Data Set Information
|
DATA_SET_NAME |
CLEMENTINE HIRES MOSAIC
|
DATA_SET_ID |
CLEM1-L-H-5-DIM-MOSAIC-V1.0
|
NSSDC_DATA_SET_ID |
94-004A-06A
|
DATA_SET_TERSE_DESCRIPTION |
Clementine High Resolution Lunar Mosaic
|
DATA_SET_DESCRIPTION |
Data Set Overview
=================
This CD contains portions of the Clementine HiRes Lunar Mosaic, a
geometrically controlled, calibrated mosaic compiled from
non-uniformity corrected, 750 nanometer ('D') filter high
resolution observations from the HiRes imaging system onboard the
Clementine Spacecraft. These mosaics cover sub-polar regions
between 80 deg S and 80 deg N with the sinusoidal equal area
mapping at 20 m/pixel, and the polar regions above 80 deg with a
stereographic mapping at 30 m/pixel resolution at the poles. The
geometric control is provided by the 100 m/pixel USGS Clementine
Basemap Mosaic (PDS CD-ROM Volumes CL_3001-3015) compiled from
the 750 nm Ultraviolet/Visible Clementine imaging system and, for
the polar mosaics, from the 150 m/pixel polar basemap mosaic.
Calibration was achieved by removing image nonuniformity largely
due to the HiRes system's light intensifier. Also provided are
offset and scale factors which transform the 8-bit HiRes data to
approximate photometric units, achieved by a fit of the HiRes
data to the corresponding UV/Vis basemap, which is
photometrically calibrated.
The mosaic on this CD covers polar regions above 80 degrees. The
mosaics are divided into square tiles 2250 pixels on a side,
which spans approximately 2.2 degrees.
This CD also contains ancillary data files that support the HiRes
Mosaic. These files include browse images with UV/Vis context
stored in a JPEG format, HTML documents that support a web
browser interface to the CDs, index files ('imgindx.tab' and
'srcindx.tab') that tabulate the contents of the CD, and
documentation files. For more information on the contents and
organization of the CD volume set refer to the 'FILES,
DIRECTORIES AND DISK CONTENTS' section of this document.
Using a web browser open the 'index.htm' file located in the
'root' directory of the CD. The html document will direct you to
other informational documents and the image browser for rapidly
viewing the image collection.
Parameters
==========
N/A
Processing
==========
Processing proceeded an orbital and latitude 'bin' basis,
reflecting the organization of the Clementine EDR CDs. A
latitude bin comprises all images of a given orbit deemed to fall
within a 10 degree latitude range based on SPICE information.
The latitude ranges are defined to fall on on 10-degree
boundaries from -90 to +90. For the sub-polar mosaics, map
projection of images from a given orbit used the same central
longitude, taken to be the orbit's longitude at the lunar
equator. Images used in the polar mosaics were warped to a
common stereographic projection relative to the pertinent pole.
The HiRes Mosaic processing comprised 5 steps: (1) Image
calibration, map project and basemap generation; (2) Low
resolution registration against the UV/Vis basemap; (3) High
resolution registration against overlapping images; (4)
Constrained placement combining high- and low-resolution
registrations; and (5) HiRes mosaic and photometric calibration
estimation.
Placement and calibration for the polar mosaics differed in some
regards from those of the sub-polar mosaics. Due to illumination
paucity, various polar locales lacked useful geometric and
photometric control. In these regions, registration between
individual HiRes frames, both with and among orbits, was the
primary placement guide. Such placement was anchored to images
which did have reliable registration against the UV/Vis basemap.
For convenience, rectangular zones centered on the poles were
defined within which placement proceeded in this manner.
Similarly, the basemap photometric calibration was considered
unreliable at the highest latitudes, and so for a given HiRes
polar mosaic, a single calibration (based on well-illuminated
tiles and basemap portions) was adopted for the entire mosaic,
rather than defining one for each individual tile.
Media/Format
============
The Clementine basemap is delivered to the Planetary Data System
using CD media. Formats are based on standards for such products
established by the Planetary Data System (PDS) [PDSSR1992].
|
DATA_SET_RELEASE_DATE |
1998-09-12T00:00:00.000Z
|
START_TIME |
1994-01-01T12:00:00.000Z
|
STOP_TIME |
N/A (ongoing)
|
MISSION_NAME |
DEEP SPACE PROGRAM SCIENCE EXPERIMENT
|
MISSION_START_DATE |
1991-11-19T12:00:00.000Z
|
MISSION_STOP_DATE |
1994-05-07T12:00:00.000Z
|
TARGET_NAME |
MOON
|
TARGET_TYPE |
SATELLITE
|
INSTRUMENT_HOST_ID |
CLEM1
|
INSTRUMENT_NAME |
LIDAR HIGH-RESOLUTION IMAGER
|
INSTRUMENT_ID |
HIRES
|
INSTRUMENT_TYPE |
CAMERA
|
NODE_NAME |
Imaging
|
ARCHIVE_STATUS |
ARCHIVED
|
CONFIDENCE_LEVEL_NOTE |
Confidence Level Overview
=========================
Geometric Accuracy
------------------
The geometric placement of the HiRes Mosaics is based primarily
on registration with the Clementine Basemap Mosaic, which has
accuracies approaching the UV/Vis scale. The UV/Vis accuracy
is discussed below, drawing extensively from the UV/Vis Basemap
Mosaic documents.
The goal of the UV/Vis basemap was for 95% of the Moon
(excluding the oblique observation gap fills) to have better
than 0.5 km/pixel absolute positional accuracy and to adjust
the camera angles so that all frames match neighboring frames
to within an accuracy of 2 pixels.
