Lunar and Planetary Science XXX 1812.pdf CLEMENTINE: A … · 2000-04-21 · The single-band design...
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CLEMENTINE: A MULTI-SPECTRAL DIGITAL IMAGE MODEL ARCHIVE OF THE MOON. Chris E. Isbell 1 , Eric M. Eliason 1 , Kevin C. Adams 1 , Tammy L. Becker 1 , Annie L. Bennett 1 , Ella M. Lee 1 , Alfred McEwen 2 , Mark Robinson 3 , John Shinaman 1 , Lynn A. Weller 1 , 1 U.S. Geological Survey, 2255 N. Gemini Drive, Flagstaff, AZ 86001; 2 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721; 3 Northwestern University, Dept. of Geol. Sciences, Evanston, IL 60205 Summary A multi-spectral global Digital Image Model (DIM) [1] of the Moon containing controlled image mosaics has been compiled by the U.S. Geological Survey for distribution through Internet services and CD-ROM optical disk media. This database is the product of an exhaustive lunar cartography project based on data from the Clementine Mission [2]. The lunar multi- spectral DIM is a radiometrically and geometrically controlled, photometrically modeled global image mo- saic at a resolution of 100 meters per pixel. The image model contains the five spectral observations acquired by the Clementine Ultra-Violet Visible (UVVIS) cam- era. A phase angle image database, at equivalent reso- lution, accompanies the UVVIS DIM. The carto- graphic design of this database is equivalent to the pre- viously published mono-spectral UVVIS 750-nm basemap [3]. Current project work will also produce a multi-spectral lunar DIM containing the 6-band com- plement of the Clementine Near Infrared (NIR) cam- era. The UVVIS Lunar DIM, organized on 78 CD vol- umes and available through the Planetary Data System Imaging Node, is expected to provide continued sup- port for lunar science investigations and also for scien- tific and engineering operations of future expeditions to the Moon. Introduction The Clementine Mission acquired nearly 1.7 mil- lion raw images covering virtually 100% of the lunar surface in 11 spectral bandpasses from 415 to 2792 nm and at resolutions from 80-330 meters/pixel [4]. Utili- zation of a subset of these raw images resulted in a previously released lunar DIM. This single band DIM was archived on CD-ROM by the U.S. Geological Sur- vey (USGS) and is available from the Planetary Data System (PDS) Imaging Node [5] (www- pdsimage.jpl.nasa.gov/PDS/). The single band base map contained only the 750-nm wavelength filter im- ages acquired by the Clementine UVVIS camera. In order to facilitate the continued use of the Clementine imaging data, the multi-band UVVIS DIM has been created. All systematic processing steps needed to characterize the spectral properties of the data have been applied. This 5-band global DIM product, and phase angle information, generated at a resolution of 100 meters per pixel (~303 pixels/degree), with each pixel stored as a 16-bit integer, results in a ~66 giga- byte data set. Ancillary data such as index catalog files and complete documentation are included in support of the DIM products. A graphical user interface, a Hy- pertext Markup Language (HTML) document, provides computer users with multi-platform access to the lunar DIM, color and ratio browse imagery, and documenta- tion provided within the archive. The complete archive collection consists of 78 CD-ROM volumes. A modi- fied tiling scheme for reduced resolution products, re- quiring 4 additional CD volumes, completes the data set. Our goal is to provide a valuable and useful re- source to the planetary science community. Clementine UVVIS Digital Image Model The Integrated Software for Imagers and Spec- trometers (ISIS) [6] processing system, developed by the USGS, was used to generate the Lunar UVVIS DIM. Processing within ISIS includes radiometric and geometric correction, spectral registration for image cubes, photometric normalization, and image mo- saicking. For Clementine data, radiometric correction involves “flat fielding,” dark current subtraction, non- linearity correction, and conversion to radiometric units [7]. Geometric transformations tie each raw im- age with the lunar ground control network [8, 9] and convert from raw image coordinates to DIM map pro- jection coordinates. Photometric normalization is ap- plied to balance brightness variations due to illumina- tion differences between Clementine images. This is a brief summary of ISIS processing capabilities in re- gards to DIM generation; a more detailed description is available in [10]. Through these processes, the planet- wide UVVIS map was generated using approximately 250,000 images acquired by the UVVIS camera. If the resulting 100-meter/pixel UVVIS DIM were presented as a single file, it would constitute a 3-dimensional image array with 5 bands, each approximately 110,000 samples by 55,000 lines in cylindrical geometry, far too cumbersome for most users. The Lunar UVVIS DIM has therefore been formatted in 996 sub-areas or “tiles” equivalent to those defined in the previously released 750-nm UVVIS base map [3]. Although the tiling schemes are equivalent, the multi-spectral DIM requires a new archive design. The single-band design now becomes a "6-band" implementation (5-bands plus phase angle for UVVIS and 6-bands for the NIR data set). The 30° “zone” of the single band base map is now divided into six sets of quadrangles such that each set completes a 650 megabyte CD volume (Figure 1). Cartographic, digital space storage, and end user data retrieval considerations determined the archive design and tiling scheme. Current project work will also pro- vide a future release of an additional multi-spectral lunar DIM containing the 6 spectral bands available from the Clementine Mission NIR camera. The NIR Lunar and Planetary Science XXX 1812.pdf
Transcript of Lunar and Planetary Science XXX 1812.pdf CLEMENTINE: A … · 2000-04-21 · The single-band design...
