Morpho-kinematics of the planetary nebula NGC 3242: an analysis beyond its multiple-shell structure

TL;DR

This study combines high-resolution imaging and spectroscopy to analyze the complex morphology and kinematics of planetary nebula NGC 3242, revealing detailed structures, their dynamics, and formation history through 3D modeling.

Contribution

It provides a comprehensive 3D morpho-kinematical model of NGC 3242, extending understanding beyond its multiple-shell structure and identifying new features like knots and ansae.

Findings

Knots are fast, low-ionisation emission regions (FLIERs) related to high velocity jets.

Halo disruptions display high velocities, likely from earlier ejection events.

Kinematic ages of structures range from 390 to 5400 years.

Abstract

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.