Using Nebular Near-infrared Spectroscopy to Measure Asymmetric Chemical Distributions in 2003fg-like Thermonuclear Supernovae
We present an analysis of three near-infrared (NIR; 1.0-2.4 μm) spectra of the SN 2003fg-like/“super-Chandrasekhar” Type Ia supernovae (SNe Ia) SN 2009dc, SN 2020hvf, and SN 2022pul at respective phases of +372, +296, and +294 days relative to the epoch of B-band maximum. We find that all objects in...
| Autores: | , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2025 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/394091 |
| Acceso en línea: | http://hdl.handle.net/10261/394091 https://api.elsevier.com/content/abstract/scopus_id/105003559663 |
| Access Level: | acceso abierto |
| Palabra clave: | Core-collapse supernovae Supernovae http://astrothesaurus.org/uat/304 http://astrothesaurus.org/uat/1668 |
| Sumario: | We present an analysis of three near-infrared (NIR; 1.0-2.4 μm) spectra of the SN 2003fg-like/“super-Chandrasekhar” Type Ia supernovae (SNe Ia) SN 2009dc, SN 2020hvf, and SN 2022pul at respective phases of +372, +296, and +294 days relative to the epoch of B-band maximum. We find that all objects in our sample have asymmetric, or “tilted,” [Fe ii] 1.257 and 1.644 μm profiles. We quantify the asymmetry of these features using five methods: velocity at peak flux, profile tilts, residual testing, velocity fitting, and comparison to deflagration-detonation transition models. Our results demonstrate that, while the profiles of the [Fe ii] 1.257 and 1.644 μm features are widely varied between 2003fg-likes, these features are correlated in shape within the same SNe. This implies that line blending is most likely not the dominant cause of the asymmetries inferred from these profiles. Instead, it is more plausible that 2003fg-like SNe have aspherical chemical distributions in their inner regions. These distributions may come from aspherical progenitor systems, such as double white dwarf mergers, or off-center delayed-detonation explosions of near-Chandrasekhar mass carbon-oxygen white dwarfs. Additional late-phase NIR observation of 2003fg-like SNe and detailed 3D non-LTE modeling of these two explosion scenarios are encouraged. |
|---|