Approximately 265,000 match points were collected at the USGS
from ~43,000 UV/Vis images, providing global coverage. About
80% of these points were collected via autonomous procedures,
whereas the 20% required the more time consuming but highly
accurate manual pattern-recognition. The oblique gap-fill
images were the most difficult to match, and required
substantial human intervention. Matching the polar regions was
time-consuming because each frame overlaps many other frames.
Most match points were found to a precision of 0.2 pixels.
The USGS match points were sent to RAND corporation for
analytical triangulations. Using these match points, control
points from the Apollo region, and the latest NAIF/SPICE
information, RAND determined improved camera orientation angles
for the global set of UV/Vis images. A spherical Moon of
constant radius (1737.4 kilometers) was assumed, which was a
significant source of error near the oblique gap fills. The
analytical triangulation is a least-squares formulation
designed to adjust the latitude and longitude of the control
points and the camera orientation angles to best fit the match
points. The final (global) analytical triangulation required
solving ~660,000 normal equations. The mean error is less than
1 pixel. This is by far the largest analytical triangulation
ever applied to a planetary body other than Earth. The results
fully define the planimetric geometry of the basemap, to which
future systematic products, such as the present HiRes Mosaic,
should be tied.
Accurate placement of the map-projected HiRes images was
accomplished by combining registration to the UV/Vis basemap at
the basemap's resolution (100 m/pixel and 150 m/pixel) with
registration of overlapping HiRes pairs at five times this
resolution (20 m/pixel and 30 m/pixel). The registrations were
facilitated with automated image correlation. These
registrations were combined in a Least Absolute Deviation fit
[BARRODALE1980] constrained to stray no further than some small
amount from the basemap-scale registration. Use of the least
absolute deviation gives outliers less importance than does a
least squares fit. Further manual placement of 1-5 percent of
the image was required; these were due either to poor initial
placement, particularly when the scene was featureless and
provided few or no overlapping features with the UV/Vis
basemap, or to mismatches of scene, resolution or illumination
across seams in the UV/Vis mosaic. Some misregistration of
adjacent HiRes images remains in the final mosaic because the
paramount goal was registration with the underlying UV/Vis
Basemap Mosaic.
As described above, the HiRes polar mosaics lacked Uv/Vis
basemap registration in shadowed regions, most notably at and
immediately adjacent to the poles. In such locales, the
placment of HiRes images was guided primarily by registration
of individual HiRes frames within and among orbits. Such
placement was applied within approximately 2 degrees of the
poles.
Radiometric Units
=================
To date, absolute photometric calibration of the HiRes image data
remains elusive. This seems particularly problematic for the
bulk of HiRes images, which were noisy due to the low gain
setting intended to extend the lifetime of the imaging system.
For these reasons, a piece-wise intensity matching of the HiRes
Mosaics to the UV/Vis Basemap Mosaic was adopted as an
approximate radiometric calibration. The further decision was
made to use 750 nm ('D') filter HiRes images in order to best
match the UV/Vis Basemap Mosaic, which dominantly comprises 750
nm ('B') filter images. A more detailed description of the
UV/Vis basemap photometric calibration may be found on the UV/Vis
basemap volumes CL_30XX.
Whereas sub-polar HiRes tiles were individually calibrated
against the underlying UV/Vis basemap, each of the four HiRes
polar mosaics have a single calibration for all tiles. This is
due to the difficulties associated with calibrating regions
perennially in shadow, which renders some portions of the
underlying polar basemap calibration unreliable. To mitigate
this problem, a well-illuminated tile and basemap portion near 85
deg latitude from each mosaic was adopted as calibration
references.
This calibration is embodied by the header values of the OFFSET
and SCALING_FACTOR entries, which defines HiRes fractional
reflectances:
OFFSET
where: DN = 8-bit pixel value of HiRes mosaic image array.
SCALING_FACTOR units are fractional reflectance per DN
OFFSET units are fractional reflectance
The calibration in every case included correction for the
non-uniformity of the raw HiRes images due to the light
intensifier.
|
CITATION_DESCRIPTION |
Citation TBD
|
ABSTRACT_TEXT |
This CD contains portions of the Clementine HiRes Lunar Mosaic, a
geometrically controlled, calibrated mosaic compiled from
non-uniformity corrected, 750 nanometer ('D') filter
high resolution observations from the HiRes imaging system
onboard the Clementine Spacecraft. These mosaics cover sub-polar
regions between 80 deg S and 80 deg N with the sinusoidal equal
area mapping at 20 m/pixel, and the polar regions above 80 deg
with a stereographic mapping at 30 m/pixel resolution at the
poles. The geometric control is provided by the 100 m/pixel USGS
Clementine Basemap Mosaic (PDS CD-ROM Volumes CL_3001-3015)
compiled from the 750 nm Ultraviolet/Visible Clementine imaging
system and, for the polar mosaics, from the 150 m/pixel polar
basemap mosaic. Calibration was achieved by removing image
nonuniformity largely due to the HiRes system's light
intensifier. Also provided are offset and scale factors which
transform the 8-bit HiRes data to approximate photometric units,
achieved by a fit of the HiRes data to the corresponding UV/Vis
basemap, which is photometrically calibrated.
|
PRODUCER_FULL_NAME |
DR. MICHAEL C. MALIN
|
SEARCH/ACCESS DATA |
Lunar Orbital Data Explorer
Imaging Planetary Image Atlas
Imaging Online Data Volumes
|
|