LPI Clementine Mapping Project Help


Area of Interest

Use the settings in this section to define the geographic area for which you would like to collect Clementine data.

The reference image at the top of the page is a simple cylindrical map projection of the entire moon. The image displays Clementine 750 nm data centered a 0° latitude and 0° longitude. The center portion of the image (-90° to +90° longitude) is the near side of the Moon while the flanking portions (-180° to -90° and +90° to +180° longitude) are the far side.

Specify North, South, East, and West boundaries where:

North
The northernmost latitude of your area of interest (valid range: -90° to +90°).
South
The southernmost latitude of your area of interest (valid range: -90° to +90°).
East
The easternmost longitude of your area of interest (valid range: -180° to +360°).
West
The westernmost longitude of your area of interest (valid range: -180° to +360°).
Constraints
Latitude and longitude values must be entered in decimal degrees.
South should always be less than North.
West should always be less than East.
The Moon uses a positive east coordinate system for longitudes.
Use -180° to +180° longitude range to specify West and East unless your area of interest crosses the ±180° meridian.
If your area of interest crosses the ±180° meridian, use 0° to 360° longitude range to specify West and East.
The longitude range entered cannot be more than 360° (East - West must be ≤ 360°).
If your browser has javascript enabled, then a red box will outline the specified area of interest. If the red outline disappears while entering boundary values, this indicates that a boundary entry error has occurred. Click on the Submit button to detect errors and display error messages.


Output Map Projection

Use the settings in this section to define the map projection for the output image files.

Specify the Projection, Projection Center Latitude, Projection Center Longitude, and Projection Scale where:

Projection
The map Projection to be used: Simple Cylindrical, Sinusoidal, Orthographic, or Polar Stereographic. For more info about map projections see: USGS Map Projections.
Projection Center Latitude
The Center Latitude defines the latitude of origin for Sinusoidal and Orthographic projections. It defines the latitude of true scale for Simple Cylindrical and Polar Stereographic projections. For Simple Cylindrical and Sinusoidal projections this is usually set to 0. For Orthographic projection this is the latitude of the center point of the output image. For Polar Stereographic projection this is the latitude that will have the least distortion (valid range: -90° to +90°).
Projection Center Longitude
The Center Longitude defines the central meridian of the projection for the Simple Cylindrical, Sinusoidal, Orthographic, and Polar Stereographic projections. This is the longitude that will appear at the center of the output image. If West and East use the -180° to +180° longitude range then Center Longitude should also use that range but if West and East use the 0° to +360° longitude range then Center Longitude should use that range (valid range: -180° to +360°)
Projection Scale(km/pix)
The resolution of the output image files in kilometers/pixel (valid range: ≥ 0.1 and ≤ 10914).
Projection Scale(pix/deg)
The resolution of the output image files in pixels/degree (valid range: ≥ 1 and ≤ 303).
Constraints
One map projection must be selected.
Center Latitude and Center Longitude values must be entered in decimal degrees.
Either Scale (km/pix) or Scale (pix/deg) must be used. If both are specified then Scale (km/pix) will be used.


Output Files

Use the settings in this section to specify which output data files you would like to create.

Data Types include:

UVVIS Multiband Mosaic
Select data from the Clementine Ultraviolet/Visible(UVVIS) Multispectral Digital Image Model dataset for the specified area of interest. The UVVIS mosaic is mapped at a resolution of 100 meters (0.1 km) per pixel and contains observations in the 415, 750, 900, 950, 1000 nm wavelength bands.
To select UVVIS Multiband Mosaic data, set the File Type option to a selection other than None.

Options... Bands
If the File Type is set to CUB or RAW, you may choose 1-5 bands to be included in your output mosaic.
If the File Type is set to PNG, you must select either only 1 band or a total of 3 bands.

For more info on the UVVIS Multispectral Digital Image Model see: (Eliason et al., 1999, The Clementine UVVIS Global Lunar Mosaic)
RGB False Color Ratio
Select RGB False Color Ratio data for the specified area of interest. The color ratio image enhances color differences related to soil mineralogy and maturity. This ratio is derived using 3 bands from the UVVIS dataset and performing the following calculation:
R = 750 nm / 415 nm
G = 750 nm / 950 nm
B = 415 nm / 750 nm
The resulting RGB values are then assembled into a color image.
To select RGB False Color Ratio data, set the File Type option to a selection other than None.
For more info on the False Color Ratio see: (Pieters et al., 1994, A Sharper View of Impact Craters from Clementine Data, Science, 266, 1844-1848)
FeO Abundance
Select iron (FeO) abundance data for the specified area of interest. Iron abundance is calculated using the 415 nm (only for Gillis option), 750 nm, and 950 nm bands from the UVVIS dataset using the algorithm selected under Options.
To select FeO Abundance data, set the File Type option to a selection other than None.

Options... Method
Lucey et al.(2000):
Algorithm developed to normalize the effect of space weathering so that composition may be determined without regard to surface state of maturity. For more info on the Lucey iron abundance algorithm see: (Lucey et al., 2000, Lunar iron and titanium algorithms based on final processing of Clementine ultraviolet-visible images, Journal of Geophysical Research, Vol. 105, No. E8, pp. 20,297-20,305, August 25, 2000)
Gillis et al.(2004):
Modified algorithm for deriving FeO concentrations that incorporates an adjustment for TiO2 content. TiO2 concentrations are derived using the Gillis et al.(2003) algorithm (see TiO2 Abundance below). For more info on the Gillis iron abundance algorithm see: (Gillis et al., 2004, Lunar surface geochemistry: Global concentrations of Th, K, and FeO as derived from Lunar Prospector and Clementine data, Geochimica and Cosmochimica, Vol. 68, No. 18, pp. 3791-3805, 2004)

Data values returned for CUB and RAW files are the actual %wt values.
Data values returned for PNG files are %wt x 10 (i.e., %wt = pixel value/10).
TiO2 Abundance
Select titanium (TiO2) abundance data for the specified area of interest. Titanium abundance is calculated using the 415 nm and 750 nm bands from the UVVIS dataset using the algorithm selected under Options.
To select TiO2 Abundance data, set the File Type option to a selection other than None.

