skip to main |
skip to sidebar
In the top left part of this image is Seuss, a complex crater with hollows present on the crater's floor. In this enhanced color image, the hollows appear as bright blue-white features. Just outside of Seuss' rim, you can see some material that appears darker brown in the image. This is LRM, or Low Reflectance Material, and was probably excavated by the impactor when Seuss was formed. Extending from Seuss are bright crater rays, which are streams of ejecta that were thrown from the crater upon impact. In the bottom right of the image, you can see an irregularly shaped, orange-yellow depression that could be a volcanic vent.
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: July 08, 2014
Image Mission Elapsed Time (MET): 47121909, 47121901, 47121905
Image ID: 6643252, 6643250, 6643251
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: 2.83º
Center Longitude: 37.11º E
Resolution: 528 meters/pixel
Scale: Seuss is 64 km (40 miles) in diameter
Incidence Angle: 15.8º
Emission Angle: 12.2º
Phase Angle: 28.0º
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This image features a simple crater in the northern smooth plains. Superimposed on the wall of this crater is another impact crater. The smaller crater is elliptical in shape, which is most likely due to being formed on a slope on the larger crater's wall. It also appears that this impact event caused material to slide down the crater wall, which can be seen in this high-resolution image.
This image was acquired as part of the MDIS low-altitude imaging campaign. During MESSENGER's second extended mission, the spacecraft makes a progressively closer approach to Mercury's surface than at any previous point in the mission, enabling the acquisition of high-spatial-resolution data. For spacecraft altitudes below 350 kilometers, NAC images are acquired with pixel scales ranging from 20 meters to as little as 2 meters.
Date acquired: July 19, 2014
Image Mission Elapsed Time (MET): 48103544
Image ID: 6712882
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 72.72°
Center Longitude: 313.7° E
Resolution: 17 meters/pixel
Scale: This image is about 9 km (5.5 miles) across.
Incidence Angle: 78.6°
Emission Angle: 0.3°
Phase Angle: 78.9°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Today's image shows an area in Mercury's northern latitudes crossed by a series of MASCS VIRS tracks displayed as a color composite, overlain on a MDIS base map mosaic. Craters Verdi and Janáček reside in this area, along with several unnamed craters. The VIRS footprints are smaller, each covering less area, in the northern hemisphere due to MESSENGER's elliptical orbit.
The VIRS composite shows hundreds of individual footprints tracks (minimum 100-200 m across and 3-4 km long) taken from different directions and altitudes. In locations where multiple footprints cover the same area, the footprint with the best illumination for mineralogical interpretation (usually the lowest incidence angle where shadows are minimized) is used for making the map. In the MDIS mosaic, some brightness variations are due to tiling of images taken at different illuminations.
Date Created: July 27, 2014
Instruments: Visible and Infrared Spectrograph (VIRS) of the Mercury Atmosphere and Surface Composition Spectrometer (MASCS) and Mercury Dual Imaging System (MDIS)
VIRS Color Composite Wavelengths: 575 nm as red, 415 nm/750 nm as green, 310 nm/390 nm as blue
Center Latitude: 57.7°
Center Longitude: 197.5° E
Resolution: 1 km/pixel
Scale: Verdi (top left) crater is 145 km (90 miles) in diameter
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This high-resolution image features hollows within an unnamed crater. Hollows often have bright halos and usually form in or around craters. Here, the hollows are forming on the crater floor, along the base of the crater wall, and on the top of the central peak.
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: October 13, 2012
Image Mission Elapsed Time (MET): 258630853
Image ID: 2758246
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 50.63°
Center Longitude: 320.6° E
Resolution: 15 meters/pixel
Scale: This image is about 16 km (10 miles) across.
Incidence Angle: 76.8°
Emission Angle: 15.0°
Phase Angle: 91.9°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Today's image shows three oblique mosaics of Hokusai, a complex crater in Mercury's northern hemisphere. The top mosaic features a view of Hokusai where north is to the left. The bottom left is a color mosaic that also has north to the left. In the bottom right is mosaic with a high incidence angle where north is now to the right. The high incidence angle emphasizes topography differences because the sun's low angle creates long shadows. Evident in all of these mosaics are Hokusai's smooth impact melt covered floor, central peak, ejecta blanket, and terraced walls.
