SN 2023ixf in the Pinwheel Galaxy M101: From Shock Breakout to the Nebular Phase
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arXiv
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| Natura: | Preprint |
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2025
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| author | Zheng, Weikang Dessart, Luc Filippenko, Alexei V. Yang, Yi Brink, Thomas G. De Jaeger, Thomas Vasylyev, Sergiy S. Van Dyk, Schuyler D. Patra, Kishore C. Jacobson-Galan, Wynn V. Stewart, Gabrielle E. Alvarado III, Efrain Arikatla, Veda Beddow, Pallas Betz, Andreas Born, Emma Bostow, Kate Burgasser, Adam J. Caceres, Osmin Carrasco, Evan M. Chuang, Elma DeGraw, Asia Gates, Elinor L. Gendreau-Distler, Eli Jacobus, Cooper Jennings, Connor Karpoor, Preethi R. Lynam, Paul Mina, Ann Mora, Katherine Pichay, Neil Ravi, Jyotsna Rees, Jon Rich, R. Michael Risin, Sophia Sandford, Nathan R. Savino, Alessandro Softich, Emma Theissen, Christopher A. Vidal, Edgar P. Wu, William Zeng, Yoomee |
| author_facet | Zheng, Weikang Dessart, Luc Filippenko, Alexei V. Yang, Yi Brink, Thomas G. De Jaeger, Thomas Vasylyev, Sergiy S. Van Dyk, Schuyler D. Patra, Kishore C. Jacobson-Galan, Wynn V. Stewart, Gabrielle E. Alvarado III, Efrain Arikatla, Veda Beddow, Pallas Betz, Andreas Born, Emma Bostow, Kate Burgasser, Adam J. Caceres, Osmin Carrasco, Evan M. Chuang, Elma DeGraw, Asia Gates, Elinor L. Gendreau-Distler, Eli Jacobus, Cooper Jennings, Connor Karpoor, Preethi R. Lynam, Paul Mina, Ann Mora, Katherine Pichay, Neil Ravi, Jyotsna Rees, Jon Rich, R. Michael Risin, Sophia Sandford, Nathan R. Savino, Alessandro Softich, Emma Theissen, Christopher A. Vidal, Edgar P. Wu, William Zeng, Yoomee |
| contents | We present photometric and spectroscopic observations of SN 2023ixf covering from day one to 442 days after explosion. SN 2023ixf reached a peak $V$-band absolute magnitude of $-18.2 \pm 0.07$, and light curves show that it is in the fast-decliner (IIL) subclass with a relatively short ``plateau'' phase (fewer than $\sim 70$ days). Early-time spectra of SN 2023ixf exhibit strong, very narrow emission lines from ionized circumstellar matter (CSM), possibly indicating a Type IIn classification. But these flash/shock-ionization emission features faded after the first week and the spectrum evolved in a manner similar to that of typical Type II SNe, unlike the case of most genuine SNe~IIn in which the ejecta interact with CSM for an extended period of time and develop intermediate-width emission lines. We compare observed spectra of SN 2023ixf with various model spectra to understand the physics behind SN 2023ixf. Our nebular spectra (between 200-400 d) match best with the model spectra from a 15 $\rm M_{\odot}$ progenitor which experienced enhanced mass loss a few years before explosion. A last-stage mass-loss rate of $\dot{M} = 0.01 \rm M_{\odot} yr^{-1}$ from the r1w6 model matches best with the early-time spectra, higher than $\dot{M} \approx 2.4 \times 10^{-3} \rm M_{\odot} yr^{-1}$ derived from the ionized H$α$ luminosity at 1.58 d. We also use SN 2023ixf as a distance indicator and fit the light curves to derive the Hubble constant by adding SN 2023ixf to the existing sample; we obtain H$_{0}=73.1^{+3.68}_{-3.50}$ km s$^{-1}$ Mpc$^{-1}$, consistent with the results from SNe~Ia and many other independent methods. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_13974 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | SN 2023ixf in the Pinwheel Galaxy M101: From Shock Breakout to the Nebular Phase Zheng, Weikang Dessart, Luc Filippenko, Alexei V. Yang, Yi Brink, Thomas G. De Jaeger, Thomas Vasylyev, Sergiy S. Van Dyk, Schuyler D. Patra, Kishore C. Jacobson-Galan, Wynn V. Stewart, Gabrielle E. Alvarado III, Efrain Arikatla, Veda Beddow, Pallas Betz, Andreas Born, Emma Bostow, Kate Burgasser, Adam J. Caceres, Osmin Carrasco, Evan M. Chuang, Elma DeGraw, Asia Gates, Elinor L. Gendreau-Distler, Eli Jacobus, Cooper Jennings, Connor Karpoor, Preethi R. Lynam, Paul Mina, Ann Mora, Katherine Pichay, Neil Ravi, Jyotsna Rees, Jon Rich, R. Michael Risin, Sophia Sandford, Nathan R. Savino, Alessandro Softich, Emma Theissen, Christopher A. Vidal, Edgar P. Wu, William Zeng, Yoomee Astrophysics of Galaxies High Energy Physics - Phenomenology We present photometric and spectroscopic observations of SN 2023ixf covering from day one to 442 days after explosion. SN 2023ixf reached a peak $V$-band absolute magnitude of $-18.2 \pm 0.07$, and light curves show that it is in the fast-decliner (IIL) subclass with a relatively short ``plateau'' phase (fewer than $\sim 70$ days). Early-time spectra of SN 2023ixf exhibit strong, very narrow emission lines from ionized circumstellar matter (CSM), possibly indicating a Type IIn classification. But these flash/shock-ionization emission features faded after the first week and the spectrum evolved in a manner similar to that of typical Type II SNe, unlike the case of most genuine SNe~IIn in which the ejecta interact with CSM for an extended period of time and develop intermediate-width emission lines. We compare observed spectra of SN 2023ixf with various model spectra to understand the physics behind SN 2023ixf. Our nebular spectra (between 200-400 d) match best with the model spectra from a 15 $\rm M_{\odot}$ progenitor which experienced enhanced mass loss a few years before explosion. A last-stage mass-loss rate of $\dot{M} = 0.01 \rm M_{\odot} yr^{-1}$ from the r1w6 model matches best with the early-time spectra, higher than $\dot{M} \approx 2.4 \times 10^{-3} \rm M_{\odot} yr^{-1}$ derived from the ionized H$α$ luminosity at 1.58 d. We also use SN 2023ixf as a distance indicator and fit the light curves to derive the Hubble constant by adding SN 2023ixf to the existing sample; we obtain H$_{0}=73.1^{+3.68}_{-3.50}$ km s$^{-1}$ Mpc$^{-1}$, consistent with the results from SNe~Ia and many other independent methods. |
| title | SN 2023ixf in the Pinwheel Galaxy M101: From Shock Breakout to the Nebular Phase |
| topic | Astrophysics of Galaxies High Energy Physics - Phenomenology |
| url | https://arxiv.org/abs/2503.13974 |