Moon Clementine NIR Empirical Calibration 500m

Primary Authors

USGS Astrogeology Science Center

Originators

Planetary Data System

Publisher

USGS Astrogeology Science Center

Abstract

Product Information: This mosaic represents a reduced-resolution version of the empirical calibration Clementine near-infrared (NIR) mosaic processed to 500 meters per pixel (m) spatial resolution 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, was launched from Vandenburg Air Force Base aboard a Titan IIG rocket, as a joint project between the and was jointly sponsored by the Ballistic Missile Defense Organization (BMDO) of the Dept of Defense and NASA. The objective of the mission was to test sensors and spacecraft components under extended exposure to the space environment and to make scientific observations of the Moon and a near-Earth asteroid (1620 Geographos). After two Earth fly-bys, lunar insertion was achieved on February 19th. Lunar mapping took place over approximately two months in two systematic mapping passes over the Moon. After the spectacular success of the Lunar mapping phase of the mission, Clementine suffered an on-board malfunction on May 7, 1994 that resulted in the activation of its altitude thrusters. This exhausted all the fuel for altitude control and left the spacecraft spinning at 80 revolutions per minute. The result of the malfunction prevented Clementine from performing the planned close fly-by of the near-Earth asteroid Geographos scheduled for August 1994. The main instrumentation on Clementine consisted of four cameras, one with a laser-ranging system. The cameras included an ultraviolet-visual (UVVIS) camera, a long-wavelength infrared (LWIR) camera, the laser-ranger (LIDAR) high-resolution (HIRES) camera, and a near-infrared (NIR) camera. The spacecraft also had two star tracker cameras (A-STAR, B- STAR), used mainly for attitude determination, but they also served as wide-field cameras for various scientific and operational purposes (PDS IMG, 2017). References: Cahill, J. T., Lucey, P. G., Gillis, J. J., & Steutel, D. (2004). Verification of quality and compatibility for the newly calibrated Clementine NIR data set. Paper presented at the 35th 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 Specification (SIS). 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 from the Clementine UVVIS imaging instrument. Paper presented at the 30th 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 near-infrared (NIR) global multispectral map of the Moon from Clementine. Paper presented at the 34th 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). Calibration of the Clementine near infrared camera: Ready for prime time. Paper presented at the 29th 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. Paper presented at the 31st Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX. https://www.lpi.usra.edu/meetings/lpsc2000/pdf/1273.pdf McEwen, A. S., & Robinson, M. S. (1997). Mapping of the Moon by Clementine. Advances in Space Research, 19(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 Overview. Science, 266(5192), 1835-1839. https://www.doi.org/10.1126/science.266.5192.1835 Pieters, C. M., & Pratt, S. (2000). Earth-based near-infrared collection of spectra for the Moon: A new PDS data set. Paper presented at the 31st 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) Cartography and Imaging Sciences Node (IMG) (2017). Clementine Mission. https://pds-imaging.jpl.nasa.gov/portal/clementine_mission.html

Purpose

In May and June of 1994, the NASA/DoD Clementine Mission acquired global, 11-band, multispectral data of the lunar surface using the ultraviolet-visible (UVVIS) and near-infrared (NIR) camera systems (e.g., Nozette et al, 1994; McEwen and Robinson, 1996). The global 5-band UVVIS Digital Image 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 delivered in 996 quads at 100 m/pixel (303 pixels/degree) in early 2004. This First Release NIR mosaic is processed to 500 m/pixel, has 6 spectral bands, and is presented in Simple Cylindrical map projection for the east (0° to 180° E) and west (180° to 360° E) lunar hemispheres. The NIR data have been radiometrically corrected, geometrically controlled to the Clementine 750-nm mosaic, and photometrically normalized to form seamless, uniformly illuminated mosaics of the lunar surface. The first four NIR bands (1100 to 2000 nm) have also been normalized to reflectance based on the approach previously applied to the calibrated UVVIS global mosaics (Pieters et al., 1999). The 2600 nm and 2780 nm NIR buands are provided as calibrated Clementine digital numbers (in counts/ms).