The top mosaic 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.
The bottom left color 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.
The bottom right mosaic was acquired as part of MDIS's high-incidence-angle base map. The high-incidence-angle base map complements the surface morphology base map of MESSENGER's primary mission that was acquired under generally more moderate incidence angles. High incidence angles, achieved when the Sun is near the horizon, result in long shadows that accentuate the small-scale topography of geologic features. The high-incidence-angle base map was acquired with an average resolution of 200 meters/pixel.
Instruments: Wide Angle Camera (WAC) and Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
WAC filters: 9, 7, 6 (996, 748, 433 nanometers) in red, green, and blue for color mosaic
Center Latitude: 57.66°
Center Longitude: 16.58° E
Scale: Hokusai is about 85 km (53 miles) in diameter.
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This image, located north of Rachmaninoff, features a possible volcanic vent to the east and an expanse of terrain that appears blue in this color view to the west. The depression's orange-yellow color and irregular shape are similar to other possible volcanic vents on Mercury. To the west of the large vent is a crater with an orange, irregularly shaped depression on its floor that may also be a vent. Vents on Mercury are indicative of explosive volcanism that was prevalent in Mercury's past.
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: July 03, 2014
Image Mission Elapsed Time (MET): 46686728, 46686748, 46686732
Image ID: 6612580, 6612585, 6612581
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: 36.10°
Center Longitude: 54.93° E
Resolution: 215 meters/pixel
Scale: The crater with a possible vent on its floor is about 20 km (12.4 miles) in diameter.
Incidence Angle: 40.6°
Emission Angle: 39.4°
Phase Angle: 78.0°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Today's image features a small, simple impact crater on Mercury's northern plains. The superimposed track is a set of altimetry measurements by the Mercury Laser Altimeter (MLA) that resolves the bowl-shaped morphology characteristic of simple craters. This morphology is evident in the topographic profile on the right of this image that displays how the crater's depth changes from point A to point B.
Instrument: Mercury Laser Altimeter (MLA)
MLA Track: MLASCIRDRAPLFN1112211457
Crater's Center Latitude: 78.1°
Crater's Center Longitude: 327.5° E
Scale: The crater has a diameter of 4.53 km (2.81 miles)
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Rikyü is an impact crater named for Sen no Rikyü, the master who was central in the development of the Japanese tea ceremony. Rikyü sits in Mercury's northern plains and is expected to host water ice because of its persistently shadowed interior and radar-bright signature. Today's image features a northwestern segment of the crater wall, where a 4.1 km-wide simple crater has resulted from an impact on Rikyü's rim. This high-resolution image also provides a fantastic view of the tiny craters that mark the crater's wall.
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: August 04, 2012
Image Mission Elapsed Time (MET): 252610116
Image ID: 2330144
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 80.17°
Center Longitude: 335.4° E
Resolution: 13 meters/pixel
Scale: The simple crater in the lower left corner is approximately 4.1 km wide (2.5 miles)
Incidence Angle: 82.8°
Emission Angle: 44.8°
Phase Angle: 127.6°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Today's color image features a small crater in Mercury's northern hemisphere. This relatively young crater is highlighted by its striking white rays, which contrast the darker, surrounding terrain of low reflectance material. The bright rays result from fine-grained and relatively unweathered material that was ejected and deposited by the 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: July 08, 2014
Image Mission Elapsed Time (MET): 47178430, 47178426, 47178424
Image ID: 6647334, 6647332, 6647331
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: 43.97°
Center Longitude: 34.76° E
Resolution: 348 meters/pixel
Scale: The crater on the right of this image is approximately 16 km (10 miles) across
Incidence Angle: 45.9°
Emission Angle: 1.6°
Phase Angle: 44.9°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Today's video is a MASCS VIRS raster scan of Lermontov in Mercury's mid latitudes. Raster scans return a large number of spectra for targeted areas of interest. This movie was created from 258 VIRS spectra, taken 1 to 5 seconds apart. The VIRS color composite has been overlain on an MDIS image of Lermontov, showing that the crater center is red and thus brighter at longer wavelengths compared to the average Mercury terrain.
