Planetary Nebulae of the Large Magellanic Cloud I: A multiwavelength analysis
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| Autores principales: | , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2024
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| _version_ | 1866911891020840960 |
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| author | Tosi, Silvia Dell'Agli, Flavia Kamath, Devika Stanghellini, Letizia Ventura, Paolo Bianchi, Stefano Gómez-Muñoz, Marco A. García-Hernández, D. A. |
| author_facet | Tosi, Silvia Dell'Agli, Flavia Kamath, Devika Stanghellini, Letizia Ventura, Paolo Bianchi, Stefano Gómez-Muñoz, Marco A. García-Hernández, D. A. |
| contents | Planetary nebulae (PNe) have three main components: a central star (CS), ionised gas and dust in the nebula. Each of them contains critical chemical fingerprints of their evolution, serving as tracers of the evolution, nucleosynthesis and dust production that occurred during the preceding asymptotic giant branch (AGB) phase. We aim to build a bridge to link the PN phase to the evolution of their progenitors, trying to better understand the dust production and mass-loss mechanism during the final AGB phase. Here, we present a comprehensive study of nine Large Magellanic Cloud (LMC) spherical or elliptical PNe whose observations from the ultraviolet (UV) through the infrared (IR) are available in the literature. We characterize nebulae and CSs, finding information as the amount of gas that makes up the nebula and the dust that surrounds the CS, necessary to reconstruct the evolutionary history of mass-loss and dust production. We compare the observed energy distribution of the selected PNe to that obtained from photoionization modeling, taking into account the presence of dust. The physical and chemical parameters of the central stars are then compared with the predictions from the evolutionary tracks. We characterized the source, assigning to each CS a progenitor, early-AGB mass. We estimated the mass of the nebula and the dust-to-gas ratio. For 5 objects, we find evidence for the presence of a near-IR bump, which would be connected to the presence of hot dust. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_03640 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Planetary Nebulae of the Large Magellanic Cloud I: A multiwavelength analysis Tosi, Silvia Dell'Agli, Flavia Kamath, Devika Stanghellini, Letizia Ventura, Paolo Bianchi, Stefano Gómez-Muñoz, Marco A. García-Hernández, D. A. Astrophysics of Galaxies Solar and Stellar Astrophysics Planetary nebulae (PNe) have three main components: a central star (CS), ionised gas and dust in the nebula. Each of them contains critical chemical fingerprints of their evolution, serving as tracers of the evolution, nucleosynthesis and dust production that occurred during the preceding asymptotic giant branch (AGB) phase. We aim to build a bridge to link the PN phase to the evolution of their progenitors, trying to better understand the dust production and mass-loss mechanism during the final AGB phase. Here, we present a comprehensive study of nine Large Magellanic Cloud (LMC) spherical or elliptical PNe whose observations from the ultraviolet (UV) through the infrared (IR) are available in the literature. We characterize nebulae and CSs, finding information as the amount of gas that makes up the nebula and the dust that surrounds the CS, necessary to reconstruct the evolutionary history of mass-loss and dust production. We compare the observed energy distribution of the selected PNe to that obtained from photoionization modeling, taking into account the presence of dust. The physical and chemical parameters of the central stars are then compared with the predictions from the evolutionary tracks. We characterized the source, assigning to each CS a progenitor, early-AGB mass. We estimated the mass of the nebula and the dust-to-gas ratio. For 5 objects, we find evidence for the presence of a near-IR bump, which would be connected to the presence of hot dust. |
| title | Planetary Nebulae of the Large Magellanic Cloud I: A multiwavelength analysis |
| topic | Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2405.03640 |