Asymmetries and Circumstellar Interaction in the Type II SN 2024bch
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arXiv
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2024
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| author | Andrews, Jennifer E. Shrestha, Manisha Bostroem, K. Azalee Dong, Yize Pearson, Jeniveve Fausnaugh, M. M. Sand, David J. Valenti, S. Ravi, Aravind P. Hoang, Emily Hosseinzadeh, Griffin Ilyin, Ilya Janzen, Daryl Lundquist, M. J. Meza, Nicolaz Smith, Nathan Jha, Saurabh W. Andrews, Moira Farah, Joseph Gonzalez, Estefania Padilla Howell, D. Andrew McCully, Curtis Newsome, Megan Pellegrino, Craig Terreran, Giacomo Wiggins, Patrick Hsu, Brian Christy, Collin T. Franz, Noah Wang, Xiofeng Liu, Jialian Chen, Liyang |
| author_facet | Andrews, Jennifer E. Shrestha, Manisha Bostroem, K. Azalee Dong, Yize Pearson, Jeniveve Fausnaugh, M. M. Sand, David J. Valenti, S. Ravi, Aravind P. Hoang, Emily Hosseinzadeh, Griffin Ilyin, Ilya Janzen, Daryl Lundquist, M. J. Meza, Nicolaz Smith, Nathan Jha, Saurabh W. Andrews, Moira Farah, Joseph Gonzalez, Estefania Padilla Howell, D. Andrew McCully, Curtis Newsome, Megan Pellegrino, Craig Terreran, Giacomo Wiggins, Patrick Hsu, Brian Christy, Collin T. Franz, Noah Wang, Xiofeng Liu, Jialian Chen, Liyang |
| contents | We present a comprehensive multi-epoch photometric and spectroscopic study of SN 2024bch, a nearby (19.9 Mpc) Type II supernova (SN) with prominent early high ionization emission lines. Optical spectra from 2.9 days after the estimated explosion reveal narrow lines of H I, He II, C IV, and N IV that disappear by day 6. High cadence photometry from the ground and TESS show that the SN brightened quickly and reached a peak M$_V \sim$ $-$17.8 mag within a week of explosion, and late-time photometry suggests a $^{56}$Ni mass of 0.050 M$_{\odot}$. High-resolution spectra from day 8 and 43 trace the unshocked circumstellar medium (CSM) and indicate a wind velocity of 30--40 km s$^{-1}$, a value consistent with a red supergiant (RSG) progenitor. Comparisons between models and the early spectra suggest a pre-SN mass-loss rate of $\dot{M} \sim 10^{-3}-10^{-2}\ M_\odot\ \mathrm{yr}^{-1}$, which is too high to be explained by quiescent mass loss from RSGs, but is consistent with some recent measurements of similar SNe. Persistent blueshifted H I and [O I] emission lines seen in the optical and NIR spectra could be produced by asymmetries in the SN ejecta, while the multi-component H$α$ may indicate continued interaction with an asymmetric CSM well into the nebular phase. SN 2024bch provides another clue to the complex environments and mass-loss histories around massive stars. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2411_02497 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Asymmetries and Circumstellar Interaction in the Type II SN 2024bch Andrews, Jennifer E. Shrestha, Manisha Bostroem, K. Azalee Dong, Yize Pearson, Jeniveve Fausnaugh, M. M. Sand, David J. Valenti, S. Ravi, Aravind P. Hoang, Emily Hosseinzadeh, Griffin Ilyin, Ilya Janzen, Daryl Lundquist, M. J. Meza, Nicolaz Smith, Nathan Jha, Saurabh W. Andrews, Moira Farah, Joseph Gonzalez, Estefania Padilla Howell, D. Andrew McCully, Curtis Newsome, Megan Pellegrino, Craig Terreran, Giacomo Wiggins, Patrick Hsu, Brian Christy, Collin T. Franz, Noah Wang, Xiofeng Liu, Jialian Chen, Liyang High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We present a comprehensive multi-epoch photometric and spectroscopic study of SN 2024bch, a nearby (19.9 Mpc) Type II supernova (SN) with prominent early high ionization emission lines. Optical spectra from 2.9 days after the estimated explosion reveal narrow lines of H I, He II, C IV, and N IV that disappear by day 6. High cadence photometry from the ground and TESS show that the SN brightened quickly and reached a peak M$_V \sim$ $-$17.8 mag within a week of explosion, and late-time photometry suggests a $^{56}$Ni mass of 0.050 M$_{\odot}$. High-resolution spectra from day 8 and 43 trace the unshocked circumstellar medium (CSM) and indicate a wind velocity of 30--40 km s$^{-1}$, a value consistent with a red supergiant (RSG) progenitor. Comparisons between models and the early spectra suggest a pre-SN mass-loss rate of $\dot{M} \sim 10^{-3}-10^{-2}\ M_\odot\ \mathrm{yr}^{-1}$, which is too high to be explained by quiescent mass loss from RSGs, but is consistent with some recent measurements of similar SNe. Persistent blueshifted H I and [O I] emission lines seen in the optical and NIR spectra could be produced by asymmetries in the SN ejecta, while the multi-component H$α$ may indicate continued interaction with an asymmetric CSM well into the nebular phase. SN 2024bch provides another clue to the complex environments and mass-loss histories around massive stars. |
| title | Asymmetries and Circumstellar Interaction in the Type II SN 2024bch |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2411.02497 |