtoff was a Russian-born French artist and designer who passed away in 1990. The crater that bears his name is a complex crater that is 48.5 km in diameter (30 miles). Here the flat floor of the crater meets the crater rim and the surrounding ejecta blanket.

Date acquired: April 20, 2013
Image Mission Elapsed Time (MET): 8771355
Image ID: 3917367
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 28.14°
Center Longitude: 242.8° E
Resolution: 29 meters/pixel
Scale: The image is 44 km (27 miles) across.
Incidence Angle: 40.8°
Emission Angle: 20.4°
Phase Angle: 61.3°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Mickiewicz Crater

Peak rings within large complex craters are common on Mercury. Here, within Mickiewicz, the lunate central peak ring also contains hollows, which are bright shallow depressions etched into older surfaces.

Date acquired: April 18, 2013
Image Mission Elapsed Time (MET): 8569855
Image ID: 3903061
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 23.15°
Center Longitude: 256.8° E
Resolution: 34 meters/pixel
Scale: The peak ring is about 18 km in diameter (11 miles).
Incidence Angle: 43.7°
Emission Angle: 20.8°
Phase Angle: 64.6°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Chiang K'ui and Other Impact Craters

This color image of the equatorial region of Mercury shows several unnamed craters and part of the crater Chiang K'ui in the northwestern corner. An elongated crater with a central ridge is found in the lower middle part of the scene. Elongated impact craters form when an asteroid or comet strikes the planet at a low angle (relative to the horizontal). Right at the center of the image is a small bright crater with an asymmetrical ray system, which is also diagnostic of a low angle of impact.

This image was acquired as a targeted high-resolution 11-color image set. Acquiring 11-color targets is a new campaign that began in March 2013 and that utilizes all of the WAC's 11 narrow-band color filters. Because of the large data volume involved, only features of special scientific interest are targeted for imaging in all 11 colors.

Date acquired: April 16, 2013
Image Mission Elapsed Time (MET): 8426122, 8426114, 8426110
Image ID: 3892837, 3892835, 3892834
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 12.43°
Center Longitude: 262.4° E
Resolution: 320 meters/pixel
Scale: The image is about 400 km across (248 miles).
Incidence Angle: 40.5°
Emission Angle: 31.2°
Phase Angle: 71.8°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Wrinkle Ridge in the Goethe Impact Basin

This view shows the edge of the Goethe Basin. The margins of the basin interior are marked by wrinkle ridges. Part of one such ridge is shown in this image. The scene also includes small secondary crater chains on the smooth plains that fill the basin, and the hummocky terrain outside of the basin.

Date acquired: February 10, 2013
Image Mission Elapsed Time (MET): 2778942, 2778934, 2778938
Image ID: 3491366, 3491364, 3491365
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 82.92°
Center Longitude: 286.5° E
Resolution: 86 meters/pixel
Scale: The small crater in the center of the image is 2.7 km (1.7 miles) in diameter.
Incidence Angle: 88.0°
Emission Angle: 17.5°
Phase Angle: 87.8°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Lermontov Crater

The crater Lermontov is named after a 19th century Russian poet, Mikhail Lermontov, who is sometimes called "the poet of the Caucasus." The color variations and irregular depressions suggest that this crater was once home to explosive volcanism. The crater also has small bright "spots" on its floor that are interpreted to be hollows.

Date acquired: February 12, 2013
Image Mission Elapsed Time (MET): 3010537, 3010557, 3010541
Image ID: 3507773, 3507778, 3507774
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 15.05°
Center Longitude: 312.1° E
Resolution: 282 meters/pixel
Scale: The larger crater, Lermontov, is 166 km in diameter (103 miles).
Incidence Angle: 49.3°
Emission Angle: 28.7°
Phase Angle: 78.0°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Tyagaraja Crater

This exciting image, taken at a highly oblique angle, shows the interior of Tyagaraja crater (with north being to the right). Complete with central peaks, extensive hollows, and sloping terraced walls, this view allows us to get a unique perspective into the crater and complements other images by adding a different look at the topography of the surface.