The VIRS composite shows hundreds of individual footprints tracks (minimum 100-200 m across and 3-4 km long) taken from different directions and altitudes. In locations where multiple footprints cover the same area, the footprint with the best illumination for mineralogical interpretation (usually the lowest incidence angle where shadows are minimized) is used for making the map.
Date Observed: August 8, 2013
Date Created: July 29, 2014
Instruments: Visible and Infrared Spectrograph (VIRS) of the Mercury Atmosphere and Surface Composition Spectrometer (MASCS) and Mercury Dual Imaging System (MDIS)
VIRS Color Composite Wavelengths: 575 nm as red, 415 nm/750 nm as green, 310 nm/390 nm as blue
Initial Latitude of Scan: 14.0°
Initial Longitude of Scan: 310.8° E
Final Latitude of Scan: 17.8°
Final Longitude of Scan: 310.0° E
Resolution: 0.25 km/pixel
Scale: Lermontov is 166 km (103 mi.) in diameter
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The left column of images shows MASCS VIRS interpolated color composites of Kertesz (top), Dominici (middle), and an unnamed crater (bottom). The middle column shows the VIRS color composite of spectral footprints, and the left column shows monochrome MDIS images for the same areas. Yellow areas are highly reflective and thought to be relatively young, exhibiting fewer effects of space weathering. Kertesz and Dominici are also known to contain hollows, which are shallow depressions with younger surfaces likely caused by the loss of volatiles.
The VIRS composite shows hundreds of individual footprints tracks (minimum 100-200 m across and 3-4 km long) taken from different directions and altitudes. In locations where multiple footprints cover the same area, the footprint with the best illumination for mineralogical interpretation (usually the lowest incidence angle where shadows are minimized) is used for making the map. Where footprints are sparse, interpolation is required for full spatial coverage.
Date Created: July 28, 2014
Instruments: Visible and Infrared Spectrograph (VIRS) of the Mercury Atmosphere and Surface Composition Spectrometer (MASCS) and Mercury Dual Imaging System (MDIS)
VIRS Color Composite Wavelengths: 575 nm as red, 415 nm/750 nm as green, 310 nm/390 nm as blue
Center Latitudes: 27.3° (top); 1.18° (middle); -3.6° (bottom)
Center Longitudes: 146.1° E (top); 323.5° E (middle); 60.9° E (bottom)
Resolution: 0.5 km/pixel
Scale: Kertesz crater (top) has a diameter of 32 km (20 mi.); Dominici crater (middle) has a diameter of 20 km (12 mi.)
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The top image is a MASCS VIRS color composite of Rembrandt, Mercury's second largest impact basin. The bottom image is a MDIS color mosaic of the same area. Rembrandt's rim appears blue in both images, indicating low reflectance relative to its center in the VIRS image. Some small, fresh craters appear in yellow and are highly reflective in VIRS.
The VIRS composite shows hundreds of individual footprints tracks (minimum 100-200 m across and 3-4 km long) taken from different directions and altitudes. In locations where multiple footprints cover the same area, the footprint with the best illumination for mineralogical interpretation (usually the lowest incidence angle where shadows are minimized) is used for making the map.
Date Created: July 27, 2014
Instruments: Visible and Infrared Spectrograph (VIRS) of the Mercury Atmosphere and Surface Composition Spectrometer (MASCS) and Mercury Dual Imaging System (MDIS)
VIRS Color Composite Wavelengths: 575 nm as red, 415 nm/750 nm as green, 310 nm/390 nm as blue
MDIS Color Wavelengths: 1000nm as red, 750nm as green, 430 as blue
Center Latitude: -34.3°
Center Longitude: 87.2° E
Resolution: 1 km/pixel
Scale: Rembrandt is 715 km (444 mi.) in diameter
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This movie consists of 214 images acquired by MESSENGER's Narrow Angle Camera (NAC) on June 8, 2014. The NAC field of view looks toward the horizon along the direction of spacecraft motion as the probe crossed the terminator into night. This view is what a traveler on the MESSENGER spacecraft might see during low-altitude operations over the next eight months. During the final phase of its mission, MESSENGER's science instruments will use low-altitude operations like this to explore the surface and subsurface of Mercury at unprecedented resolution.
