[meteorite-list] The Imaging Campaigns of MESSENGER's Mercury Dual Imaging System

From: Ron Baalke <baalke_at_meteoritecentral.com>
Date: Wed, 11 May 2011 13:04:57 -0700 (PDT)
Message-ID: <201105112004.p4BK4vN8005046_at_zagami.jpl.nasa.gov>

http://messenger.jhuapl.edu/soc/highlights.html

MESSENGER Science Highlights from Mercury's Orbit
May 10, 2011

The Imaging Campaigns of MESSENGER's Mercury Dual Imaging System

As the first spacecraft to orbit the planet Mercury, MESSENGER has the
opportunity to make many observations of the Solar System's innermost
planet that had not previously been possible. Each of MESSENGER's eight
science investigations has a one-year data collection plan that has been
carefully designed to meet the goal of maximizing the science return for
the mission. MESSENGER's Mercury Dual Imaging System (MDIS)
is composed of two cameras, a wide-angle
camera (WAC) and a narrow-angle camera (NAC). MDIS is scheduled to
acquire more than 75,000 WAC and NAC images during the one-year orbital
mission in support of MESSENGER's science goals. A range of imaging
campaigns achieves a balance between globally mapping the entire surface
of Mercury and obtaining targeted higher-resolution images in support of
specific science goals. Together, MDIS's imaging campaigns will provide
a new view of Mercury and will address one of the mission's main science
questions: What is the geologic history of Mercury?

[Figure 1] A portion of the surface morphology base map. The mosaic is
centered at 22.63?S, 219.71?E, and has a resolution of 216 m/pixel. The
large crater in the center is Valmiki (210 km diameter). Inset globe:
example of planned base map image coverage during a typical week,
showing how mosaics of large regions of the surface are built up from
numerous individual images.

During the first 176 days of the orbital mission, equal to one solar day
on Mercury, MDIS will acquire images to produce a high-resolution base
map for surface morphology (morphology is the term given to the shape
and texture of the surface). This map will cover more than 90% of
Mercury's surface at an average resolution of 250 m/pixel (0.16
miles/pixel or 820 feet/pixel) or better. At this resolution, features
about 1 km in horizontal scale are recognizable in the images. Images
acquired for the surface morphology base map have off-vertical solar
illumination and visible shadows so as to reveal clearly the topographic
form of geologic features. Because of MESSENGER's highly elliptical
orbit>, the spacecraft passes close to the
surface at high northern latitudes but is far above the southern
hemisphere, so both the NAC and the WAC are being used to construct the
global base map. For the southern hemisphere, images are obtained with
the NAC, which has a 1.5? field of view and can acquire images at seven
times greater resolution than the WAC. For the northern hemisphere, when
the spacecraft is closer to and moving faster over the surface, the WAC
is used, because its 10.5? field of view enables good image coverage.
Images from both the NAC and the WAC will be mosaicked together to
produce the global map. Shown in Figure 1 is an example mosaic of four
images acquired as part of the surface morphology campaign.


Color Base Map

In addition to the surface morphology base map, MDIS is currently
acquiring a color base map during the mission's first 176 days. The
color base map is composed of WAC images taken through eight different
narrow-band color filters and will cover more than 90% of Mercury's
surface at an average resolution of 1 km/pixel (0.6 miles/pixel) or
better. In contrast to the imaging conditions best suited for seeing
surface topography, the highest-quality color images of Mercury's
surface are obtained when both the spacecraft and the Sun are overhead
and shadows are limited. The eight different color filters of the WAC
that are used to create the color base map have central wavelengths of
430, 480, 560, 630, 750, 830, 900, and 1000 nm. The images acquired
through these narrow-band filters are combined to create color images
that accentuate color differences on Mercury's surface. As an example,
the image in Figure 2 was created by using three images acquired as part
of the color base map with the central wavelengths of 1000, 750, and 430
nm displayed in red, green, and blue, respectively.


[Figure 2] A portion of the color base map. The image is centered at
3.46?S, 275.92?E, and has a resolution of 960 m/pixel. The bright, rayed
crater is Snorri (21 km diameter).