Date acquired: November 12, 2011
Image Mission Elapsed Time (MET): 229624183
Image ID: 1005096
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 4.40°
Center Longitude: 211.4° E
Resolution: 39 meters/pixel
Scale: Tyagaraja has a diameter of 97 kilometers (60 miles)
Incidence Angle: 9.4°
Emission Angle: 68.8°
Phase Angle: 78.3°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Eminescu Crater

Centered in this stunning image lies Eminescu crater, illuminated by a bright halo of material around its edge. The ends of a ray system emanating from Xiao Zhao are on the right side of the image. Standing in stark contrast with the low reflectance material within the crater (identifiable as the dark regions on the crater's floor) are bright hollows (identifiable as the bright ring near the crater's center).

Today's image title is in reference to the Cat's Eye Nebula, a well studied, iconic nebula that shares similar features to this image of Eminescu, such as notably the blues, yellows, and spherical shape of the formation.

Date acquired: January 03, 2012
Image Mission Elapsed Time (MET): 234069356, 234069376, 234069360
Image ID: 1218103, 1218108, 1218104
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 10.47°
Center Longitude: 113.8° E
Resolution: 466 meters/pixel
Scale: Eminescu has a diameter 130 km (81 mi)
Incidence Angle: 26.6°
Emission Angle: 23.5°
Phase Angle: 50.2°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Hollows and Pyroclastic Deposits in Praxiteles Crater

This surface, located around the central peak ring of the crater Praxiteles, exhibits the effects that both hollows and pyroclastic deposits can have on pre-existing features. The peak ring (located to the left of this image) can be thought of as being eroded or depressed from the combination of such features. Pyroclastic deposits disturb surface material through volcanic-like events, and hollows are believed to be caused by the sublimation of volatiles, which release sub-surface material and depress the surface even further.

Date acquired: September 04, 2011
Image Mission Elapsed Time (MET): 223615476
Image ID: 716372
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 27.24°
Center Longitude: 301.0° E
Resolution: 19 meters/pixel
Scale: This image is about 20 km (12 mi.) across.
Incidence Angle: 62.4°
Emission Angle: 0.5°
Phase Angle: 61.8°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Volcanic Vent in Kipling Crater

This volcano-like feature is found in Kipling crater and shares similarities to other pyroclastic deposits on Mercury. Where on Earth volcanoes frequently form mountains, on Mercury most of the "volcanoes" that have been identified are characterized by pits or depressions. Described as rimless depressions with irregular shapes, most pyroclastic deposits on Mercury are on the order of a few tens of kilometers in size.

Date acquired: August 16, 2011
Image Mission Elapsed Time (MET): 221974660
Image ID: 638531
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -19.15°
Center Longitude: 71.37° E
Resolution: 51 meters/pixel
Scale: From top to bottom, this feature measures approx. 35 km (22 mi.)
Incidence Angle: 49.7°
Emission Angle: 18.1°
Phase Angle: 31.6°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Matabei Crater

The crater Matabei, shown here, exhibits a dark ray system projecting from one side of the crater. Rays emanating from only certain sides of the crater can be due to an impactor that came in at a grazing angle, such as seen for the craters Hovnatanian and Qi Baishi. However dark rays like these can also indicate an irregular distribution of dark material below the surface. The dark rays are likely sub-surface material that was excavated and ejected out during the initial impact. It is also interesting to note the extensive hollows, identifiable as the bright regions in the southern half of the crater.