The image frames were taken once per second while MESSENGER was at altitudes ranging from 115 to 165 kilometers, traveling at a speed of 3.7 kilometers per second relative to the surface. The movie is sped up by a factor of seven for ease of viewing. The images have resolutions ranging from 21 to 45 meters/pixel. Higher-resolution images of Mercury's surface are possible if the camera is pointed directly below the spacecraft rather than looking to the horizon, and such operations are the routine approach for low-altitude imaging. To observe an aerial view of MESSENGER's flight path, see PIA18637. To look closely at the flight path imagery, see PIA18636.
Date acquired: June 8, 2014
Image Mission Elapsed Time (MET): 44519827-44520005
Image ID: 6458912-6459090
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Initial Center Latitude: 77.2°
Initial Center Longitude: 78.1° E
Final Center Latitude: 79.2°
Final Center Longitude: 193.6° E
Resolution: 21 meters/pixel-45 meters/pixel
Scale: The first image is approximately 10.5 km (6.5 miles) across
Incidence Angle: 80.0°-87.6°
Emission Angle: 78.4°-83.5°
Phase Angle: 66.3°-66.4°
Video credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This image features an elongated impact crater north of Rembrandt impact basin. This crater was most likely formed by a oblique impact (less than 15 degrees from the horizontal), which created the crater's distinct elongated shape and central peak. This crater's rays have faded over time due to space weathering, but when they were still visible, they would have formed a butterfly pattern from the crater's rim.
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: July 04, 2014
Image Mission Elapsed Time (MET): 46777429
Image ID: 6618818
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: -18.60°
Center Longitude: 95.44° E
Resolution: 162 meters/pixel
Scale: The oblong impact is about 34.2 km (21.3 miles) long and 19.3 km (12 miles) wide.
Incidence Angle: 65.0°
Emission Angle: 31.8°
Phase Angle: 41.1°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This image is one of the highest resolution images taken by the MESSENGER spacecraft to date. It features a field of secondary craters in Mercury's northern smooth plains. Secondary craters are formed by the re-impact of debris strewn from a larger crater. The largest secondary craters in this image are roughly a few hundred meters across. If you look closely, you can see some small craters that are only tens of meters across. All of these craters are simple craters.
This image was acquired as part of the MDIS low-altitude imaging campaign. During MESSENGER's second extended mission, the spacecraft makes a progressively closer approach to Mercury's surface than at any previous point in the mission, enabling the acquisition of high-spatial-resolution data. For spacecraft altitudes below 350 kilometers, NAC images are acquired with pixel scales ranging from 20 meters to as little as 2 meters.
On 25 July 2014, MESSENGER moved closer to Mercury than any spacecraft has before, dropping to an altitude of 100 kilometers (60 miles) above the planet's surface. By 19 August 2014, the minimum altitude will be cut in half, to only 50 kilometers (31 miles)! MESSENGER will execute three more orbit-correction maneuvers in order to delay the end of mission to late March 2015. For more details on this event, read this news story.
Date acquired: June 11, 2014
Image Mission Elapsed Time (MET): 44779109
Image ID: 6477542
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 69.84°
Center Longitude: 48.47° E
Resolution: 2.9 meters/pixel
Scale: This image is about 3 km (1.8 miles) across.
Incidence Angle: 79.4°
Emission Angle: 0.1°
Phase Angle: 79.6°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
This color view of Raditladi gives us a fresh view of the peak-ring basin. The bright hollows of Raditladi stand out in white along the peak ring against the smooth crater floor. These shallow depressions may result from the loss of volatile materials. Today's image also shows the darker ejecta of a crater that impacted the basin just above the southern peak-ring structure. The darker material was likely excavated during the small crater's 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: June 22, 2014
Image Mission Elapsed Time (MET): 45761752, 45761748, 45761746
Image ID: 6547149, 6547147, 6547146
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: 28.37°
Center Longitude: 120.3° E
Resolution: 732 meters/pixel
Scale: Raditladi crater has a diameter of 257.7 km (160.1 miles)
Incidence Angle: 57.3°
Emission Angle: 38.5°
Phase Angle: 89.4°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Today's image features Laxness, a crater on Mercury's northern plains named for Halldör Laxness, a twentieth-century Icelandic writer. The overlain MLA track bisecting Laxness reveals the crater's topography, which is difficult to resolve in images because of the crater's persistently shadowed interior. On the right of the image is a cross-section of Laxness showing how the crater's depth changes from point A to point B. The MLA data show that Laxness is a complex crater with a central peak (light blue). While the crater's central peak is not obvious in the Mercury Dual Imaging System (MDIS), it is clearly distinguishable to MLA.
