  Aims. Numerous planetary nebulae show complicated inner structures not
obviously explained. For one such object we undertake a detailed 3D
photoionization and kinematical model analysis for a better understanding of
the underlying shaping processes. Methods. We obtained 2D ARGUS/IFU
spectroscopy covering the whole nebula in selected, representative emission
lines. A 3D photoionization modelling was used to compute images and line
profiles. Comparison of the observations with the models was used to fine-tune
the model details. This predicts the approximate nebular 3D structure and
kinematics. Results. We found that within a cylindrical outer nebula there is a
hidden, very dense, bar-like or cylindrical inner structure. Both features are
co-axial and are inclined to the sky by 40 deg. A wide asymmetric one-sided
plume attached to one end of the bar is proposed to be a flat structure. All
nebular components share the same kinematics, with an isotropic velocity field
which monotonically increases with distance from the star before reaching a
plateau. The relatively low velocities indicate that the observed shapes do not
require particularly energetic processes and there is no indication for the
current presence of a jet. The 3D model reproduces the observed line ratios and
the detailed structure of the object significantly better than previous models.
