SN 2023vbg: A Type IIn Supernova Resembling SN 2009ip, with a Long-Duration Precursor and Early-Time Bump
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| Format: | Preprint |
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2025
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| author | Goto, Sota Yamanaka, Masayuki Nagayama, Takahiro Maeda, Keiichi Kawabata, Miho Sahu, D. K. Singh, Avinash Gangopadhyay, Anjasha Dkuniya, Naveen Misra, Kuntal Dubey, Monalisa Ailawadhi, Bhavya |
| author_facet | Goto, Sota Yamanaka, Masayuki Nagayama, Takahiro Maeda, Keiichi Kawabata, Miho Sahu, D. K. Singh, Avinash Gangopadhyay, Anjasha Dkuniya, Naveen Misra, Kuntal Dubey, Monalisa Ailawadhi, Bhavya |
| contents | Type IIn supernovae (SNe) resembling SN 2009ip (09ip-like SNe) originate from the interaction between circumstellar material (CSM) and the ejecta. This subclass not only shares similar observational properties around the maximum, but is commonly characterized by a long-duration precursor before its maximum. Investigating the observed properties of the precursor provides constraints on the mass-loss history of the progenitor. We present observational data of SN 2023vbg, a 09ip-like type IIn SN that displayed unique observational properties compared to other 09ip-like SNe. SN 2023vbg showed a long-duration precursor at approximately Mg = -14 mag lasting for about 100 days, followed by a bright bump at Mg = -17 mag at 12-25 days before the maximum. The luminosity of the precursor is similar to those of other 09ip-like SNe, but the bright bump has not been observed in other cases. After reaching the peak luminosity, the light curve exhibited a relatively smooth decline. While the H-alpha profile displays two velocity components (approximately 500 and 3000 km/s), a broad component observed in other 09ip-like SNe was not seen, though it may emerge later. We suggest that these properties are explained by the difference in the CSM structure as compared to other 09ip-like SNe; SN 2023vbg had an inner denser CSM component, as well as generally smooth CSM density distribution on a more extended scale, than in the others. Such diversity of CSM likely reflects the diversity of pre-SN outbursts, which in turn may mirror the range of evolutionary pathways in the final stages of the progenitors. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2504_15988 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | SN 2023vbg: A Type IIn Supernova Resembling SN 2009ip, with a Long-Duration Precursor and Early-Time Bump Goto, Sota Yamanaka, Masayuki Nagayama, Takahiro Maeda, Keiichi Kawabata, Miho Sahu, D. K. Singh, Avinash Gangopadhyay, Anjasha Dkuniya, Naveen Misra, Kuntal Dubey, Monalisa Ailawadhi, Bhavya High Energy Astrophysical Phenomena Solar and Stellar Astrophysics Type IIn supernovae (SNe) resembling SN 2009ip (09ip-like SNe) originate from the interaction between circumstellar material (CSM) and the ejecta. This subclass not only shares similar observational properties around the maximum, but is commonly characterized by a long-duration precursor before its maximum. Investigating the observed properties of the precursor provides constraints on the mass-loss history of the progenitor. We present observational data of SN 2023vbg, a 09ip-like type IIn SN that displayed unique observational properties compared to other 09ip-like SNe. SN 2023vbg showed a long-duration precursor at approximately Mg = -14 mag lasting for about 100 days, followed by a bright bump at Mg = -17 mag at 12-25 days before the maximum. The luminosity of the precursor is similar to those of other 09ip-like SNe, but the bright bump has not been observed in other cases. After reaching the peak luminosity, the light curve exhibited a relatively smooth decline. While the H-alpha profile displays two velocity components (approximately 500 and 3000 km/s), a broad component observed in other 09ip-like SNe was not seen, though it may emerge later. We suggest that these properties are explained by the difference in the CSM structure as compared to other 09ip-like SNe; SN 2023vbg had an inner denser CSM component, as well as generally smooth CSM density distribution on a more extended scale, than in the others. Such diversity of CSM likely reflects the diversity of pre-SN outbursts, which in turn may mirror the range of evolutionary pathways in the final stages of the progenitors. |
| title | SN 2023vbg: A Type IIn Supernova Resembling SN 2009ip, with a Long-Duration Precursor and Early-Time Bump |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2504.15988 |