CLEMENTINE: A MULTI-SPECTRAL DIGITAL IMAGE MODEL ARCHIVE OF THE MOON. Chris E.Isbell1, Eric M. Eliason1, Kevin C. Adams1, Tammy L. Becker1, Annie L. Bennett1, Ella M. Lee1, Alfred McEwen2,Mark Robinson3, John Shinaman1, Lynn A. Weller1, 1U.S. Geological Survey, 2255 N. Gemini Drive, Flagstaff, AZ86001; 2Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721; 3Northwestern University, Dept.of Geol. Sciences, Evanston, IL 60205
SummaryA multi-spectral global Digital Image Model (DIM)
[1] of the Moon containing controlled image mosaicshas been compiled by the U.S. Geological Survey fordistribution through Internet services and CD-ROMoptical disk media. This database is the product of anexhaustive lunar cartography project based on datafrom the Clementine Mission [2]. The lunar multi-spectral DIM is a radiometrically and geometricallycontrolled, photometrically modeled global image mo-saic at a resolution of 100 meters per pixel. The imagemodel contains the five spectral observations acquiredby the Clementine Ultra-Violet Visible (UVVIS) cam-era. A phase angle image database, at equivalent reso-lution, accompanies the UVVIS DIM. The carto-graphic design of this database is equivalent to the pre-viously published mono-spectral UVVIS 750-nmbasemap [3]. Current project work will also produce amulti-spectral lunar DIM containing the 6-band com-plement of the Clementine Near Infrared (NIR) cam-era. The UVVIS Lunar DIM, organized on 78 CD vol-umes and available through the Planetary Data SystemImaging Node, is expected to provide continued sup-port for lunar science investigations and also for scien-tific and engineering operations of future expeditionsto the Moon.
IntroductionThe Clementine Mission acquired nearly 1.7 mil-
lion raw images covering virtually 100% of the lunarsurface in 11 spectral bandpasses from 415 to 2792 nmand at resolutions from 80-330 meters/pixel [4]. Utili-zation of a subset of these raw images resulted in apreviously released lunar DIM. This single band DIMwas archived on CD-ROM by the U.S. Geological Sur-vey (USGS) and is available from the Planetary DataSystem (PDS) Imaging Node [5] (www-pdsimage.jpl.nasa.gov/PDS/). The single band basemap contained only the 750-nm wavelength filter im-ages acquired by the Clementine UVVIS camera. Inorder to facilitate the continued use of the Clementineimaging data, the multi-band UVVIS DIM has beencreated. All systematic processing steps needed tocharacterize the spectral properties of the data havebeen applied. This 5-band global DIM product, andphase angle information, generated at a resolution of100 meters per pixel (~303 pixels/degree), with eachpixel stored as a 16-bit integer, results in a ~66 giga-byte data set. Ancillary data such as index catalog filesand complete documentation are included in support ofthe DIM products. A graphical user interface, a Hy-pertext Markup Language (HTML) document, provides
computer users with multi-platform access to the lunarDIM, color and ratio browse imagery, and documenta-tion provided within the archive. The complete archivecollection consists of 78 CD-ROM volumes. A modi-fied tiling scheme for reduced resolution products, re-quiring 4 additional CD volumes, completes the dataset. Our goal is to provide a valuable and useful re-source to the planetary science community.
