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   PR # 42125
   The current paradigm for active galactic nuclei consists of an
   accreting supermassive black hole surrounded by an optically thick
   structure which obscures the nucleus from direct view along some
   lines-of-sight. There is much scientific merit in determining the
   depth of obscuring material along the line-of-sight in a large sample
   of objects, and this can be done in both the infrared and X-ray
   regimes. The ability to combine results from the two methods is
   clearly desirable. Currently, a universal gas-to-dust ratio is
   assumed, but the uncertainty in the relationship between the gas and
   dust columns is unknown. In NGC 3281, there is evidence that the
   ratio may be significantly different from the assumed value, and we
   request ASCA observations to test this hypothesis.
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