SN 2024iss: Double-Peaked Light Curves and Implications for a Yellow Supergiant Progenitor
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arXiv
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| Formato: | Preprint |
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2025
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| _version_ | 1866913729791131648 |
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| author | Yamanaka, Masayuki Nagayama, Takahiro Horikiri, Tsukiha |
| author_facet | Yamanaka, Masayuki Nagayama, Takahiro Horikiri, Tsukiha |
| contents | We report the multi-band photometric observations of the Type IIb supernova (SN) 2024iss with ultra-violet (UV), optical, and near-infrared (NIR) wavelengths starting one day after the explosion. The UV and optical light curves show the first peak two days after the explosion date. Following a first peak, a secondary maximum is observed in the optical and NIR bands, similar to SNe IIb with double-peaked light curves. The quasi-bolometric light curve shows the fast decay until a week after the explosion. From the analysis of the bolometric light curve, the ejecta mass and kinetic energy are estimated to be $M_{ej}=2.8\pm0.6~M_{\odot}$ and $E_{kin}=9.4\pm4.1\times10^{50}$ erg. The mass of the radioactive $^{56}$Ni is estimated to be $M(^{56}Ni)=0.2~M_{\odot}$. Fitting a black-body function to the spectral energy distribution reveals that the photospheric temperature exhibits a rapid exponential decline during the first week after the explosion. An analytic model describing the cooling emission after shock breakout provides a reasonable explanation for the observed temperature evolution. From these ejecta parameters, we calculated the progenitor radius to be $R_{pro}=50-340$~$R_{\odot}$. We conclude that these explosion properties are consistent with a core-collapse explosion from a yellow supergiant (YSG) progenitor. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_05054 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | SN 2024iss: Double-Peaked Light Curves and Implications for a Yellow Supergiant Progenitor Yamanaka, Masayuki Nagayama, Takahiro Horikiri, Tsukiha High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We report the multi-band photometric observations of the Type IIb supernova (SN) 2024iss with ultra-violet (UV), optical, and near-infrared (NIR) wavelengths starting one day after the explosion. The UV and optical light curves show the first peak two days after the explosion date. Following a first peak, a secondary maximum is observed in the optical and NIR bands, similar to SNe IIb with double-peaked light curves. The quasi-bolometric light curve shows the fast decay until a week after the explosion. From the analysis of the bolometric light curve, the ejecta mass and kinetic energy are estimated to be $M_{ej}=2.8\pm0.6~M_{\odot}$ and $E_{kin}=9.4\pm4.1\times10^{50}$ erg. The mass of the radioactive $^{56}$Ni is estimated to be $M(^{56}Ni)=0.2~M_{\odot}$. Fitting a black-body function to the spectral energy distribution reveals that the photospheric temperature exhibits a rapid exponential decline during the first week after the explosion. An analytic model describing the cooling emission after shock breakout provides a reasonable explanation for the observed temperature evolution. From these ejecta parameters, we calculated the progenitor radius to be $R_{pro}=50-340$~$R_{\odot}$. We conclude that these explosion properties are consistent with a core-collapse explosion from a yellow supergiant (YSG) progenitor. |
| title | SN 2024iss: Double-Peaked Light Curves and Implications for a Yellow Supergiant Progenitor |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2503.05054 |