Moon Clementine UVVIS Global Mosaic 118m

Primary Authors

USGS Astrogeology Science Center

Originators

Planetary Data System

Publisher

USGS Astrogeology Science Center

Publication Date

2009-04-09

Abstract

Product Information: The Clementine Ultraviolet/Visible (UVVIS) Version 2 mosaic is a grayscale data set representing the albedo (brightness of the lunar surface) as measured at the 750 nanometer (nm) wavelength by the UVVIS camera (Lee, et al., 2009). Resolution of this mosaic is 118 meters per pixel (m). In late 2008, a revised 750nm mosaic (v. 2.0) was created at USGS to refine the locations of component images by using the latest geodetic control and projecting onto a topographic model of the lunar surface (Archinal et al., 2006). The base map was radiometrically and geometrically controlled, photometrically modeled global image mosaic compiled using more than 43,000 images from the 750nm filter observations. 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: Archinal, B. A., Rosiek, M. R., Kirk, R. L., & Redding, B. (2006). The Unified Lunar Control Network 2005, Open-File Report 2006-1367, Reston, VA, U.S. Geological Survey. http://pubs.usgs.gov/of/2006/1367 Eliason, E., et al. (1997). Clementine Basemap Mosaic, PDS Volumes USA_NASA_PDS_CL_3001 through 3015, produced by the U.S. Geological Survey and distributed on CD media by the Planetary Data System. http://pds.nasa.gov/ds-view/pds/viewProfile.jsp?dsid=CLEM1-L-H-5-DIM-MOSAIC-V1.0 Lee, E. M., Gaddis, L. R., Weller, L., Richie, J. O., Becker, T., Shinaman, J., Rosiek, M. R., & Archinal, B. A. (2009). A New Clementine Basemap of the Moon. Paper presented at the 40th Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX. http://www.lpi.usra.edu/meetings/lpsc2009/pdf/2445.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 Planetary Data Systems (PDS) Cartography and Imaging Sciences Node (IMG) (2017). Clementine Mission. https://pds-imaging.jpl.nasa.gov/portal/clementine_mission.html

Purpose

Because of recent improvements in the geodetic control network of the Moon and the availability of a detailed 3D shape model on which to project the images, we created this new controlled Clementine basemap. This product supercedes the original base map created in 1998, and also the warped product generated to reflect the shift from the original control point positions to the new positions in the 2005 control network.

Contact and Distribution

Format

Global Mosaic, Image, Remote-sensing Data

Access Constraints

None

Access Scope

PDS

Use Constraints

Public domain

Edition

2

Supplemental Information

http://pds.nasa.gov/ds-view/pds/viewProfile.jsp?dsid=CLEM1-L-H-5-DIM-MOSAIC-V1.0, http://www.lpi.usra.edu/meetings/lpsc2009/pdf/2445.pdf, https://pdsimage.wr.usgs.gov/archive/clem1-l-u-5-dim-uvvis-v1.0/cl_4001/document/volinfo.htm

Native Data Set Environment

ISIS v3

Astrogeology Theme

Geomorphology, Image Processing, Satellites

Mission Names

Clementine

Instrument Names

UVVIS

Online Package Link

https://astrogeology.usgs.gov/search/map/moon_clementine_uvvis_global_mosaic_118m

External File Size

4 GB

Online File Link

https://planetarymaps.usgs.gov/mosaic/Lunar_Clementine_UVVIS_750nm_Global_Mosaic_118m_v2.1.tif

Contact Address

2255 N. Gemini Drive

Contact City

Flagstaff

Contact State

AZ

Contact Postal Code

86001

Contact Email

astroweb@usgs.gov

Data Status and Quality

Time Period of Content (start)

1994-02-01

Time Period of Content (stop)

1994-05-31

Currentness Reference

Ground condition

Progress

Complete

Update Frequency

None planned

Logical Consistency

The few gaps in the global mosaic were filled with images taken at 900nm or 950nm wavelengths.

Completeness Report

The new Clementine mosaic corrects many of the problems identified in the earlier basemap mosaic. Procedures and processing scripts are now in place that will allow us to easily regenerate the mosaic when a new global geodetic control solution is available.

Process Description

Approximately 43, 000 Clementine frames were radiometrically calibrated, photometrically corrected, geodetically controlled, and projected onto a spherical shape model of the Moon [4] to create a global mosaic at a uniform 100 m/pixel resolution. The USGS Integrated Software for Imagers and Spectrometers (ISIS) software was used to process the Clementine data for the basemap mosaic. The ingestion, radiometric calibration, and merging of low and high exposure image pairs were performed using the program ‘uv-viscal’ in the earlier ISIS 2 software. The analysis of the control network, repair or removal of bad control points in the network, updating of the camera pointing information to correct obvious offsets between images, and creation of the tone-matched mosaic was performed using the newest ISIS 3 software. The images were then photometrically corrected (using the Lunar Lambert photometric model and the ‘Moon Albedo’ normalization model) and trimmed in ISIS 3.

Lineage

Process Date

2008-12-01

Source Title

CLEMENTINE HIRES MOSAIC

Source Online Linkage

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

PDS Status

PDS 3 Archived

Attribute Accuracy Report

Accurate to Control Net

Horizontal Positional Accuracy Report

Accurate to Control Net

Geospatial Information

Target

Moon

System

Earth

Minimum Latitude

-90

Maximum Latitude

90

Minimum Longitude

-180

Maximum Longitude

180

Direct Spatial Reference Method

Raster

Object Type

Grid Cell

Raster Row Count (lines)

46080

Raster Column Count (samples)

92160

Bit Type (8, 16, 32)

8

Quad Name

Radius A

1737400

Radius C

1737400

Bands

1

Pixel Resolution (meters/pixel)

118.451

Scale (pixels/degree)

256

Map Projection Name

Simple Cylindrical

Latitude Type

Planetocentric

Longitude Direction

Positive East

Longitude Domain

-180 to 180