Morpho-kinematics of the planetary nebula NGC 3242: an analysis beyond
  its multiple-shell structure
  In this paper we present the results of optical high-resolution imaging and
spectroscopy of the complex planetary nebula (PN) NGC~3242. Our study is based
on the analysis of the narrowband H$\alpha$ $\lambda$6563\AA , [O III]
$\lambda$5007\AA , [N II] $\lambda$6584\AA , and [S II] $\lambda$6724{\AA}
images, and high- resolution spectroscopy using spectral ranges centered on the
H$\alpha$ $\lambda$6564\AA , [N II] $\lambda$6583\AA , and [O III]
$\lambda$5007\AA . We detected and analysed morphological components beyond the
multiple shell structure of this PN, to investigate the small-scale
morphological components aligned towards its major axis (such as knots and
ansae, as well as the arc-like features) and its surroundings. Thus, we
investigated the morpho-kinematical properties of NGC~3242, as well as their
nature and formation. Our results regarding the elliptical double-shell
structure and the distance to this nebula are in concordance with previous
studies. Furthermore, we have used the software SHAPE to construct a 3D model
of NGC~3242, allowing us to successfully reproduce our observational data. We
conclude that the prominent knots emitting in the [N II] line are fast,
low-ionisation emission regions (FLIERs) related to high velocity jets and the
so-called ansae-like features rather resemble bubbles. The disruptions immersed
in the halo, whose emission was detected in the the [O III] high-excitation
emission line, remarkably display high velocities and were formed likely in an
earlier ejection event, in comparison to the innermost FLIERs and bubbles.
Finally, according to our model, the kinematical ages of the structures in
NGC~3242 range from 390 to 5400 yr.
