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Establish the color-color transformation, for late
spectral type stars.
|  Compile a catalog for nearby stars with known distance (Parallax), and
UV data (IUE, TD-1, Others)
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| Get all the IR information in the LOS of the stars in the catalog.
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| Get the radio information (21cm line) for the
direction of the stars.
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| Compile a new transformation coefficients for
the stars (How good are the atmospheric models ???)
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| Compare the results with the predictions.
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Study the deviation of the predicted UV magnitude
from the observed UV magnitude.
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| .
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| Use the previous results to
study the distribution of extinction, and the spectral nature of it.
|  Produce an all-sky-map of the total
extinction in each TD-1 bands.
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| Compare the map to IR studies of dust
distribution.
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| Compare the map to radio observation (21 cm
line) of natural hydrogen.
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| Produce a 3-D map of the dust distribution
and mount it on the net (compare first with some known programs, like
the EUVE etc.)
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| PAPER
and kill the referee
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