Date acquired: August 30, 2011
Image Mission Elapsed Time (MET): 223185654
Image ID: 695876
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -40.07°
Center Longitude: 345.8° E
Resolution: 98 meters/pixel
Scale: Matabei is 24 km. in diameter (15 mi.)
Incidence Angle: 42.4°
Emission Angle: 6.4°
Phase Angle: 46.6°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Impact Craters and Low-Reflectance Materials

Despite the relatively low (1.6 km/pixel) resolution of this image, some clear differences are visible between the the relatively blue, low-reflectance material (LRM) and the nearby terrain. While one large crater near the center left of the image excavates LRM, another to the north has exposed a brighter, redder deposit, suggesting this region is home to compositions that are heterogeneous on a very local scale.

Date acquired: September 21, 2011
Image Mission Elapsed Time (MET): 225100792, 225100800, 225100794
Image ID: 788077, 788082, 788078
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 22.29°
Center Longitude: 21.46° E
Resolution: 1587 meters/pixel
Scale: Image Width 567 km (350 mi)
Incidence Angle: 34.1°
Emission Angle: 0.2°
Phase Angle: 33.9°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Joplin Crater

Joplin crater stands out brilliantly in 3D. With red-cyan glasses, you get an amazing view of Joplin's central peak, which rises around 1 km (0.6 mi.) above the crater floor. This picture has been rotated so that north is toward the bottom to enhance the 3D effect.

Date acquired: January 16, 2012
Image Mission Elapsed Time (MET): 235169452, 235423824
Image ID: 1271337, 1283624
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -38.87° -39.34°
Center Longitude: 26.48° E 26.44° E
Resolution: 176 meters/pixel 187 meters/pixel
Scale: Joplin crater is 135 km (84 mi) in diameter
Incidence Angle: 75.2° 67.9°
Emission Angle: 21.6° 33.4°
Phase Angle: 80.3° 92.6°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Impact Craters and Ghost Craters in the Northern Plains

The very smooth region shown in this image is a part of Mercury's vast northern plains. These smooth plains are thought to have originated as volcanic outflows, in a similar manner to those within the Caloris basin. If you look closely, you can see several impact craters that were buried beneath the lava. These craters are known as "ghost craters" because only faint outlines of their rims remain.

This image was acquired as part of MDIS's high-resolution 3-color imaging campaign. The map produced from this campaign complements the 8-color base map (at an average resolution of 1 km/pixel) acquired during MESSENGER's primary mission by imaging Mercury's surface in a subset of the color filters at the highest resolution possible. The three narrow-band color filters are centered at wavelengths of 430 nm, 750 nm, and 1000 nm, and image resolutions generally range from 100 to 400 meters/pixel in the northern hemisphere.

Date acquired: September 03, 2012
Image Mission Elapsed Time (MET): 255173296, 255173291, 255173293
Image ID: 2512514, 2512512, 2512513
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 51.83°
Center Longitude: 46.39° E
Resolution: 279 meters/pixel
Scale: 188 km (117 mi)
Incidence Angle: 65.2°
Emission Angle: 0.2°
Phase Angle: 65.4°

Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Anaglyph of Crater Hollows

Today's image is another chance to whip out your red-cyan 3D glasses! This multidimensional view, where north is to the left, helps bring to life the extensive hollow network on the crater floor. Look how these bright, irregular depressions create such a dramatic etched appearance!

This image was acquired as a targeted set of stereo images. Targeted stereo observations are acquired at resolutions much higher than that of the 200-meter/pixel stereo base map. These targets acquired with the NAC enable the detailed topography of Mercury's surface to be determined for a local area of interest.

Date acquired: April 24, 2013
Image Mission Elapsed Time (MET): 9145650, 9145778
Image ID: 3944041, 3944042
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 40.26°
Center Longitude: 221.9° E
Resolution: 24 meters/pixel, 28 meters/pixel
Scale: Crater diameter is about 35 km (21.7 miles)
Incidence Angle: 44.6°
Emission Angle: 2.1° 19.9°
Phase Angle: 43.3° 29.4°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Apollodorus Crater

Today's image highlights the striking central uplift of the Apollodorus Crater, located near the center of the Caloris basin. Such peak structures form in complex craters when material is uplifted from depth as a result of the impact process.

