WFST Supernovae in the First Year: III. Systematical Study of the Photometric Behavior of Early-phase Core-collapse Supernovae
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arXiv
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| Format: | Preprint |
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2026
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| _version_ | 1866911457043546112 |
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| author | Zhao, Junhan Jiang, Ji-an Xu, Zelin Zhang, Yu-Hao Fang, Qiliang Liu, Liang-Duan Zhu, Qingfeng Yu, Yun-Wei Maeda, Keiichi Galbany, Lluís Kuncarayakti, Hanindyo Ivezić, Željko Jha, Saurabh W. Yoachim, Peter Meng, Dezheng Wu, Weiyu Liu, Zhengyan Connolly, Andrew J. Jia, Ziqing Zhao, Wen Fan, Lulu Liang, Ming Wang, Hairen Wang, Jian Zhang, Hongfei |
| author_facet | Zhao, Junhan Jiang, Ji-an Xu, Zelin Zhang, Yu-Hao Fang, Qiliang Liu, Liang-Duan Zhu, Qingfeng Yu, Yun-Wei Maeda, Keiichi Galbany, Lluís Kuncarayakti, Hanindyo Ivezić, Željko Jha, Saurabh W. Yoachim, Peter Meng, Dezheng Wu, Weiyu Liu, Zhengyan Connolly, Andrew J. Jia, Ziqing Zhao, Wen Fan, Lulu Liang, Ming Wang, Hairen Wang, Jian Zhang, Hongfei |
| contents | We investigate the multiband photometric properties of seven supernovae (SNe) showing double-peaked light-curve evolution and prominent shock-cooling emission, observed by the Wide Field Survey Telescope (WFST) during its first year of operation. By jointly employing an analytic early shock-cooling model and the Arnett radioactive-diffusion model, we fit the bolometric light curves and infer ejecta masses in the range $1.1$-$2.6 M_\odot$, consistent with a transitional population between ultra-stripped supernovae (USSNe) and normal stripped-envelope supernovae (SESNe). The envelope masses are estimated to be $M_{\rm env}=0.1$-$0.4 M_\odot$, while the progenitors are constrained to be yellow or blue supergiants (YSGs/BSGs) with radii of $R=120$-$300 R_\odot$. Using empirical relations, we estimate progenitor luminosities of $L=10^{4.6}$-$10^{4.9} L_\odot$, corresponding to zero-age main-sequence (ZAMS) masses of $8$-$20 M_\odot$. Theoretical models suggest that such progenitors are more naturally produced through binary evolution channels, as single-star evolutionary pathways are unable to yield ejecta masses this low. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2602_17275 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | WFST Supernovae in the First Year: III. Systematical Study of the Photometric Behavior of Early-phase Core-collapse Supernovae Zhao, Junhan Jiang, Ji-an Xu, Zelin Zhang, Yu-Hao Fang, Qiliang Liu, Liang-Duan Zhu, Qingfeng Yu, Yun-Wei Maeda, Keiichi Galbany, Lluís Kuncarayakti, Hanindyo Ivezić, Željko Jha, Saurabh W. Yoachim, Peter Meng, Dezheng Wu, Weiyu Liu, Zhengyan Connolly, Andrew J. Jia, Ziqing Zhao, Wen Fan, Lulu Liang, Ming Wang, Hairen Wang, Jian Zhang, Hongfei High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We investigate the multiband photometric properties of seven supernovae (SNe) showing double-peaked light-curve evolution and prominent shock-cooling emission, observed by the Wide Field Survey Telescope (WFST) during its first year of operation. By jointly employing an analytic early shock-cooling model and the Arnett radioactive-diffusion model, we fit the bolometric light curves and infer ejecta masses in the range $1.1$-$2.6 M_\odot$, consistent with a transitional population between ultra-stripped supernovae (USSNe) and normal stripped-envelope supernovae (SESNe). The envelope masses are estimated to be $M_{\rm env}=0.1$-$0.4 M_\odot$, while the progenitors are constrained to be yellow or blue supergiants (YSGs/BSGs) with radii of $R=120$-$300 R_\odot$. Using empirical relations, we estimate progenitor luminosities of $L=10^{4.6}$-$10^{4.9} L_\odot$, corresponding to zero-age main-sequence (ZAMS) masses of $8$-$20 M_\odot$. Theoretical models suggest that such progenitors are more naturally produced through binary evolution channels, as single-star evolutionary pathways are unable to yield ejecta masses this low. |
| title | WFST Supernovae in the First Year: III. Systematical Study of the Photometric Behavior of Early-phase Core-collapse Supernovae |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2602.17275 |