Clementine UVVIS Digital Image ModelThe Integrated Software for Imagers and Spec-
trometers (ISIS) [6] processing system, developed bythe USGS, was used to generate the Lunar UVVISDIM. Processing within ISIS includes radiometric andgeometric correction, spectral registration for imagecubes, photometric normalization, and image mo-saicking. For Clementine data, radiometric correctioninvolves “flat fielding,” dark current subtraction, non-linearity correction, and conversion to radiometricunits [7]. Geometric transformations tie each raw im-age with the lunar ground control network [8, 9] andconvert from raw image coordinates to DIM map pro-jection coordinates. Photometric normalization is ap-plied to balance brightness variations due to illumina-tion differences between Clementine images. This is abrief summary of ISIS processing capabilities in re-gards to DIM generation; a more detailed description isavailable in [10]. Through these processes, the planet-wide UVVIS map was generated using approximately250,000 images acquired by the UVVIS camera. If theresulting 100-meter/pixel UVVIS DIM were presentedas a single file, it would constitute a 3-dimensionalimage array with 5 bands, each approximately 110,000samples by 55,000 lines in cylindrical geometry, fartoo cumbersome for most users. The Lunar UVVISDIM has therefore been formatted in 996 sub-areas or“tiles” equivalent to those defined in the previouslyreleased 750-nm UVVIS base map [3]. Although thetiling schemes are equivalent, the multi-spectral DIMrequires a new archive design. The single-band designnow becomes a "6-band" implementation (5-bands plusphase angle for UVVIS and 6-bands for the NIR dataset). The 30° “zone” of the single band base map isnow divided into six sets of quadrangles such that eachset completes a 650 megabyte CD volume (Figure 1).Cartographic, digital space storage, and end user dataretrieval considerations determined the archive designand tiling scheme. Current project work will also pro-vide a future release of an additional multi-spectrallunar DIM containing the 6 spectral bands availablefrom the Clementine Mission NIR camera. The NIR
Lunar and Planetary Science XXX 1812.pdf
MULTI-SPECTRAL DIGITAL IMAGE MODEL ARCHIVE: C. E. Isbell, et al., XXX LPSC
camera acquired images utilizing 1100, 1250, 1500,2000, 2600, and 2780 nm wavelength filters.
The Clementine UVVIS DIM is partitioned on theCD-ROM collection in the Sinusoidal Equal-Areaprojection. The 5-band DIM image cube and phaseangle image are each presented as separate files. Theimage cube contains the spectral bands (415, 750, 900,950, and 1000 nm) acquired by the UVVIS camera.The phase angle image contains the phase (spacecraft-surface-sun) angle value associated with each pixel inthe DIM. The UVVIS DIM design results in a 78-volume archive set containing the full resolution (0.1km/pixel) image model. Four additional CD volumes,containing reduced-resolution planetwide coverage at0.5, 2.5, and 12.5 km/pixel and other ancillary data,complete the archive collection. For each full- and re-duced-resolution UVVIS image product, sub-sampledenhanced color and comparative ratio browse imagesare provided. The enhanced color derivations are pre-sented with the 415, 750, and 950 nm spectral datarepresented respectively as blue, green, and red chan-nels of a 3-color digital image. The ratio comparisonsare presented with the 415nm/750nm, 750nm/950nm,and 750nm/415nm ratios represented respectively asblue, green, and red channels of a 3-color digital im-age. The browse images are provided in Joint Photo-graphic Experts Group (JPEG) format.
A HTML document provides computer system us-ers a graphical interface to products and informationstored on each archive volume. This document can beused by web browser software to view representativecolor and ratio “browse” images, documentation, andother pertinent information provided on the archive.
In addition to and in support of the lunar UVVISDIM, ancillary information are provided. Documenta-tion and index table files present detailed informationthat describes the data collection. Documentation files,provided in a variety of formats, describe content andbackground details regarding the archive. Index tablesare organized as flat files; each row contains attributeinformation such as cartographic and geometric vari-ables for each image product. These tables can beloaded into catalog and spreadsheet applications foruse in image search and retrieval.
This and other PDS planetary DIM products can bemanipulated by the software tool “MapMaker,” devel-oped by and available from the PDS Imaging Node(www-pdsimage.jpl.nasa.gov/PDS/). MapMaker en-ables users to create seamless mosaics derived from
DIM tiles. User defined output parameters withinMapMaker allow for selection of latitude and longitudelimits, image resolution, and various map projections.
Figure. 1. This 30°-longitude section illustrates thetiling and CD archive scheme used for the 100 me-ter/pixel Lunar UVVIS DIM. Bold lines indicate CDvolume boundaries. The representation is rotationallysymmetric about the equator and can be repeated eastand west beginning at 0° longitude.
References: [1] Batson, R.M. (1987) Photogrammetric Engineering and Remote Sensing, 53, 1211-1218. [2]Nozette, S. et al. (1994) Science, 266, 1835. [3] Isbell, C.E. et al. (1997) LPS XXVIII, 623-624. [4] McEwen, A.S.,Robinson, M.S. (1996) Mapping of the Moon by Clementine, Advances in Space Research. [5] Eliason, E.M. et al.(1995) LPS, XXVI, 369-370. [6] Torson, J.M. and Becker, K.J. (1997) LPS XXVIII, 1443-1444. [7] McEwen, A.S.,et al. (1998) LPS XXIX, #1466. [8] Davies, et al. (1996) Modern Lunar Geodetic Control, International Moon Work-shop, Berlin. [9] Edwards, K.E. et al. (1996) LPS XXVII, 335-336. [10] Eliason, E.M. et al. (1999), A Global Mul-tispectral Map of the Moon From the Clementine UVVIS Imaging Instrument, This volume.
Lunar and Planetary Science XXX 1812.pdf
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