SN 2021foa: the bridge between SN IIn and Ibn
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arXiv
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| Format: | Preprint |
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2024
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| author | Gangopadhyay, Anjasha Dukiya, Naveen Moriya, Takashi J Tanaka, Masaomi Maeda, Keiichi Howell, D. Andrew Singh, Mridweeka Singh, Avinash Sollerman, Jesper Kawabata, Koji S Brennan, Sean J Pellegrino, Craig Dastidar, Raya Nakaoka, Tatsuya Kawabata, Miho Misra, Kuntal Schulze, Steve Chandra, Poonam Taguchi, Kenta Sahu, Devendra K McCully, Curtis Bostroem, K. Azalee Gonzalez, Estefania Padilla Newsome, Megan Hiramatsu, Daichi Takei, Yuki Yamanaka, Masayuki Tajitsu, Akito Isogai, Keisuke |
| author_facet | Gangopadhyay, Anjasha Dukiya, Naveen Moriya, Takashi J Tanaka, Masaomi Maeda, Keiichi Howell, D. Andrew Singh, Mridweeka Singh, Avinash Sollerman, Jesper Kawabata, Koji S Brennan, Sean J Pellegrino, Craig Dastidar, Raya Nakaoka, Tatsuya Kawabata, Miho Misra, Kuntal Schulze, Steve Chandra, Poonam Taguchi, Kenta Sahu, Devendra K McCully, Curtis Bostroem, K. Azalee Gonzalez, Estefania Padilla Newsome, Megan Hiramatsu, Daichi Takei, Yuki Yamanaka, Masayuki Tajitsu, Akito Isogai, Keisuke |
| contents | We present the long-term photometric and spectroscopic analysis of a transitioning SN~IIn/Ibn from $-$10.8 d to 150.7 d post $V$-band maximum. SN~2021foa shows prominent He {\sc i} lines comparable in strength to the H$α$ line around peak, placing SN~2021foa between the SN~IIn and SN~Ibn populations. The spectral comparison shows that it resembles the SN~IIn population at pre-maximum, becomes intermediate between SNe~IIn/Ibn and at post-maximum matches with SN~IIn 1996al. The photometric evolution shows a precursor at $-$50 d and a light curve shoulder around 17d. The peak luminosity and color evolution of SN 2021foa are consistent with most SNe~IIn and Ibn in our comparison sample. SN~2021foa shows the unique case of a SN~IIn where the narrow P-Cygni in H$α$ becomes prominent at 7.2 days. The H$α$ profile consists of a narrow (500 -- 1200 km s$^{-1}$) component, intermediate width (3000 -- 8000 km s$^{-1}$) and broad component in absorption. Temporal evolution of the H$α$ profile favours a disk-like CSM geometry. Hydrodynamical modelling of the lightcurve well reproduces a two-component CSM structure with different densities ($ρ$ $\propto$ r$^{-2}$ -- $ρ$ $\propto$ r$^{-5}$), mass-loss rates (10$^{-3}$ -- 10$^{-1}$ M$_{\odot}$ yr$^{-1}$) assuming a wind velocity of 1000 km s$^{-1}$ and having a CSM mass of 0.18 M$_{\odot}$. The overall evolution indicates that SN~2021foa most likely originated from a LBV star transitioning to a WR star with the mass-loss rate increasing in the period from 5 to 0.5 years before the explosion or it could be due to a binary interaction. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_02666 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | SN 2021foa: the bridge between SN IIn and Ibn Gangopadhyay, Anjasha Dukiya, Naveen Moriya, Takashi J Tanaka, Masaomi Maeda, Keiichi Howell, D. Andrew Singh, Mridweeka Singh, Avinash Sollerman, Jesper Kawabata, Koji S Brennan, Sean J Pellegrino, Craig Dastidar, Raya Nakaoka, Tatsuya Kawabata, Miho Misra, Kuntal Schulze, Steve Chandra, Poonam Taguchi, Kenta Sahu, Devendra K McCully, Curtis Bostroem, K. Azalee Gonzalez, Estefania Padilla Newsome, Megan Hiramatsu, Daichi Takei, Yuki Yamanaka, Masayuki Tajitsu, Akito Isogai, Keisuke High Energy Astrophysical Phenomena We present the long-term photometric and spectroscopic analysis of a transitioning SN~IIn/Ibn from $-$10.8 d to 150.7 d post $V$-band maximum. SN~2021foa shows prominent He {\sc i} lines comparable in strength to the H$α$ line around peak, placing SN~2021foa between the SN~IIn and SN~Ibn populations. The spectral comparison shows that it resembles the SN~IIn population at pre-maximum, becomes intermediate between SNe~IIn/Ibn and at post-maximum matches with SN~IIn 1996al. The photometric evolution shows a precursor at $-$50 d and a light curve shoulder around 17d. The peak luminosity and color evolution of SN 2021foa are consistent with most SNe~IIn and Ibn in our comparison sample. SN~2021foa shows the unique case of a SN~IIn where the narrow P-Cygni in H$α$ becomes prominent at 7.2 days. The H$α$ profile consists of a narrow (500 -- 1200 km s$^{-1}$) component, intermediate width (3000 -- 8000 km s$^{-1}$) and broad component in absorption. Temporal evolution of the H$α$ profile favours a disk-like CSM geometry. Hydrodynamical modelling of the lightcurve well reproduces a two-component CSM structure with different densities ($ρ$ $\propto$ r$^{-2}$ -- $ρ$ $\propto$ r$^{-5}$), mass-loss rates (10$^{-3}$ -- 10$^{-1}$ M$_{\odot}$ yr$^{-1}$) assuming a wind velocity of 1000 km s$^{-1}$ and having a CSM mass of 0.18 M$_{\odot}$. The overall evolution indicates that SN~2021foa most likely originated from a LBV star transitioning to a WR star with the mass-loss rate increasing in the period from 5 to 0.5 years before the explosion or it could be due to a binary interaction. |
| title | SN 2021foa: the bridge between SN IIn and Ibn |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2409.02666 |