2025MNRAS.541.1628B

Central to our understanding of stellar evolution and its impact on processes in our Galaxy and across the Universe is the study of mass-loss. While the general framework is well established, recent JWST observations of objects like NGC 3132 have revealed intricate nebular structures, suggesting complex mass-loss processes likely driven by multiple star system at its core. These findings pose new challenges for the currently available investigation tools. The primary goal of this study is the first detailed comparison of the physical properties and chemical composition obtained for NGC 3132, based on the latest detailed 3D model and observations from MUSE, JWST, and Spitzer. We evaluate the reliability of the traditional empirical method and photoionization model for abundances estimations, both based on the same available high-quality spatially resolved observations. We find that the model and empirical method yield consistent results for the integrated total properties such as $T_{\rm e}$, $n_{\rm e}$, and chemical abundances. However, when applied to simulated observations from the model, the empirical method fails to recover the model input abundances, providing only an approximate estimate. This discrepancy arises in part from the loss of information when summing fluxes over regions that have complex ionization structures. This discrepancy in the case of oxygen has been estimated to be up to 35 per cent. Moreover, the latest IR data reveal a spatial correlation between H$_2$, c(H $\beta$), and the [8.0]/[4.5] IRAC ratio. Finally, new clumps are discovered in [Ni II] 7378 Å, [Fe II] 8617 Å, and [Fe III] 5270 Å emission lines.