clemphot Documentation

clemphot - Photometric correction for Clementine UVVIS images
This procedure executes the ISIS photometric normalization
programs, photompr and photom with the parameters set specifically for
processing Clementine UVVIS images. The 'moonpr' function is chosen in
photompr with the phase angle set at 30 degrees.  In conjunction, within
photom the 'albedo' option is selected, with values set specifically for
highland areas, mare areas or the average for each UVVIS band.  This
procedure reads the band from the image labels to determine if it is
an lua, lub, luc, lud, or lue image.  For further details, please
refer to the help within photompr and photom.

References for the photometric function:
1) McEwen, A.S., A Precise Lunar Photometric Function: Proceeding
of the 27th Lunar and Planetary Science Conference, pp. 841-842,
1996.
2) McEwen, A.S., E. Eliason, P. Lucey, E. Malaret, C. Pieters,
M. Robinson, T. Sucharski, Summary of Radiometric Calibration and
Photometric Normalization Steps for the Clementine UVVIS Images:
Proceedings of the 29th Lunar and Planetary Conference, on CD-ROM
media, 1998.
3) Buratti, B.J., J.K. Hillier, and M. Wang, 1996, The Lunar
Opposition Surge:  Observations by Clementine, Icarus, 124,
pp. 490-499.
4) McEwen, A.S., 1991, Photometric Functions for Photoclimonmetry
and other applications, Icarus, v. 92, pp. 298-311.

Programmer: Mark Robinson, Original
            Ella Lee       Revisions
            Tammy Becker   Revisions-June 25, 1999

INPUT IMAGE FILE NAME

NONE

OUTPUT IMAGE FILE NAME

NONE

ALBEDO DEPENDENT PARAMS
(H=highlands M=mare A=Average)

"A"

Output pixel type
   0 = input type
   1 = 8 bit
   2 = 16 bit
   3 = 32 bit

0

Output min/max data range

0,0

Incidence Angle

89.0

Emission Angle

89.0

ADDITIONAL NOTES:

Parm	Description
FROM	Specifies the name of the file which contains the input disk image.
TO	Specifies the name of the file which will contain the output disk image.
ALBEDO	Specifies which parameter values to use in the normalization A=Average M=Mare H=Highlands
OTYPE	Output pixel data type. Permitted values are: 0 = output type is same as input file pixel type 1 = 8-bit (integer with type conversion parameters) 2 = 16-bit (integer with type conversion parameters) 3 = 32-bit (floating point)
ORANGE	If the input file is 16-bit, for any UVVIS image, an orange of (-4.5,4.5) works well. If the input image is 32-bit, orange is ignored, as noted below. It is not recommended to run photometry on 8-bit data. If OTYPE=1 (8-bit) or OTYPE=2 (16-bit), then the CORE_BASE and CORE_MULTIPLIER in the output file will be set to values that allow representing the specified range of output values. Output values outside this range will be stored as a special "representation saturation" value. The ORANGE parameter is ignored if OTYPE=3 (32-bit) since the CORE_BASE and CORE_MULTIPLIER are not applicable to floating point pixel values. **NOTE** For a more detailed explanation of ORANGE, tutor the orange.pdf.
INC	For Clementine north and south pole images, it is recommended to use 89.95. INC is used as an incidence angle boundary. For any pixel point of the input cube that is greater than INC, it is set to null, "cut-off". This effects the terminator of the planet in the cube. This value should not be set above 90 degrees.
EMA	For Clementine north and south pole images, it is recommended to use 89.95. EMA is used as an emission angle boundary. For any pixel point of the input cube that is greater than EMA, it is set to null, "cut-off". This effects the limb of the planet in the cube. This value should not be set above 90 degrees.