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mklut stsdas.graphics.sdisplay


NAME · USAGE · DESCRIPTION · PARAMETERS · EXAMPLES · BUGS · SEE_ALSO

NAME

mklut -- Generate a lookup table for image display.

USAGE

mklut infile

DESCRIPTION

This task creates a text lookup table (LUT) which contains a translation between the flux and the display brightness level. This text file can then be used to display an image such that the brightness and contrast levels of the displayed image are similar to that obtained from a hardcopy device such as the CELCO. The output of this task is sent to the screen. You can redirect it to a file, see the example below.

The LUT is constructed as follows. Let the cumulative histogram (that is, the integral of the histogram) of the input DN be called T(x), for data number x. T is monotonic nondecreasing. (Use of T as the LUT is the histogram equalization method.) Let the desired output histogram of gray levels be g(x) which is a Gaussian function with the width of sigma. Multiplying the contrast parameter (see below) with sigma gives the range from either end of the data range to the midlle point (the gray level). The cumulative histogram (integral) of g will be called G(x).

Construct the inverse of G and call it Ginv(y). Then the desired LUT to transform input DN to output gray level is

                                
                         LUT = Ginv(T(x)).

The result has many gray levels near middle gray, but significant numbers at saturated black and white. Moreover, the result has less contrast than that given by histogram equalization; but like histogram equalization, all values of DN are represented in the output. The steep sides of the Gaussian function help reduce the contrast in the output, while the finite value of the Gaussian at the ends of the total range in DN ensures that pixels with those DN are also represented in the output image. For instance, this allows faint nebulosity in a wispy region of the Orion nebula to be seen as well as bright stars, whose images are not bloomed but rather are fairly point-like. As another example, histogram specification as the Gaussian described above allows moons in the vicinity of Saturn to show clearly as well as features on the chip (noise) and details of the planet and rings.

Extremely high and low counts in the original data are excluded from the cumulative histogram by setting an upper and lower limit of the data set. These are specified in the parameters upper and lower (see below). For example, if upper = 0.99 and lower = 0.01, then the top and bottom 1% data points are rejected.

To apply the newly created lookup table to display an image, do the following:


	display image_name ztrans="user" lutfile=lookup_table_name

PARAMETERS

infile = "" [string]
Name of the input image.
lower = "0.01" [real]
Lower limit of the usable histogram.
upper = "0.99" [real]
Upper limit of the usable histogram.
contrast = "3.0" [real]
Contrast measure. Smaller number has higher contrast. Experience shows that the default number of 3 should be suitable for most applications.

EXAMPLES

1. Make a lookup table called lut for the standard IRAF image, dev$pix.


wf> mklut dev$pix > lut

BUGS

SEE ALSO

display


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