Moon Clementine UVVIS 5 Band Warped Image Mosaic 200m

Primary Authors

Trent Hare

Originators

Eric Eliason, Chris Isbell, Ella Lee, Tammy Becker, Lisa Gaddis, Alfred McEwen, Mark Robinson

Publisher

USGS Astrogeology Science Center

Publication Date

2008-03-01

Abstract

Product Information: The Clementine Ultraviolet/Visible (UVVIS) mosaic of Earth's Moon is a radiometrically and geometrically controlled, photometrically modeled global Mosaicked Digital Image Model (DIM) compiled using more than 400,000 images from multiple spectral observations of the Ultraviolet/Visible camera onboard the Clementine Spacecraft (Eliason, et al., 1999). The mosaic is composed of the 415nm, 750nm, 900nm, 950nm, and 1000nm wavelength as a single 5 band image. This version was warped from the original spatial location using the ULCN2005 control network (Hare, et al, 2008). Resolution of this mosaic is 200 meters per pixel (m). 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: Eliason, E., Isbell, C., Lee, E., Becker, T., Gaddis, L., McEwen, A., Robinson, M., Mission to the Moon: The Clementine UVVIS Global Lunar Mosaic, PDS Volumes USA_NASA_PDS_CL_4001 through 4078, produced by the U.S. Geological Survey and distributed on CD media by the Planetary Data System, 1999. Hare, T. M., Archinal, B. A., Becker, T. L., Lee, E. M., Gaddis, L. R., Redding, B. L., & Rosiek, M. R. (2008). Clementine Mosaics Warped to ULCN 2005 Network. Paper presented at the 39th Lunar and Planetary Science Conference, Lunar and Planetary Institute, Houston, TX. https://www.lpi.usra.edu/meetings/lpsc2008/pdf/2337.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

This 5 band image allows one to create band-ratio derived images including titanium abundance, optical maturity maps, and various other mineral ratios.

Contact and Distribution

Format

Global Mosaic, Mineral Map, Remote-sensing Data

Access Constraints

None

Access Scope

PDS

Use Constraints

None

Edition

1

Supplemental Information

http://www.lpi.usra.edu/meetings/lpsc2008/pdf/2337.pdf, http://pdsimage.wr.usgs.gov/archive/clem1-l-u-5-dim-uvvis-v1.0/cl_4001/document/volinfo.htm, http://pubs.usgs.gov/of/2006/1367/, https://pds.nasa.gov/ds-view/pds/viewProfile.jsp?dsid=CLEM1-L-H-5-DIM-MOSAIC-V1.0

Native Data Set Environment

ISIS v3

Astrogeology Theme

Cartography, Image Processing, Remote Sensing

Mission Names

Clementine

Instrument Names

UVVIS

Online Package Link

https://astrogeology.usgs.gov/search/map/moon_clementine_uvvis_5_band_warped_image_mosaic_200m

External File Size

14 GB

Online File Link

https://planetarymaps.usgs.gov/mosaic/Lunar_Clementine_UVVIS_WarpMosaic_5Bands_200m.tif

Access Instructions

You will need an image viewer, remote sensing, or GIS application to view.

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)

1994-01-25

Time Period of Content (stop)

1994-05-07

Currentness Reference

Ground condition

Progress

Complete

Update Frequency

None planned

Logical Consistency

For the original mosaic approximately 265, 000 match points were collected at the USGS from ~43, 000 UVVIS 750nm images providing global coverage. About 80% of these points were collected via autonomous procedures, whereas the remaining 20% required the more time consuming but highly accurate pattern-recognition capability of the human eye-brain.

Completeness Report

The basemap has 95% coverage of the Moon (excluding the oblique observation gap fills).

Process Description

To facilitate warping we utilized the warp command within Esri's Arc/Info Workstation. Tests showed that a 6th order warp was needed. During the warp, we used a bilinear resampling since this routine optimizes the output pixel resolution. Thus before releasing the tiles to the community, they were again bilinearly resampled to the original resolution (Hare et al., 2008). The original Clementine UVVIS mosaic was geometrically controlled to the previously published Clementine Basemap Mosaic by tying individual UVVIS images that make up a color set to the corresponding image in the color set that was used to produce the basemap mosaic (Eliason et al., 1999). To convert the 16-bit integer values found in the image arrays of the UVVIS multispectral mosaic to fractional reflectance an offset and scaling factor need to be applied as shown: FRACTIONAL_REFLECTANCE = (SCALING_FACTOR * DN) where: DN = 16-bit pixel value of UVVIS DIM image array. SCALING_FACTOR = 1.3700E-04

Lineage

Process Date

2008-01-01

Source Title

The Clementine UVVIS Global Lunar 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 Like

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)

27273

Raster Column Count (samples)

54545

Bit Type (8, 16, 32)

16

Quad Name

Radius A

1737400

Radius C

1737400

Control Net

ULCN 2005

Bands

5

Pixel Resolution (meters/pixel)

200.1341

Scale (pixels/degree)

151.515

Map Projection Name

Simple Cylindrical

Latitude Type

Planetocentric

Longitude Direction

Positive East

Longitude Domain

-180 to 180