Saved in:
| Main Authors: | , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | https://arxiv.org/abs/2503.13017 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866910885314822144 |
|---|---|
| author | Michel, Philip D. Mazzali, Paolo A. Perley, Daniel A. Hinds, K-Ryan Wise, Jacob L. |
| author_facet | Michel, Philip D. Mazzali, Paolo A. Perley, Daniel A. Hinds, K-Ryan Wise, Jacob L. |
| contents | SN 2023ixf is one of the brightest Core Collapse Supernovae of the 21st century and offers a rare opportunity to investigate the late stage of a Supernova through nebular phase spectroscopy. We present four nebular phase spectra from day +291 to +413 after explosion. This is supplemented with high cadence early phase spectroscopic observations and photometry covering the first 500 days to investigate explosion parameters. The narrow and blue-shifted nebular Oxygen emission lines are used to infer an ejected Oxygen mass of $<0.65M_\odot$, consistent with models of a relatively low mass ($M_{ZAMS}<15M_\odot$) progenitor. An energy of 0.3 to $1.4 \times10^{51}$ erg and a light curve powered by an initial $^{56}$Ni mass of $0.049 \pm 0.005 M_\odot$ appear consistent with a relatively standard Type II explosion, while an incomplete $γ$-ray trapping (with timescale of $240\pm4$ days) suggests a lower ejecta mass. Assuming a typical explosion, the broad Hydrogen and Calcium profiles suggest a common origin within a lower mass, partially stripped envelope. Hydrogen emission broadens with time, indicating contribution from an additional power source at an extended distance; while the emergence of high velocity ($\sim$6,000 km s$^{-1}$) Hydrogen emission features (beginning around day +200) may be explained by Shock Interaction with a dense Hydrogen-rich region located at $\sim1.5 \times 10^{16}$cm. Such envelope mass loss for a low mass progenitor may be explained through theoretical models of Binary interaction. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_13017 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The nebular spectra of SN 2023ixf: A lower mass, partially stripped progenitor may be the result of binary interaction Michel, Philip D. Mazzali, Paolo A. Perley, Daniel A. Hinds, K-Ryan Wise, Jacob L. High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics SN 2023ixf is one of the brightest Core Collapse Supernovae of the 21st century and offers a rare opportunity to investigate the late stage of a Supernova through nebular phase spectroscopy. We present four nebular phase spectra from day +291 to +413 after explosion. This is supplemented with high cadence early phase spectroscopic observations and photometry covering the first 500 days to investigate explosion parameters. The narrow and blue-shifted nebular Oxygen emission lines are used to infer an ejected Oxygen mass of $<0.65M_\odot$, consistent with models of a relatively low mass ($M_{ZAMS}<15M_\odot$) progenitor. An energy of 0.3 to $1.4 \times10^{51}$ erg and a light curve powered by an initial $^{56}$Ni mass of $0.049 \pm 0.005 M_\odot$ appear consistent with a relatively standard Type II explosion, while an incomplete $γ$-ray trapping (with timescale of $240\pm4$ days) suggests a lower ejecta mass. Assuming a typical explosion, the broad Hydrogen and Calcium profiles suggest a common origin within a lower mass, partially stripped envelope. Hydrogen emission broadens with time, indicating contribution from an additional power source at an extended distance; while the emergence of high velocity ($\sim$6,000 km s$^{-1}$) Hydrogen emission features (beginning around day +200) may be explained by Shock Interaction with a dense Hydrogen-rich region located at $\sim1.5 \times 10^{16}$cm. Such envelope mass loss for a low mass progenitor may be explained through theoretical models of Binary interaction. |
| title | The nebular spectra of SN 2023ixf: A lower mass, partially stripped progenitor may be the result of binary interaction |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2503.13017 |