We show from modeling the Fe K \alpha line in the ASCA spectra of four X-ray bright narrow emission line galaxies ( Seyfert types 1.9 and 2 ) that two equally viable physical models can describe the observed line profile .
The first is discussed by Turner et al .
( 1998 ) and consists of emission from a nearly pole-on accretion disk .
The second , which is statistically preferred , is a superposition of emission from an accretion disk viewed at an intermediate inclination of \sim 48 ^ { \circ } and a distinct , unresolved feature that presumably originates some distance from the galaxy nucleus .
The intermediate inclination is entirely consistent with unified schemes and our findings challenge recent assertions that Seyfert 2 galaxies are preferentially viewed with their inner regions face-on .
We derive mean equivalent widths for the narrow and disk lines of < { EQW } _ { N } > = 60 eV and < { EQW } _ { D } > = 213 eV , respectively .
The X-ray data are well described by a geometry in which our view of the active nucleus intersects and is blocked by the outer edges of the obscuring torus , and therefore do not require severe misalignments between the accretion disk and the torus .