Contact and Distribution

Format

Global Mosaic, Remote-sensing Data

Access Constraints

public domain

Access Scope

PDS

Use Constraints

None

Edition

1

Supplemental Information

http://astrogeology.usgs.gov/maps/moon-clementine-near-ir-global-map, http://www.lpi.usra.edu/meetings/lpsc2007/pdf/2092.pdf , https://isis.astrogeology.usgs.gov

Native Data Set Environment

ISIS v3

Astrogeology Theme

Image Processing, Mineral resources, Remote Sensing

Mission Names

Clementine

Instrument Names

NIR

Online Package Link

https://astrogeology.usgs.gov/search/map/moon_clementine_nir_empirical_calibration_500m

External File Size

2 GB

Online File Link

https://planetarymaps.usgs.gov/mosaic/Lunar_Clementine_NIR_cal_empcor_500m.tif

Contact Address

2255 N. Gemini Drive

Contact City

Flagstaff

Contact State

AZ

Contact Postal Code

86001

Contact Email

astroweb@usgs.gov

Currentness Reference

Publication date

Progress

Complete

Update Frequency

None planned

Logical Consistency

For these products, we used the radiometric camera model described in Lucey et al. (2000) along with a thermal background correction described 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 having residual errors in the values associated with the instrument operating modes (gain, offset, and exposure values); 2) residual errors existing in the thermal background correction; and 3) the shading properties of the sensor array changing with the thermal conditions of the camera that have not been properly characterized. In addition to the major radiometric and photometric processing, empirically derived frame offset corrections were applied to produce a second version of the global mosaics with reduced variability across camera modes and adjacent orbits. This additional processing resulted in the "empirically corrected" mosaics and is described in more detail below. Similar before-and-after comparisons are shown for the Aristarchus Plateau region and the eastern portion of the South Pole-Aitken basin region. Finally, 1500/2000-nm ratios of the western hemisphere and the Aristarchus Plateau are shown to illustrate the magnitude of the changes between the calibrated and empirically corrected versions of the NIR mosaics.

Completeness Report

-70 to 70 latitude

Process Description

Details of the processing of the NIR mosaics have been described in several publications: Lucey et al., 1998, LPS XXIX, #1576 (25 KB, PDF); Lucey et al., 2000, LPS XXXI, #1273 (55 KB, PDF); and Eliason et al., 2003, LPS XXXIV, #2093 (210 KB, PDF). Processing of the global mosaics based on the radiometric and photometric procedures described in these references resulted in the "standard processing" global mosaics presented above. FRACTIONAL_REFLECTANCE = (SCALING_FACTOR * DN) where: DN = 16-bit pixel value of UVVIS DIM image array. SCALING_FACTOR = 1.3500E-04

Source Online Linkage

{https://pds-imaging.jpl.nasa.gov/volumes/clementine.html,https://pds-imaging.jpl.nasa.gov/portal/clementine_mission.html}

Source PDS Archive

Clementine

PDS Status

PDS 3 Like

Geospatial Information

Target

Moon

System

Earth

Minimum Latitude

-70

Maximum Latitude

70

Minimum Longitude

-180

Maximum Longitude

180

Direct Spatial Reference Method

Raster

Object Type

Grid Cell

Raster Row Count (lines)

8491

Raster Column Count (samples)

21833

Bit Type (8, 16, 32)

16

Quad Name

LQ-1, LQ-30

Radius A

1737400

Radius C

1737400

Bands

6

Pixel Resolution (meters/pixel)

500

Scale (pixels/degree)

60.6467008

Map Projection Name

Simple Cylindrical

Latitude Type

Planetocentric

Longitude Direction

Positive East

Longitude Domain

-180 to 180