Lunar image flash viewer

You have reached a WMS server for Lunar data.
The WMS server URL, to be used by WMS client applications is
If you are writing a WMS client, or use one that allows the definition of a coordinate system, please use the IAU2000 namespace for coordinate reference systems encoding, in which the lunar geographic projection is encoded as IAU2000:30100

The following datasets are available:

Clementine image


The Clementine 750 nm Base Map data is a greyscale image representing the albedo (brightness of the lunar surface) as measured at the 750 nm wavelength by the UV/Vis camera. This lunar base map is a radiometrically and geometrically controlled, photometrically modeled global image mosaic compiled using more than 43,000 images from the 750 nanometer filter observations of the Ultraviolet/Visible camera onboard the Clementine Spacecraft. The final NASA PDS archive (volumes CL_3001 through CL_3015) was produced in July, 1997 by the USGS Astrogeology Research Program in cooperation with University of Arizona (Lunar and Planetary Laboratory) and Northwestern University, Evanston, IL. The resulting image was warped using a 6th order polynomial to conform to the ULCN2005 control network.
To see the Clementine mosaic using GoogleEarth use this KML file:OnMoon_Clementine.kml.

Lunar Orbiter image

Lunar Orbiter Mosaic

This Lunar Orbiter global digital mosaic was constructed using data aquired by LO III, IV and V; High- and Medium- Resolution cameras that were projected to Equirectangular projection at 512 pixels/degree (~59.0 meters/pixel). A high pass boxfilter was applied to the individual frames before mosaicking in order to normalize the relative brightness. The results emphasize the high-frequency data by retaining only 10% of the low-frequency brightness variation. For further information, visit USGS Planetary GIS Web Server

Clementine UV and Visual image

Clementine UV and Visual, multispectral.

This layer contains the full resolution, 5 band, 16 bit per pixel Clementine ultraviolet and visual mosaics, warped to match the ULCN2005. Coverage is limited to latitudes between S60 to N60. The default style contains bands 2,1 and 0, mapped to red,green and blue, and then scaled to a 8 bit range.
The Ultraviolet/Visible (UV/Vis) camera was designed to study the surface of the Moon at five different wavelengths in the ultraviolet and visible spectrum. This experiment yielded information on the petrologic properties of the surface material on the Moon, as well as giving images useful for morphologic studies and cratering statistics. Most images were taken at low Sun angles, which is useful for petrologic studies but not for observing morphology. The global images were further warped using a 6th order polynomial to conform to the ULCN2005 control network.
Band 1 - 415 nm, Ultraviolet-Violet
Band 2 - 750nm, Red-Near Infrared
Band 3 - 900nm, Near Infrared
Band 4 - 950nm, Near Infrared
Band 5 - 1000nm, Near Infrared

Lunar Elevation

ULCN 2005Elevation

The lunar elevation as 16 bit integers, matching the Unified Lunar Control Network 2005, 16 data points per degree. The default style is scaled to 8 bit range. The full precision DEM can be requested by useing PNG format and the "short_int" style.
The elevation model, at 1895m per pixel, is based on a local polynomial of first degree with a segmented a circular search area having four segments to select the closest minimum of 5 and maximum of 25 control network points.


Colorized and shaded elevation

Image obtained by applying a color scale to the elvation, with extra hillshading.


Grayscale and shaded elevation
Grayscale elevation, with hillshading.

The shaded relief data were originally published as a series of 1:5 million shaded relief maps. This series included three U.S. Geological Survey maps: I-1218-B, Shaded Relief Map of the Lunar Far Side, 1980; I-1326-A, Shaded Relief Map of the Lunar Polar Regions, 1981; and I-2276, Sheet 2 of 2, Shaded Relief Map of the Lunar Near Side, 1992. These maps were digitized and mosaicked into a single digital file. An area of approximately 500,000 km2 near the south pole was not visible in any pre-Clementine images and is blank on the published map. The digitized relief base was revised based on the Clementine mosaic and recent Earth-based radar imagery to show features in this area. Errors that were present in the original interpretations of lunar morphology have not been corrected in the digital version of the warped shaded relief map base. These original errors were caused by scanty data, ambiguities introduced by highly oblique solar incidence angles, and distortions created in generating orthophotographs from oblique images.