We propose to test the `Unified Model' for Active Galactic
Nuclei (AGN) by searching for broad emission lines in the spectrum
of the most famous Seyfert 2 galaxy, NGC1068. In the context
of the unified model, it harbours a quasar-like nucleus which is
obscured from direct view by dust. This model explains much of the
diversity observed among AGN simply by taking into account orientation
effects, which result in different amounts of obscuring material to lie
along the line of sight. In fact, polarimetric studies have shown that
some Seyfert 2 nuclei, and in particular NGC1068, have Seyfert
1 characteristics, i.e. broad permitted lines and a non-stellar
continuum when observed in polarized light (Antonucci & Miller 1985).
Nevertheless, the interpretation of the polarization data are not
unique (see Antonucci 1993) and hence independent tests for the unified
model are required. One way to reduce the effect of the
obscuring material is by observing at longer IR wavelengths where the
extinction rapidly decreases. The detection of broad recombination
lines in the near-IR would provide definite proof of the existence of
the highly energetic processes linked to the central engine of a
Seyfert 1 or QSO. Although the obscuration decreases dramatically
with increasing wavelength, the intrinsic strengths of the hydrogen
lines also decrease, the best line for such observations is the Pfund
alpha line (7.46 microns) which will still be somewhat attenuated
but intense enough to allow a good determination of its profile. The
high signal to noise ratio required to clearly detect the  broad
wings means that such a project is unfeasible for the vast majority
of Seyfert 2s, and we have therefore chosen to observe the brightest.
These observations will allow us to disentangle the controversy
surrounding the amount of absorbing material required to explain its
observed spectrum within the context of the Unified Model.