Date acquired: June 29, 2013
Image Mission Elapsed Time (MET): 14849521
Image ID: 4349591
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 30.56°
Center Longitude: 163.3° E
Resolution: 34 meters/pixel
Scale: Apollodorus crater is approximately 41 km (25.5 mi.) in diameter.
Incidence Angle: 77.4°
Emission Angle: 32.6°
Phase Angle: 110.0°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Hovnatanian Crater

Today's color image features Hovnatanian crater, named for Armenian painter Hakop Hovnatanian. The crater's elliptical shape and the bright rays' butterfly pattern indicate that a very oblique impact produced Hovnatanian. The brightness of the rays indicate that they are relatively young features on Mercury's surface.

This image was acquired as a targeted high-resolution 11-color image set. Acquiring 11-color targets is a new campaign that began in March 2013 and that utilizes all of the WAC's 11 narrow-band color filters. Because of the large data volume involved, only features of special scientific interest are targeted for imaging in all 11 colors.

Date acquired: May 01, 2013
Image Mission Elapsed Time (MET): 9751363, 9751355, 9751351
Image ID: 3986986, 3986984, 3986983
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: -7.39°
Center Longitude: 172.9° E
Resolution: 394 meters/pixel
Scale: Hovnatanian crater is about 34 km (21 miles) long.
Incidence Angle: 15.7°
Emission Angle: 40.0°
Phase Angle: 28.0°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Rupes

Today's image features a scarp, or cliff face, which is longer than the 77 km shown in this frame. Scarps form as one block of crust is thrusted forward over another, which can result from the cooling of the planet's interior causing global contraction. On Mercury, scarps are called "rupes," which is Latin for cliff.

This image was acquired as a high-resolution targeted observation. Targeted observations are images of a small area on Mercury's surface at resolutions much higher than the 200-meter/pixel morphology base map. It is not possible to cover all of Mercury's surface at this high resolution, but typically several areas of high scientific interest are imaged in this mode each week.

Date acquired: July 08, 2013
Image Mission Elapsed Time (MET): 15627633
Image ID: 4404792
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 20.47°
Center Longitude: 141.0° E
Resolution: 51 meters/pixel
Scale: Image width is about 65 km (40.4 miles)
Incidence Angle: 83.4°
Emission Angle: 38.9°
Phase Angle: 45.4°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Sander Crater

Today's color image highlights the bright hollows on the floor and peaks of Sander crater, named after the German photographer August Sander. The process responsible for these bright, shallow formations is still unknown, but it is possible that volatile sublimation is etching away at the surface.

This image was acquired as a targeted high-resolution 11-color image set. Acquiring 11-color targets is a new campaign that began in March 2013 and that utilizes all of the WAC's 11 narrow-band color filters. Because of the large data volume involved, only features of special scientific interest are targeted for imaging in all 11 colors.

Date acquired: June 06, 2013
Image Mission Elapsed Time (MET): 12802777, 12802773, 12802771
Image ID: 4204118, 4204116, 4204115
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 42.53°
Center Longitude: 154.2° E
Resolution: 265 meters/pixel
Scale: Crater diameter is about 51 km (31.7 miles)
Incidence Angle: 42.9°
Emission Angle: 26.5°
Phase Angle: 69.4°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Impact Craters in Mercury's Southern Hemisphere

This image of Mercury's southern hemisphere shows the large size variation and multiple generations of impact craters on Mercury. Mercury's southern hemisphere is easier to image due to MESSENGER's elliptical orbit, but this orbit also prevents acquisition of high resolution images like those taken in the northern hemisphere.

