We propose to look for the 9.7 micron silicate feature in quasars.
 While the existence of dust in quasars has long been suspected,
 detection of the silicate feature would be the first direct evidence
 for dust.  In addition, comparison with models would allow
 investigation of the geometry, amount, and composition of the dust.
 The resulting information can ultimately be used to study the
 generation and balance of energy in these active nuclei.

 Observation of the silicate feature have already proven useful in
 investigations of the dust content and geometry in lower luminosity
 AGN such as Seyferts.  However, in general it is impossible to
 observe this feature in higher-luminosity objects, i.e. quasars,
 with ground-based instruments: for redshifts z>0.2, the band begins
 to be shifted beyond the 13 micron atmospheric cutoff.  Even in the
 few lower redshift quasars this feature has been inaccessible
 because of faint flux levels.  With ISOCAM's CVF, these objects
 will be easily observable.