Options... Method
Lucey et al.(2000):
Algorithm developed to normalize the effect of space weathering so that composition may be determined without regard to surface state of maturity. For more info on the Lucey titanium abundance algorithm see: (Lucey et al., 2000, Lunar iron and titanium algorithms based on final processing of Clementine ultraviolet-visible images, Journal of Geophysical Research, Vol. 105, No. E8, pp. 20,297-20,305, August 25, 2000)
Gillis et al.(2003):
Modified algorithm for deriving TiO2 concentrations using two different sets of regression parameters to relate regolith compositions from sampling locations to Clementine data properties at those sites. For more info on the Gillis titanium abundance algorithm see: (Gillis et al., 2003, A revised algorithm for calculating TiO2 from Clementine UVVIS data: A synthesis of rock, soil, and remotely sensed TiO2 concentrations, Journal of Geophysical Research, Vol. 108, No. E2, pp. 3791-3805, 2003)

Data values returned for CUB and RAW files are the actual %wt values.
Data values returned for PNG files are %wt x 10 (i.e., %wt = pixel value/10).
Topography
Select topography data for the specified area of interest. This dataset is a lunar topographic model based on the USGS Unified Lunar Control Network 2005 (ULCN 2005) that was derived from Clementine, Earth based, Apollo, Mariner 10, and Galileo images. The dataset resolution is 16 pixels/degree or about 1.895 km/pixel. Data will be interpolated for higher resolution requests. This dataset is available in two forms, Original and Smoothed, which may be selected under Options.
To select Topography data, set the File Type option to a selection other than None.

Options... Method
Original:
Data as originally derived from parent datasets.
Smoothed:
Polynomial smoothed original data.

Data values returned for CUB and RAW files are planetary radii in meters.
Data values returned for PNG files are linearly scaled values ranging from 0 to 255 which correspond to the minimum and maximum topographic values in the area of interest. These minimum and maximum topographic values (planetary radii in meters) can be found in the History section of the job_summary.txt file supplied with your output files when your job has been processed.
For more info on the Unified Lunar Control Network 2005 see: (Archinal et al., 2006, The Unified Lunar Control Network 2005)

File Types include:

PNG
Portable Network Graphic (PNG) format (.png file extension). This image format is compatible with most web browsers and image manipulation programs like Photoshop and Paint Shop Pro. A PNG file contains 8-bit data values in either 1 band (grayscale) or 3 bands (RGB color).
A PNG World file (.pgw file extension) is also provided. A world file is a plain text file used by geographic information systems (GIS) to provide georeferencing information for raster map images.
For more info about GIS world files see: Wikipedia "World file" entry.
CUB
ISIS cube format (.cub file extension). This image format is compatible with the USGS Integrated Software for Imaging Spectrometers (ISIS) software. A CUB file may contain 8-bit or 16-bit integer or 32-bit floating-point data values in one or more bands.
For more info about USGS ISIS software see: USGS ISIS Homepage.
RAW
Raw data format (.raw file extension). This image format contains no header information and is compatible with many data modelling programs like IDL, Matlab, and Mathematica. A RAW file may contain 8-bit or 16-bit integer or 32-bit floating-point data values in one or more bands.
When importing RAW file data into an application like those mentioned above it is usually necessary to know the number of samples, lines, and bands in the dataset and the data type of the values. The number of samples, lines, and bands can be determined by examining the NS, NL, and NB values found in the History section of the job_summary.txt file supplied with your output files when your job has been processed.
RAW file data format will depend upon the requested Data Type as follows:


UVVIS Multiband Mosaic RAW file data format will be 16-bit (2-byte) Sun integer values.
RGB False Color Ratio RAW file data format will be 32-bit (4-byte) IEEE Sun floating-point values.
FeO Abundance RAW file data format will be 32-bit (4-byte) IEEE Sun floating-point values.
TiO2 Abundance RAW file data format will be 32-bit (4-byte) IEEE Sun floating-point values.
Topography RAW file data format will be 32-bit (4-byte) IEEE Sun floating-point values.


Contact Information

E-mail

Specify a valid e-mail address to receive notification of job completion or processing errors.
Upon successful completion of your job an e-mail message will be sent to this address containing a link to the FTP site from which you can download your requested data files.
If your job is unable to run as submitted, an e-mail message will be sent to this address containing a summary of your job and suggestions on how to modify your request to run successfully.


Acknowledgements

The Lunar and Planetary Institute would like to acknowledge the United States Geological Survey for supplying data and software used by the LPI Clementine Online web application. We would particularly like to thank the USGS for the use of the Clementine UVVIS Digital Image Model (DIM) multispectral dataset, the Unified Lunar Control Network 2005 (ULCN 2005) topography dataset, and the Integrated Software for Imaging Spectrometers (ISIS).

The Lunar and Planetary Institute would also like to acknowledge Dr. Paul G. Lucey, PhD and Dr. Jeffery J. Gillis, PhD for the use of their FeO and TiO2 lunar abundance algorithms.


In Case of Trouble

If you are having problems using this application which cannot be resolved after carefully reading this document, please send a detailed e-mail message to Brian Fessler at the Lunar and Planetary Institute.