Instrument: Mercury Laser Altimeter (MLA)
MLA Track: MLASCIRDRAPLFN1202071801
Crater's Center Latitude: 83.3°
Crater's Center Longitude: 310.0° E
Scale: The crater has a diameter of 25.9 km (16.1 miles)
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Today's image features the sharp rim of an unnamed complex crater on Mercury. Both the terrain outside the crater's rim and the floor of the crater are marked with small craters, easy to spot in this high-resolution image at a pixel scale of 15 meters. The wall of the crater, however, is relatively smooth, as material has slumped onto the floor.
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: May 05, 2012
Image Mission Elapsed Time (MET): 244718181
Image ID: 1769016
Instrument: Narrow Angle Camera (NAC) of the Mercury Dual Imaging System (MDIS)
Center Latitude: 66.99°
Center Longitude: 227.6° E
Resolution: 15 meters/pixel
Scale: The image is approximately 7.7 km (4.8 miles) across
Incidence Angle: 68.6°
Emission Angle: 1.6°
Phase Angle: 70.3°
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The top image is a MASCS VIRS interpolated color composite of craters Munch and Sander (center), with Poe toward the east. These craters are in the north of Caloris basin. The center image is a MASCS color composite showing individual spectral footprints. The bottom image is a monochrome MDIS mosaic of the same area. The three crater rims are blue, indicating low reflectance. Sander's floor is yellow, however, which is high reflectance and indicative of fresh material.
The VIRS composite shows hundreds of individual footprints tracks (minimum 100-200 m across and 3-4 km long) taken from different directions and altitudes. In locations where multiple footprints cover the same area, the footprint with the best illumination for mineralogical interpretation (usually the lowest incidence angle where shadows are minimized) is used for making the map. In areas where footprints are sparse (separated by tens of km), observations are interpolated for complete coverage of the surface. This is particularly true in the northern hemisphere, where Caloris is located. In the MDIS mosaic, some brightness variations are due to tiling of images taken at different illuminations.
Date Created: June 16, 2014
Instruments: Visible and Infrared Spectrograph (VIRS) of the Mercury Atmosphere and Surface Composition Spectrometer (MASCS) and Mercury Dual Imaging System (MDIS)
VIRS Color Composite Wavelengths: 575 nm as red, 415 nm/750 nm as green, 310 nm/390 nm as blue
Center Latitude: 42.5°
Center Longitude: 154.5° E
Resolution: 1 km/pixel
Scale: Sander crater (center) is about 50 km (31 mi.) in diameter.
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
The top image is a MASCS VIRS color composite of Waters crater (center) in Mercury's mid latitudes. The bottom image is a monochrome MDIS mosaic of the same area. The central blue area corresponds to both Waters and its impact melt flow. The encompassing yellow area likely relates to Waters' ejecta blanket. Blue areas indicate low reflectance, while yellow areas relate to high reflectance and newer material.
The VIRS composite shows hundreds of individual footprints tracks (minimum 100-200 m across and 3-4 km long) taken from different directions and altitudes. In locations where multiple footprints cover the same area, the footprint with the best illumination for mineralogical interpretation (usually the lowest incidence angle where shadows are minimized) is used for making the map. In the MDIS mosaic, some brightness variations are due to tiling of images taken at different illuminations.
Date Created: July 7, 2014
Instruments: Visible and Infrared Spectrograph (VIRS) of the Mercury Atmosphere and Surface Composition Spectrometer (MASCS) and Mercury Dual Imaging System (MDIS)
VIRS Color Composite Wavelengths: 575 nm as red, 415 nm/750 nm as green, 310 nm/390 nm as blue
Center Latitude: -9.1°
Center Longitude: 254.6° E
Resolution: 0.5 km/pixel
Scale: Waters crater (center) is about 15 km (9.3 mi.) in diameter.
Image credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington
Posts