Date acquired: February 08, 2013
Image Mission Elapsed Time (MET): 2613780
Image ID: 3479116
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 9 (996 nanometers)
Center Latitude: -80.38°
Center Longitude: 302.4° E
Resolution: 1486 meters/pixel
Scale: The complex crater in the center of the image is 151 km in diameter (94 miles).
Incidence Angle: 85.0°
Emission Angle: 25.8°
Phase Angle: 59.1°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Stravinsky Crater's Southern Rim

This image is of the southern rim of the crater Stravinsky. In this high-incidence-angle lighting, the topography of the crater is easily seen. Particularly noticeable is the difference between the crater's flat floor and the hummocky terrain of the ejecta blanket outside the crater. The area in the lower left of the image is part of the Vyasa basin. Since Stravinsky's ejecta overlaps Vyasa, we can deduce that Stravinsky is younger than Vyasa.

Date acquired: February 15, 2013
Image Mission Elapsed Time (MET): 3211541
Image ID: 3522080
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 50.01°
Center Longitude: 281.1° E
Resolution: 256 meters/pixel
Scale: The smaller crater in the upper left is 7.8 km (4.8 miles) in diameter.
Incidence Angle: 82.7°
Emission Angle: 0.1°
Phase Angle: 82.7°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Ghost Crater Amid Ridges

The northern plains on Mercury have lower elevation than surrounding regions. This view of the northern plains includes many wrinkle ridges, a result of tectonic deformation. The ridges outline the rim of a ghost crater, formed when lava covered the crater and differential sagging took place over the rim. The ghost rim is joined by four other prominent ridges.

Date acquired: February 13, 2013
Image Mission Elapsed Time (MET): 3038383, 3038375, 3038379
Image ID: 3509798, 3509796, 3509797
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 69.58°
Center Longitude: 284.1° E
Resolution: 91 meters/pixel
Scale: The ghost crater is 21 km (13 miles) in diameter.
Incidence Angle: 84.9°
Emission Angle: 0.1°
Phase Angle: 85.0°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Monteverdi Crater

The northern plains of Mercury are home to many volcanically flooded craters such as Monteverdi, which occupies part of the lower edge of this image. The plains have abundant wrinkle ridges and fresh craters.

This image was acquired as part of MDIS's minimum-phase-angle color campaign. Near the north polar region, the incidence angle (measured from the vertical) is always fairly high because the Sun is low on the horizon. The minimum-phase-angle color campaign acquires images under conditions that minimize the shadows in an image by viewing the surface as nearly as possible from the same direction as the Sun's illumination, which minimizes the phase angle. Images are acquired through five of the WAC's narrow-band color filters, for regions north of 60° N, at an average resolution of 500 meters/pixel. The minimum-phase-angle color campaign began in March 2013.

Date acquired: April 18, 2013
Image Mission Elapsed Time (MET): 8598032, 8598023, 8598029
Image ID: 3905074, 3905071, 3905073
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 66.83°
Center Longitude: 276.7° E
Resolution: 312 meters/pixel
Scale: The image is about 240 km across (149 miles).
Incidence Angle: 78.3°
Emission Angle: 50.3°
Phase Angle: 28.0°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

A Wrinkle Ridge in Goethe Basin

This small unnamed crater occurs near a wrinkle ridge in Goethe Basin. Since this image was taken near the north pole of Mercury, the shadows are more dramatic than in the equatorial region.

Date acquired: February 09, 2013
Image Mission Elapsed Time (MET): 2721322, 2721314, 2721318
Image ID: 3487267, 3487265, 3487266
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 83.35°
Center Longitude: 291.6° E
Resolution: 86 meters/pixel
Scale: The larger crater in this image is 9.5 km in diameter (6 miles).
Incidence Angle: 87.6°
Emission Angle: 18.9°
Phase Angle: 87.5°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Enhanced Color Map of Mercury

This colorful view of Mercury is similar to that used to generate this movie [23MB, 6.5MB] of Mercury as a spinning globe, and these two individual views (centered at 140°E and 320°E) of the innermost planet. The enhanced color view is overlaid on the global monochrome base map, which is available for download here.

