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| Autores principales: | , , , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| Materias: | |
| Acceso en línea: | https://arxiv.org/abs/2504.01063 |
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| _version_ | 1866908295688617984 |
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| author | Schwab, Michaela Kwok, Lindsey A. Jha, Saurabh W. McCully, Curtis Graur, Or Foley, Ryan J. Camacho-Neves, Yssavo Newman, Max J. B. Larison, Conor Sears, Huei |
| author_facet | Schwab, Michaela Kwok, Lindsey A. Jha, Saurabh W. McCully, Curtis Graur, Or Foley, Ryan J. Camacho-Neves, Yssavo Newman, Max J. B. Larison, Conor Sears, Huei |
| contents | Type Iax supernovae (SNe Iax) are thermonuclear explosions of white dwarfs, peculiar and underluminous compared to the normal type Ia supernovae. Observations of SNe Iax provide insight into the physics of white-dwarf explosions and suggest that some may not be terminal events. Late-time photometry ($\sim$1400 days post-peak) of the type Iax SN 2012Z, the only white dwarf supernova with a pre-explosion detection of a progenitor system, revealed a flux excess that may be explained by a gravitationally bound remnant driving a radioactively powered wind. We present further late-time Hubble Space Telescope photometry of SN 2012Z, $\sim$2500 days after the explosion, and find that the SN is still brighter than, but trending towards, the pre-explosion flux. Additionally, we observe that the excess F555W flux seen in previous data has grown more pronounced. The color of the excess flux disfavors a light echo or interaction with the circumstellar material. The decline rate of the excess flux is consistent with energy deposition from $^{55}$Fe, but the luminosity is higher than expected from models of the ejecta, further suggesting evidence for a bound remnant. Combining our data with future observations should allow for the detection of emission from the ejecta shock-heating of the companion helium star seen in the progenitor system. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_01063 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Remarkable Late-Time Flux Excess in Hubble Space Telescope Observations of the Type Iax Supernova 2012Z Schwab, Michaela Kwok, Lindsey A. Jha, Saurabh W. McCully, Curtis Graur, Or Foley, Ryan J. Camacho-Neves, Yssavo Newman, Max J. B. Larison, Conor Sears, Huei High Energy Astrophysical Phenomena Type Iax supernovae (SNe Iax) are thermonuclear explosions of white dwarfs, peculiar and underluminous compared to the normal type Ia supernovae. Observations of SNe Iax provide insight into the physics of white-dwarf explosions and suggest that some may not be terminal events. Late-time photometry ($\sim$1400 days post-peak) of the type Iax SN 2012Z, the only white dwarf supernova with a pre-explosion detection of a progenitor system, revealed a flux excess that may be explained by a gravitationally bound remnant driving a radioactively powered wind. We present further late-time Hubble Space Telescope photometry of SN 2012Z, $\sim$2500 days after the explosion, and find that the SN is still brighter than, but trending towards, the pre-explosion flux. Additionally, we observe that the excess F555W flux seen in previous data has grown more pronounced. The color of the excess flux disfavors a light echo or interaction with the circumstellar material. The decline rate of the excess flux is consistent with energy deposition from $^{55}$Fe, but the luminosity is higher than expected from models of the ejecta, further suggesting evidence for a bound remnant. Combining our data with future observations should allow for the detection of emission from the ejecta shock-heating of the companion helium star seen in the progenitor system. |
| title | The Remarkable Late-Time Flux Excess in Hubble Space Telescope Observations of the Type Iax Supernova 2012Z |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2504.01063 |