HST/WFPC2 imaging analysis and Cloudy modelling of the multiple shell planetary nebulae NGC 3242, NGC 6826 and NGC 7662

TL;DR

This study combines high-resolution imaging and photoionisation modelling to analyze the structure and physical conditions of three complex planetary nebulae, revealing insights into shock regions and nebular properties.

Contribution

It provides a detailed analysis of multiple shell planetary nebulae using HST imaging and Cloudy models, highlighting the role of shocks and inhomogeneities in nebular emission.

Findings

Shocked regions correlate with FLIERs and LISs.

Photoionisation models fit [O III] and H alpha profiles well.

Discrepancies in [N II] and [S II] profiles suggest gas inhomogeneities or UV leakage.

Abstract

We performed a detailed photometric analysis and photoionisation modelling on three high excitation multiple shell planetary nebulae: NGC 3242, NGC 6826 and NGC 7662. Archival HST/WFPC2 narrow band filter images were used to investigate shocked regions by two independent methods: using low excitation ions (via H alpha/[N II] vs H alpha/[S II] extended diagnostic diagrams) and by means of high excitation species looking for regions of enhanced [O III]/H alpha line ratios. Shocked region analysis via low excitation ions shows that major deviations from the general inside to outside ionisation trend correspond only to regions where FLIERs or LISs are located. The reduction on the SNR at the outskirts of the [O III]/H alpha ratio maps, made us unable to unambiguously identified for an enhancement on the [O III]/H alpha line ratio as an indicator for shocks. For non-shocked regions we performed a photoionisation modelling using Cloudy. Fittings to the [O III] and H alpha observed radial profiles lead us to constrain on the free parameters of the density laws and filling factors together to temperatures and luminosities for the CSPNe. Best fit models show a very well representation of the [O III] and H alpha emission. Discrepancies in the model fittings to the [N II] and [S II] profiles at NGC 6826 and NGC 3242, can be attributed in the former case, due to a contamination by the light of the CSPN and, in the latter case, either due to gas inhomogeneities within the clumps or to a leaking of UV radiation.