2025/03/26 by H. Monteiro, Cristina Mendes de Oliveira, Monteiro, H. +15
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Photocathodes and Microchannel Plates #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.2503.20640
openalex publication_date 2025/03/26 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present a detailed 3D photoionization model of the planetary nebula NGC 3132, constrained by the latest observations. Using the MOCASSIN code, the model incorporates integrated and spatially resolved spectroscopy, velocity-resolved line profiles, emission line maps, and photometry, including recent high-quality data from MUSE (VLT) and JWST among others. Based on new data from the SAMFP instrument at SOAR, the three-dimensional density structure of the nebula was obtained by assuming homologous expansion of the surrounding nebular gas. The final fitted model successfully reproduces all key observational constraints available, particularly in terms of the detailed emission line integrated fluxes and ionization structures across different ionic stages. The results of the model show that the progenitor star had a mass of (2.7 ± 0.2)M\odot and is surrounded by a He poor shell of dust and gas. The abundances of He, C, N, O, and S determined by the model show that the nebula has C/O=(2.02 ± 0.28) and N/O=(0.39 ± 0.38) consistent with the progenitor mass found.