IR OBSERVATIONS. We have extended previous infrared imaging studies (cf. Hora & Latter 1994 ApJ 437, 281; Kastner et al. 1996 ApJ 462, 777) through wide and narrow band filters.

In these images: (a) JHK′ morphology is similar to the optical structure. The knots are brighter at the shorter wavelengths, while the core is brighter at K′. (b) [He I] 1.083 μm that traces the highly ionized region, is concentrated along the axial region and extends throughout the lobes (33″ × 9″). It shows the knots very prominently. (c) [Fe II] 1.644 μm, that traces the shock excited regions, extends []throughout the lobes; it is more prominent in the northern knot and it is very strong in the core. (d) The excited molecular H2 lines are concentrated on a wide ‘torus’ in the equatorial plane. This geometry is similar to that exhibited by most bipolar planetary nebulae where H2 has been detected (e.g., Kastner et al. 1996). No H2 emission is seen in the core. (e) Paγ shows emission in only in the core and the northern knot. (f) Brγ shows emission in the core and in knots N2, S2 and S3. (g) No significant emission in CO was obtained.