SN 2024iss: A Multi-Wavelength Exposé of a Type IIb Supernova with an Early-Time Ultraviolet Spectrum and Shock Breakout Constraints
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2026
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| author | Yete, Rujula Jacobson-Galan, Wynn Ferdinand, Ferdinand Dessart, Luc Kasliwal, Mansi Davis, Kyle Piro, Anthony Villar, Victoria Andreoni, Igor Auchettl, Katie Chambers, Kenneth Chornock, Ryan Coughlin, Michael Coulter, David Dekany, Richard Foley, Ryan Fox, Ori Galbany, Lluís Gall, Christa Gangopadhyay, Anjasha Goldberg, Jared Govindaraj, Gowri Guo, Xinze Huber, Mark Jaimes, Joahan Karcheski, Jenna Kaur, Ravjit Kilpatrick, Charles Laher, Russ LeBaron, Natalie Lin, Chien-Cheng Margutti, Raffaella Pan, Yen-Chen Patra, Kishore Perkins, Haille Pessi, Priscila Pyshna, Oleksandra Rest, Armin Romagnoli, Sara Schulze, Steve Sears, Huei Sedgewick, Aidan Siebert, Matthew Singh, Avinash Sollerman, Jesper Sravan, Niharika Tinyanont, Samaporn Wainscoat, Richard Wang, Qinan Warshofsky, Daniel Yao, Yuhan Zenati, Yossef |
| author_facet | Yete, Rujula Jacobson-Galan, Wynn Ferdinand, Ferdinand Dessart, Luc Kasliwal, Mansi Davis, Kyle Piro, Anthony Villar, Victoria Andreoni, Igor Auchettl, Katie Chambers, Kenneth Chornock, Ryan Coughlin, Michael Coulter, David Dekany, Richard Foley, Ryan Fox, Ori Galbany, Lluís Gall, Christa Gangopadhyay, Anjasha Goldberg, Jared Govindaraj, Gowri Guo, Xinze Huber, Mark Jaimes, Joahan Karcheski, Jenna Kaur, Ravjit Kilpatrick, Charles Laher, Russ LeBaron, Natalie Lin, Chien-Cheng Margutti, Raffaella Pan, Yen-Chen Patra, Kishore Perkins, Haille Pessi, Priscila Pyshna, Oleksandra Rest, Armin Romagnoli, Sara Schulze, Steve Sears, Huei Sedgewick, Aidan Siebert, Matthew Singh, Avinash Sollerman, Jesper Sravan, Niharika Tinyanont, Samaporn Wainscoat, Richard Wang, Qinan Warshofsky, Daniel Yao, Yuhan Zenati, Yossef |
| contents | We present multi-wavelength observations and a comprehensive analysis of the nearby (D$\sim$14 Mpc) Type IIb supernova (SN IIb) 2024iss. Observations of SN2024iss include an early ZTF detection at $\sim$40 minutes after first light and the earliest Hubble Space Telescope UV spectrum for a SN IIb to date at 7 days after first light. With the bolometric light curve and He-star models, we estimate an ejecta mass range of $\sim 1.1-3.3~M_{\odot}$ and a $^{56}\textrm{Ni}$ mass of $0.11 \pm 0.01~M_{\odot}$. We fit shock-cooling emission models to the first peak in the light curve and estimate a progenitor radius of $100-320~R_{\odot}$ and a H-rich envelope mass of $0.07-0.46~M_{\odot}$. We also compared optical/UV spectra to binary progenitor model spectra, which indicate a stripped H-rich envelope mass of $0.19-0.28~M_{\odot}$. We use early-time X-ray detections to calculate CSM densities that are consistent with a progenitor mass-loss rate of $5\times10^{-4}~M_{\odot}$ ($v_w = 100~$km/s), corresponding to a period of significant mass ejection in the final ~2-5 years before core collapse. In the UV spectrum, we observe strong Mg II emission extending to $\sim15,000 ~$km/s as well as weak P-Cygni profiles of iron-group elements (e.g., Fe, Ti, Al, Ni) present in the outer SN ejecta during the end of shock cooling phase. We find that the overall spectroscopic evolution of SN2024iss is comparable to other SNe IIb, but that the increased brightness following the initial light curve peak is likely influenced by SN ejecta-CSM interaction. Finally, optical/NIR nebular spectroscopy of SN2024iss at $\sim 260-412~$ days reveals multi-peaked forbidden line profiles of O I and Mg I] indicative of inner ejecta asymmetry and/or clumping. We demonstrate the utility of a rich, multi-wavelength dataset for constraining the progenitor systems and explosion dynamics of SNe IIb. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2603_20375 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | SN 2024iss: A Multi-Wavelength Exposé of a Type IIb Supernova with an Early-Time Ultraviolet Spectrum and Shock Breakout Constraints Yete, Rujula Jacobson-Galan, Wynn Ferdinand, Ferdinand Dessart, Luc Kasliwal, Mansi Davis, Kyle Piro, Anthony Villar, Victoria Andreoni, Igor Auchettl, Katie Chambers, Kenneth Chornock, Ryan Coughlin, Michael Coulter, David Dekany, Richard Foley, Ryan Fox, Ori Galbany, Lluís Gall, Christa Gangopadhyay, Anjasha Goldberg, Jared Govindaraj, Gowri Guo, Xinze Huber, Mark Jaimes, Joahan Karcheski, Jenna Kaur, Ravjit Kilpatrick, Charles Laher, Russ LeBaron, Natalie Lin, Chien-Cheng Margutti, Raffaella Pan, Yen-Chen Patra, Kishore Perkins, Haille Pessi, Priscila Pyshna, Oleksandra Rest, Armin Romagnoli, Sara Schulze, Steve Sears, Huei Sedgewick, Aidan Siebert, Matthew Singh, Avinash Sollerman, Jesper Sravan, Niharika Tinyanont, Samaporn Wainscoat, Richard Wang, Qinan Warshofsky, Daniel Yao, Yuhan Zenati, Yossef High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We present multi-wavelength observations and a comprehensive analysis of the nearby (D$\sim$14 Mpc) Type IIb supernova (SN IIb) 2024iss. Observations of SN2024iss include an early ZTF detection at $\sim$40 minutes after first light and the earliest Hubble Space Telescope UV spectrum for a SN IIb to date at 7 days after first light. With the bolometric light curve and He-star models, we estimate an ejecta mass range of $\sim 1.1-3.3~M_{\odot}$ and a $^{56}\textrm{Ni}$ mass of $0.11 \pm 0.01~M_{\odot}$. We fit shock-cooling emission models to the first peak in the light curve and estimate a progenitor radius of $100-320~R_{\odot}$ and a H-rich envelope mass of $0.07-0.46~M_{\odot}$. We also compared optical/UV spectra to binary progenitor model spectra, which indicate a stripped H-rich envelope mass of $0.19-0.28~M_{\odot}$. We use early-time X-ray detections to calculate CSM densities that are consistent with a progenitor mass-loss rate of $5\times10^{-4}~M_{\odot}$ ($v_w = 100~$km/s), corresponding to a period of significant mass ejection in the final ~2-5 years before core collapse. In the UV spectrum, we observe strong Mg II emission extending to $\sim15,000 ~$km/s as well as weak P-Cygni profiles of iron-group elements (e.g., Fe, Ti, Al, Ni) present in the outer SN ejecta during the end of shock cooling phase. We find that the overall spectroscopic evolution of SN2024iss is comparable to other SNe IIb, but that the increased brightness following the initial light curve peak is likely influenced by SN ejecta-CSM interaction. Finally, optical/NIR nebular spectroscopy of SN2024iss at $\sim 260-412~$ days reveals multi-peaked forbidden line profiles of O I and Mg I] indicative of inner ejecta asymmetry and/or clumping. We demonstrate the utility of a rich, multi-wavelength dataset for constraining the progenitor systems and explosion dynamics of SNe IIb. |
| title | SN 2024iss: A Multi-Wavelength Exposé of a Type IIb Supernova with an Early-Time Ultraviolet Spectrum and Shock Breakout Constraints |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2603.20375 |