Empirical Calibration NIR Moon Clementine 500m v1 (2023)

Luna Clementina Empirical NIR Calibration 500m v1

Product Information:

This mosaic represents a reduced-resolution version of the empirically calibrated near-infrared (NIR) Clementine mosaic processed at a spatial resolution of 500 meters per pixel (m) as an ISIS cube (70°N to 70°S).

Mission and instrument information:

On January 25, 1994, the Deep Space Program Science Experiment (DSPSE), better known as Clementine, launched from Vandenburg Air Force Base aboard a Titan IIG rocket as a joint project and was jointly sponsored. by the Ballistic Missile Defense Organization (BMDO). ) from the Department of Defense and NASA. The objective of the mission was to test sensors and spacecraft components under prolonged exposure to the space environment and to make scientific observations of the Moon and a near-Earth asteroid (1620 Geographos).

Lunar insertion was achieved on February 19 after two flybys of Earth. The lunar mapping was carried out in two systematic mapping passes over the moon over approximately two months. Following the spectacular success of the lunar mapping phase of the mission, on May 7, 1994, Clementine suffered an onboard malfunction that resulted in the activation of her high-altitude engines. This used up all the fuel for altitude control and the spacecraft turned at 80 rpm. The result of the malfunction prevented Clementine from completing the scheduled August 1994 close flyby of the near-Earth asteroid Geographos.

Clementine's main instruments consisted of four cameras, one with a laser range-finding system. The cameras included an ultraviolet visual camera (UVVIS), a long-wavelength infrared (LWIR) camera, a high-resolution laser ranger (LIDAR) camera (HIRES), and a near-infrared (NIR) camera. The spacecraft also carried two star tracking cameras (A-STAR, B-STAR), which were used primarily for attitude determination, but also served as wide-field cameras for various scientific and operational purposes (PDS IMG, 2017). .


Cahill, J. T., Lucey, P. G., Gillis, J. J. y Steutel, D. (2004).Checking the quality and compatibility of the newly calibrated Clementine NIR dataset.Vortrag auf der 35. Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX.https://www.lpi.usra.edu/meetings/lpsc2004/pdf/1469.pdf

Eliason, E.M., Malaret, E. & Bachman, N. (1994). Clementine EDR Image Software Interface (SIS) Specification.https://pds-imaging.jpl.nasa.gov/documentation/clementine_edrsis.pdf

Eliason, E. M., McEwen, A. S., Robinson, M. S., Lee, E. M., Becker, T., Gaddis, L., Weller, L. A., et al. (1999).Digital processing for a global multispectral map of the Moon using the Clementine UVVIS imaging instrument.Vortrag auf der 30. Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX.https://www.lpi.usra.edu/meetings/LPSC99/pdf/1933.pdf

Eliason, E. M., Lee, E. M., Becker, T. L., Weller, L. A., Isbell, C. E., Staid, M. I., Gaddis, L. R., et al. (2003).A global near-infrared (NIR) multispectral map of Clementine's moon.Vortrag auf der 34. Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX.https://www.lpi.usra.edu/meetings/lpsc2003/pdf/2093.pdf

Lucey , P. G. , Hinrichs , J. , Budney , C. , Smith , G. , Frost , C. , Hawke , B. R. , Malaret , E. , et al. (1998).Near Infrared Camera Calibration Clementine: Ready for prime time.Vortrag auf der 29. Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX.https://www.lpi.usra.edu/meetings/LPSC98/pdf/1576.pdf

Lucey , P. G. , Blewett , D. T. , Eliason , E. M. , Weller , L. A. , Sucharski , R. , Malaret , E. , Hinrichs , J. L. , et al. (2000).Optimized calibration constants for the Clementine NIR camera.Vortrag auf der 31. Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX.https://www.lpi.usra.edu/meetings/lpsc2000/pdf/1273.pdf

McEwen, AS and Robinson, MS (1997). Mapping of Clementine's Moon.Advances in space exploration, 19th century(10), 1523-1533.https://doi.org/10.1016/S0273-1177(97)00365-7

Nozette, S., Rustan, P. Pleasance, L.P., Kordas, J.F., Lewis, I.T., Park, H.S., Priest, R.E., et al. (1994). The Clementine Mission to the Moon: Scientific Description.science, 266(5192), 1835-1839.https://www.doi.org/10.1126/science.266.5192.1835