Stereo Base Map

After the surface morphology base map is acquired during the first
Mercury solar day, a second, complementary near-global map, called the
stereo base map, will be acquired during the second Mercury solar day of
MESSENGER's one-year orbital mission. The stereo base map will be used
in combination with the surface morphology base map to create
high-resolution stereo views of Mercury's surface at an average
resolution of 250 m/pixel (0.16 miles/pixel or 820 feet/pixel) or
better. As with the surface morphology base map, images are acquired
under non-vertical solar illumination, so that shadows accentuate the
topography of the surface. In addition, the stereo basemap images are
acquired under viewing angles that differ from those for the morphology
base map by about 20?, allowing stereo information about the surface to
be determined. As the mission is currently in the first Mercury solar
day, no images have yet been acquired in support of the stereo base map.
However, different viewing conditions during MESSENGER's second and
third Mercury flybys allowed stereo information to be obtained for a
portion of Mercury's surface at an image resolution of 500 m/pixel. View
this example of Rembrandt
<http://messenger.jhuapl.edu//gallery/sciencePhotos/image.php?image_id=347>
to see the type of stereo data that will be derived from the two sets of
image base maps.


[Figure 3] Example of south polar monitoring. The resolution is 1.5
km/pixel.

South Polar Monitoring

In addition to the three global base maps, there is an MDIS imaging
campaign to monitor the south polar region of Mercury. By imaging the
south polar region once every four MESSENGER orbits (once every two
Earth days) as illumination conditions change, features that were in
shadow on earlier orbits can be discerned and any permanently shadowed
areas can be identified over one Mercury solar day. Identifying areas of
permanent shadow are of interest to understand the unusual materials at
Mercury's poles and whether these highly
radar-reflective materials consist of water ice. During MESSENGER's
one-year mission, the WAC is used to monitor the polar region south of
70?S at 1.5 km/pixel for the first Mercury solar day. On the second
Mercury solar day, the NAC will be used for imaging the polar region
south of 85?S at 300 m/pixel. An example WAC image acquired as part of
MDIS's south polar monitoring campaign is shown in Figure 3.

[Figure 4] Example of limb imaging. The image is centered at 58.57?S,
308.10?E, and has a resolution of 1.5 km/pixel.

Limb Imaging

Once per week, MDIS captures images of Mercury's limb (the edge of the
sunlit planet with space), with an emphasis on imaging the southern
hemisphere limb. An example of one of those limb images is shown in
Figure 4. The spacecraft was high above Mercury's south polar region
when capturing this image. However, even when the spacecraft is at its
highest altitude above Mercury, a single WAC image cannot capture the
entire limb of Mercury. Consequently, two images are taken and mosaicked
together to image Mercury's entire limb. These limb images will provide
information about Mercury's shape and will complement measurements of
topography made by the Mercury Laser Altimeter (MLA) of Mercury's
northern hemisphere.

[Figure 5] Example of a targeted observation. The image mosaic is
centered at 83.06?N, 290.05?E, and has a resolution of 15 m/pixel. The
inset shows the locations of a number of planned targeted observations
within the floor of the Caloris basin.

Targeted Observations

MDIS also acquires targeted images of small areas on Mercury's surface
at resolutions much higher than those of the morphology, stereo, or
color base maps. It is not possible to cover all of Mercury's surface at
such high resolutions during MESSENGER's one-year primary mission, but
several areas of high scientific interest are generally imaged in this
mode each week. Additionally, as new features of particular science
interest are imaged from orbit, targets are added to a database list and
will be imaged if possible at higher resolution by MDIS, or with
multiple instruments, the next time that area of Mercury is in view from
the spacecraft. Figure 5 shows a mosaic of four images from a targeted
observation acquired at 15 m/pixel, a resolution that is more than an
order of magnitude improvement over the surface morphology base map.
These ultra-high-resolution images are revealing Mercury's surface in
unprecedented detail.

Calibrations

In addition to the science imaging campaigns described above, MDIS also
acquires a few images each week in support of calibration of the
instrument. Some of these images are of star fields, to verify the
pointing of the camera and to assess any changes in instrument
characteristics during the mission. These star images resemble those
acquired in support of the vulcanoid search effort, carried out during
MESSENGER's journey prior to orbit insertion. Other calibration images
include repeated imaging of the same portion of Mercury's surface under
different lighting and viewing geometries. These image sets provide
information about the photometric corrections that must be applied to
compare images acquired under a range of lighting and viewing conditions.
Received on Wed 11 May 2011 04:04:57 PM PDT