The enhanced color was produced by using images from the color base map imaging campaign during MESSENGER's primary mission. These colors are not what Mercury would look like to the human eye, but rather the colors enhance the chemical, mineralogical, and physical differences between the rocks that make up Mercury's surface. This specific color combination places the second principal component in the red channel, the first principal component in the green channel, and the ratio of the 430 nm/1000 nm filters in the blue channel.

Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 0°
Center Longitude: 180° E
Map Projection: Simple cylindrical projection
Resolution: 3.74 km/pixel
Scale: Mercury's diameter is 4880 kilometers (3030 miles)

Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Digital Elevation Model of Mercury's Northern Hemisphere

The above image is from a digital elevation model (DEM) created by using orbital MLA data. The colors illustrate Mercury's topography, which spans roughly from -5 km (deep blue) to 5 km (red). The specific color bar is given on the ACT-REACT QuickMap description of this DEM layer. Also in QuickMap, this DEM can be used to generate 3D views of the surface.

The DEM can be downloaded on MESSENGER's Global Mosaics of Mercury webpage in a variety of formats and resolutions. The DEM was created by using MLA orbital data through that released by the PDS on March 8, 2013. Due to MESSENGER's highly elliptical orbit, MLA can only range to the surface in the northern hemisphere. Consequently, the DEM products derived from MLA data only cover the northern hemisphere of Mercury. Additionally, the accuracy of each DEM product is higher closer to the north pole, and near the equator, the data are highly interpolated.

Instrument: Mercury Laser Altimeter (MLA)
Center Latitude: 90° N
Map Projection: Polar stereographic projection, extending southward to 55° N, with 0° longitude at the bottom
Resolution: 2 km/pixel
Scale: The distance across the center of this polar map projection is approximately 2,980 kilometers (1850 miles)
Download: Global Mosaics of Mercury Webpage

Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Crater Chains Near an Unnamed Impact Crater

This unnamed complex crater in Mercury's northern hemisphere has produced crater chains. These chains form when a crater ejects material that then plummets towards the surface, producing more craters, often in long linear chains. Another set of crater chains can be seen within the large crater in this image, which most likely originated from the crater Hokusai. Since Hokusai's crater chains lie on top of the crater in this image, the crater Hokusai must be younger!

Date acquired: February 01, 2013
Image Mission Elapsed Time (MET): 2001572
Image ID: 3436074
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filter: 7 (748 nanometers)
Center Latitude: 54.87°
Center Longitude: 6.15° E
Resolution: 234 meters/pixel
Scale: The large crater is 64 km in diameter (40 miles).
Incidence Angle: 54.9°
Emission Angle: 4.5°
Phase Angle: 50.4°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Ray Systems, From Hokusai Crater and Another Impact Crater

This region in Mercury's northern mid-latitudes shows the the rays of the crater Hokusai, along with the bright rays of a much smaller crater in the southeastern portion of the image. Rays are produced when material is excavated from a crater and "thrown" across the surface of a planet. The "butterfly" pattern of the smaller rayed crater is believed to be created during very low-angle impacts where material is ejected in an asymmetrical pattern.

Date acquired: February 01, 2013
Image Mission Elapsed Time (MET): 2001682, 2001674, 2001678
Image ID: 3436082, 3436080, 3436081
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 47.96°
Center Longitude: 7.84° E
Resolution: 131 meters/pixel
Scale: The crater along the southwestern edge of the image is 12.3 km in diameter (7.6 miles).
Incidence Angle: 48.0°
Emission Angle: 0.1°
Phase Angle: 47.9°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

North Polar Terrain

This image highlights a rough region near Mercury's northern pole. It is challenging to image the terrain neat the northern pole, because the sun is always low on the horizon, causing long shadows. In this case, the shadows dramatically accentuate the topography.

