Low velocity streams inside the planetary nebula H 2-18. A 3D photoionization and kinematical reconstruction

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.