Pieters, C. M. y Pratt, S. (2000).Collecting ground-based near-infrared spectra for the Moon: a new PDS dataset.Vortrag auf der 31. Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX.https://www.lpi.usra.edu/meetings/lpsc2000/pdf/2059.pdf

Planetary Data Systems (PDS) Mapping and Imaging Science (IMG) Nodes (2017). Clementine Mission.https://pds-imaging.jpl.nasa.gov/portal/clementine_mission.html

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In May and June 1994, the NASA/DoD Clementine mission acquired 11-band multispectral global data from the lunar surface using ultraviolet-visible (UVVIS) and near-infrared (NIR) camera systems (eg, Nozette et al. al. 1994; McEwen and Robinson, 1996). The global 5-band UVVIS Digital Imaging Model (DIM) of the Moon at 100 m/pixel was released to the Planetary Data System (PDS) in 2000 (Eliason et al., 1999). The NIR DIM has six spectral bands (1100, 1250, 1500, 2000, 2600 and 2780 nm) and will be available in early 2004 in 996 quads at 100 m/pixel (303 pixels/degree).

This first edition NIR mosaic is processed at 500 m/pixel, has 6 spectral bands, and is presented in a simple cylindrical map projection for the eastern (0° to 180° east) and western (180° to 360° east) lunar hemispheres. . NIR data were radiometrically corrected, geometrically verified for the 750 nm Clementine mosaic, and photometrically normalized to form uniform, illuminated mosaics of the lunar surface. The first four NIR bands (1100 to 2000 nm) were also normalized to reflectance according to the approach previously applied to the calibrated global UVVIS mosaics (Pieters et al., 1999). The 2600nm and 2780nm NIR beams are provided as calibrated Clementine digital numbers (in counts/ms).

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Data status and quality

current reference
release date
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Logical Consistency Report
For these products we have in Lucey et al. the described radiometric camera model is used. (2000) along with one in Eliason et al. (2003). Residual radiometric artifacts remain in these data and are clearly visible when a ratio of two NIR bands is generated. The artifacts are attributed to 1) the radiometric camera model with residual errors in the values ​​associated with the instrument's operating modes (gain, compensation, and exposure values); 2) residual errors present in the thermal background correction; and 3) the shading characteristics of the sensor array change with the thermal conditions of the chamber, which have not been adequately characterized. In addition to extensive radiometric and photometric processing, empirically derived frame shift corrections were applied to create a second version of the global tessellations with reduced variability between camera modes and adjacent orbits. This additional processing resulted in the "empirically corrected" tiles and is described in more detail below. Similar before-and-after comparisons are shown for the Aristarchus Plateau region and the eastern part of the South Pole-Aitken Basin region. Finally, the 1500/2000 nm ratios of the Western Hemisphere and the Aristarchus Plateau are shown to illustrate the magnitude of changes between the calibrated and empirically corrected versions of the NIR mosaics.
full report

-70 to 70 latitude

Process description

Details on the processing of NIR mosaics have been described in several publications: Lucey et al., 1998, LPS XXIX, #1576 (25 KB, PDF); Lucey et al., 2000, LPS XXXI, No. 1273 (55KB, PDF); and Eliason et al., 2003, LPS XXXIV, No. 2093 (210 KB, PDF). Processing of the global mosaics based on the radiometric and photometric methods described in these references resulted in the "standard processing" global mosaics presented above.


where: DN = 16-bit pixel value of the UVVIS-DIM image matrix. SCALE FACTOR = 1.3500E-04


PDS Status
PS 3 likes
Source PDS file
author source
planetary data system
Source link online
Middle Quell Art


location description
minimum latitude
maximum latitude
Minimum length
Maximum length
Direct Spatial Reference Method
object type
lines (pixels)
samples (pixels)
bit type
quadruple name
LQ-1, LQ-30
Radio A
Radio C
Pixel resolution (meters/pixels)
Scale (pixels/degrees)
Horizontal coordinate system units
Map projection name
simply cylindrical
latitude type
length direction
this positive
length range
-180 a 180
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