Date acquired: June 22, 2012
Image Mission Elapsed Time (MET): 248865807, 248865802, 248865804
Image ID: 2064058, 2064056, 2064057
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 84.33°
Center Longitude: 150.1° E
Resolution: 156 meters/pixel
Scale: 107.18 km (66.6 mi) diagonal image length
Incidence Angle: 84.3°
Emission Angle: 28.7°
Phase Angle: 84.9°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Enterprise Rupes and Rembrandt Basin

This false-color image is located just at the edge of the Rembrandt Basin. The basin edge crosses the newly named Enterprise Rupes. This is just a small meeting of two titans, as Enterprise extends for ~822 km (510 mi.), and Rembrandt is about 723 km (450 mi) in diameter. The edge of Rembrandt is loosely marked with a pink line, and Enterprise with a yellow line.

Date acquired: August 14, 2011
Image Mission Elapsed Time (MET): 221845855, 221845875, 221845859
Image ID: 632458, 632463, 632459
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: -36.15°
Center Longitude: 75.66° E
Resolution: 576 meters/pixel
Scale: This image is about 640 km (398 mi.) across.
Incidence Angle: 56.7°
Emission Angle: 0.5°
Phase Angle: 56.3°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Belgica Rupes

This image highlights the difference between the areas on and below the newly named Belgica Rupes. The arrows show Belgica's location, stretching along most of this image for about 764 km. Notice how some of the smaller, newer craters obscure the scarp line, while the older craters were clearly disrupted by the formation of Belgica Rupes.

The word 'rupes' comes from the latin word for cliff. All rupes on Mercury are named after vehicles of exploration. Belgica was a Belgian ship that explored the south pole of earth in 1898. Belgian Rupes is also very close to the southern pole of Mercury. It's name was approved by the IAU on June 6, 2013 along with 9 other rupes.

Date acquired: August 17, 2011
Image Mission Elapsed Time (MET): 222063126, 222063130, 222063122
Image ID: 642667, 642668, 642666
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 3, 4, 6 (479, 558, 433 nanometers) in red, green, and blue
Center Latitude: -52.80°
Center Longitude: 64.08° E
Resolution: 896 meters/pixel
Scale: Belgica Rupes extends 764 km (475 miles).
Incidence Angle: 63.3°
Emission Angle: 0.4°
Phase Angle: 63.2°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Impact Craters and a Scarp

Within the yellow box, three unnamed craters are stacked one upon another. The rim of the largest of the three is partially obscured, and the crater floor appears filled in, likely due to flooding by volcanism. Superposed on this crater is another younger crater, which has also been impacted by an even younger crater. To the north of the craters, a long scarp (yellow arrows) cuts across the region.

Date acquired: March 30, 2011
Image Mission Elapsed Time (MET): 209960906
Image ID: 67407
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -63.00°
Center Longitude: 5.11° E
Resolution: 387 meters/pixel
Scale: The yellow box is ~60.5 km (37.6 mi) wide.
Incidence Angle: 63.5°
Emission Angle: 1.9°
Phase Angle: 61.8°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

Raden Saleh Crater

This color image shows Raden Saleh crater in a new light. The crater's bright ejecta rays are superimposed on the surrounding terrain, including a patch of dark low reflectance material (LRM). In the lower right corner, rays from Qi Baishi crater are also visible.

This image was acquired as a targeted high-resolution 11-color image set. Acquiring 11-color targets is a new campaign that began in March 2013 and that utilizes all of the WAC's 11 narrow-band color filters. Because of the large data volume involved, only features of special scientific interest are targeted for imaging in all 11 colors.

Date acquired: May 08, 2013
Image Mission Elapsed Time (MET): 10356510, 10356502, 10356498
Image ID: 4029993, 4029991, 4029990
Instrument: Wide Angle Camera (WAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue
Center Latitude: 2.04°
Center Longitude: 158.8° E
Resolution: 440 meters/pixel
Scale: Raden Saleh crater is about 23 km (14 miles) in diameter
Incidence Angle: 21.5°
Emission Angle: 38.1°
Phase Angle: 59.6°

Photo credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington