SN 2024iss: A Double-peaked Type IIb Supernova with Evidence of Circumstellar Interaction
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| Format: | Preprint |
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2025
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| author | Chen, Liyang Wang, Xiaofeng Wu, Qinyu Andrews, Moira Farah, Joseph Ochner, Paolo Reguitti, Andrea Brink, Thomas G. Zhang, Jujia Song, Cuiying Liu, Jialian Filippenko, Alexei V. Sand, David J. Albanese, Irene Alexander, Kate D. Andrews, Jennifer Bostroem, K. Azalee Cai, Yongzhi Christy, Collin Esamdin, Ali Farina, Andrea Franz, Noah Howell, D. Andrew Hsu, Brian Hu, Maokai Iskandar, Abdusamatjan Li, Liping Li, Gaici Li, Dongyue Li, Wenxiong Liu, Jinzhong McCully, Curtis Newsome, Megan Ni, Yuan Qi Pastorello, Andrea Gonzalez, Estefania Padilla Pearson, Jeniveve Peng, Haowei Ransome, Conor Shrestha, Manisha Smith, Nathan Subrayan, Bhagya Terreran, Giacomo Valerin, Giorgio Vinkó, J. Vasylyev, Sergiy S. Wang, Letian Wang, Zhenyu Wang, Hao Wheeler, J. Craig Wynn, Kathryn Xiang, Danfeng Yan, Shengyu Yuan, Weimin Zhang, Juan Zheng, WeiKang Zhang, Yu |
| author_facet | Chen, Liyang Wang, Xiaofeng Wu, Qinyu Andrews, Moira Farah, Joseph Ochner, Paolo Reguitti, Andrea Brink, Thomas G. Zhang, Jujia Song, Cuiying Liu, Jialian Filippenko, Alexei V. Sand, David J. Albanese, Irene Alexander, Kate D. Andrews, Jennifer Bostroem, K. Azalee Cai, Yongzhi Christy, Collin Esamdin, Ali Farina, Andrea Franz, Noah Howell, D. Andrew Hsu, Brian Hu, Maokai Iskandar, Abdusamatjan Li, Liping Li, Gaici Li, Dongyue Li, Wenxiong Liu, Jinzhong McCully, Curtis Newsome, Megan Ni, Yuan Qi Pastorello, Andrea Gonzalez, Estefania Padilla Pearson, Jeniveve Peng, Haowei Ransome, Conor Shrestha, Manisha Smith, Nathan Subrayan, Bhagya Terreran, Giacomo Valerin, Giorgio Vinkó, J. Vasylyev, Sergiy S. Wang, Letian Wang, Zhenyu Wang, Hao Wheeler, J. Craig Wynn, Kathryn Xiang, Danfeng Yan, Shengyu Yuan, Weimin Zhang, Juan Zheng, WeiKang Zhang, Yu |
| contents | We present optical, ultraviolet, and X-ray observations of supernova (SN) 2024iss, a Type IIb SN that shows a prominent double-peaked light curve. We modeled the first peak with a semianalytical shock-cooling model and the X-ray emission with a free-free model. We compare the envelope radius and mass-loss rate with other Type IIb SNe to explore the relationships between the progenitor envelope and the circumstellar material (CSM). The shock-cooling peak in the $V$-band light curve reached $M_V = -17.33\pm 0.26$mag, while the $^{56}$Ni-powered second peak attained $M_V = -17.43\pm 0.26$mag. Early spectra show an photospheric velocity of $\sim19,400\,km\,s^{-1}$ at 3.82days from the H$α$ P~Cygni profile. The Balmer lines persist at least +87 days after the explosion, characterizing hydrogen-rich ejecta. Modeling the first light-curve peak suggests an extended envelope with a mass of $0.11\pm0.04\,M_{\odot}$ and a radius of $244\pm43~R_{\odot}$. Fitting the second light-curve peak with an Arnett-like model indicates a typical $^{56}$Ni mass of $ 0.117\pm0.013~M_{\odot}$ and a relatively low ejecta mass of $1.272\pm0.343\,M_{\odot}$. X-ray observations reveal bright thermal bremsstrahlung emission and indicate a mass-loss rate of $1.6\times10^{-5}\ M_{\odot} \ \rm{yr}^{-1}$. SN 2024iss occupies a transitional position between the two subclasses of extended (eIIb) and compact (cIIb) Type IIb SNe. Its envelope radius and pre-explosion mass-loss rate appear to be correlated as theoretically predicted. The observational properties of SN 2024iss are compatible with a binary interaction scenario being the dominant mechanism for envelope stripping. Furthermore, the low column density of neutral hydrogen suggests a compact CSM with an outer radius of $\lesssim1.3\times10^{14}$ cm, indicating that the progenitor star experienced eruptive mass loss within $\sim4\,yr$ of its terminal explosion. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_22997 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | SN 2024iss: A Double-peaked Type IIb Supernova with Evidence of Circumstellar Interaction Chen, Liyang Wang, Xiaofeng Wu, Qinyu Andrews, Moira Farah, Joseph Ochner, Paolo Reguitti, Andrea Brink, Thomas G. Zhang, Jujia Song, Cuiying Liu, Jialian Filippenko, Alexei V. Sand, David J. Albanese, Irene Alexander, Kate D. Andrews, Jennifer Bostroem, K. Azalee Cai, Yongzhi Christy, Collin Esamdin, Ali Farina, Andrea Franz, Noah Howell, D. Andrew Hsu, Brian Hu, Maokai Iskandar, Abdusamatjan Li, Liping Li, Gaici Li, Dongyue Li, Wenxiong Liu, Jinzhong McCully, Curtis Newsome, Megan Ni, Yuan Qi Pastorello, Andrea Gonzalez, Estefania Padilla Pearson, Jeniveve Peng, Haowei Ransome, Conor Shrestha, Manisha Smith, Nathan Subrayan, Bhagya Terreran, Giacomo Valerin, Giorgio Vinkó, J. Vasylyev, Sergiy S. Wang, Letian Wang, Zhenyu Wang, Hao Wheeler, J. Craig Wynn, Kathryn Xiang, Danfeng Yan, Shengyu Yuan, Weimin Zhang, Juan Zheng, WeiKang Zhang, Yu High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We present optical, ultraviolet, and X-ray observations of supernova (SN) 2024iss, a Type IIb SN that shows a prominent double-peaked light curve. We modeled the first peak with a semianalytical shock-cooling model and the X-ray emission with a free-free model. We compare the envelope radius and mass-loss rate with other Type IIb SNe to explore the relationships between the progenitor envelope and the circumstellar material (CSM). The shock-cooling peak in the $V$-band light curve reached $M_V = -17.33\pm 0.26$mag, while the $^{56}$Ni-powered second peak attained $M_V = -17.43\pm 0.26$mag. Early spectra show an photospheric velocity of $\sim19,400\,km\,s^{-1}$ at 3.82days from the H$α$ P~Cygni profile. The Balmer lines persist at least +87 days after the explosion, characterizing hydrogen-rich ejecta. Modeling the first light-curve peak suggests an extended envelope with a mass of $0.11\pm0.04\,M_{\odot}$ and a radius of $244\pm43~R_{\odot}$. Fitting the second light-curve peak with an Arnett-like model indicates a typical $^{56}$Ni mass of $ 0.117\pm0.013~M_{\odot}$ and a relatively low ejecta mass of $1.272\pm0.343\,M_{\odot}$. X-ray observations reveal bright thermal bremsstrahlung emission and indicate a mass-loss rate of $1.6\times10^{-5}\ M_{\odot} \ \rm{yr}^{-1}$. SN 2024iss occupies a transitional position between the two subclasses of extended (eIIb) and compact (cIIb) Type IIb SNe. Its envelope radius and pre-explosion mass-loss rate appear to be correlated as theoretically predicted. The observational properties of SN 2024iss are compatible with a binary interaction scenario being the dominant mechanism for envelope stripping. Furthermore, the low column density of neutral hydrogen suggests a compact CSM with an outer radius of $\lesssim1.3\times10^{14}$ cm, indicating that the progenitor star experienced eruptive mass loss within $\sim4\,yr$ of its terminal explosion. |
| title | SN 2024iss: A Double-peaked Type IIb Supernova with Evidence of Circumstellar Interaction |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2510.22997 |