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Evidence for an Instability-Induced Binary Merger in the Double-Peaked, Helium-Rich Type IIn Supernova 2023zkd

Fuente: arXiv

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Autori principali:	Gagliano, A., Villar, V. A., Matsumoto, T., Jones, D. O., Ransome, C. L., Nugent, A. E., Hiramatsu, D., Auchettl, K., Tsuna, D., Dong, Y., Gomez, S., Aleo, P. D., Angus, C., de Boer, T., Bostroem, K. A., Chambers, K. C., Coulter, D. A., Davis, K. W., Fairlamb, J. R., Farah, J., Farias, D., Foley, R. J., Gall, C., Gao, H., Gonzalez, E. P., Howell, D. A., Huber, M. E., Kilpatrick, C. D., Lin, C. -C., MacLeod, M. E., Magnier, E. A., McCully, C., Minguez, P., Narayan, G., Newsome, M., Patra, K. C., Rest, A., Rest, S., Smartt, S., Smith, K. W., Terreran, G., Wainscoat, R. J., Wang, Q., Yadavalli, S. K., Zenati, Y.
Natura:	Preprint
Pubblicazione:	2025
Soggetti:	High Energy Astrophysical Phenomena
Accesso online:	Acceder al recurso
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_version_	1866909514096181248
author	Gagliano, A. Villar, V. A. Matsumoto, T. Jones, D. O. Ransome, C. L. Nugent, A. E. Hiramatsu, D. Auchettl, K. Tsuna, D. Dong, Y. Gomez, S. Aleo, P. D. Angus, C. de Boer, T. Bostroem, K. A. Chambers, K. C. Coulter, D. A. Davis, K. W. Fairlamb, J. R. Farah, J. Farias, D. Foley, R. J. Gall, C. Gao, H. Gonzalez, E. P. Howell, D. A. Huber, M. E. Kilpatrick, C. D. Lin, C. -C. MacLeod, M. E. Magnier, E. A. McCully, C. Minguez, P. Narayan, G. Newsome, M. Patra, K. C. Rest, A. Rest, S. Smartt, S. Smith, K. W. Terreran, G. Wainscoat, R. J. Wang, Q. Yadavalli, S. K. Zenati, Y.
author_facet	Gagliano, A. Villar, V. A. Matsumoto, T. Jones, D. O. Ransome, C. L. Nugent, A. E. Hiramatsu, D. Auchettl, K. Tsuna, D. Dong, Y. Gomez, S. Aleo, P. D. Angus, C. de Boer, T. Bostroem, K. A. Chambers, K. C. Coulter, D. A. Davis, K. W. Fairlamb, J. R. Farah, J. Farias, D. Foley, R. J. Gall, C. Gao, H. Gonzalez, E. P. Howell, D. A. Huber, M. E. Kilpatrick, C. D. Lin, C. -C. MacLeod, M. E. Magnier, E. A. McCully, C. Minguez, P. Narayan, G. Newsome, M. Patra, K. C. Rest, A. Rest, S. Smartt, S. Smith, K. W. Terreran, G. Wainscoat, R. J. Wang, Q. Yadavalli, S. K. Zenati, Y.
contents	We present ultraviolet to infrared observations of the extraordinary Type IIn supernova 2023zkd (SN 2023zkd). Photometrically, it exhibits persistent and luminous precursor emission spanning $\sim$4 years preceding discovery ($M_r\approx-15$ mag, 1,500~days in the observer frame), followed by a secondary stage of gradual brightening in its final year. Post-discovery, it exhibits two photometric peaks of comparable brightness ($M_r\lesssim-18.7$ mag and $M_r\approx-18.4$ mag, respectively) separated by 240 days. Spectroscopically, SN 2023zkd exhibits highly asymmetric and multi-component Balmer and He I profiles that we attribute to ejecta interaction with fast-moving ($1,\!000-2,\!000\;\mathrm{km}\;\mathrm{s}^{-1}$) He-rich polar material and slow-moving ($\sim$$400\;\mathrm{km}\;\mathrm{s}^{-1}$) equatorially-distributed H-rich material. He II features also appear during the second light curve peak and evolve rapidly. Shock-driven models fit to the multi-band photometry suggest that the event is powered by interaction with $\sim$$5-6\;M_{\odot}$ of CSM, with $2-3\;M_{\odot}$ associated with each light curve peak, expelled during mass-loss episodes $\sim$$3-4$ and $\sim$$1-2$ years prior to explosion. The observed precursor emission, combined with the extreme mass-loss rates required to power each light curve peak, favors either super-Eddington accretion onto a black hole or multiple long-lived eruptions from a massive star to luminosities that have not been previously observed. We consider multiple progenitor scenarios for SN 2023zkd, and find that the brightening optical precursor and inferred explosion properties are most consistent with a massive ($M_{\mathrm{ZAMS}}\geq30\;M_{\odot}$) and partially-stripped He star undergoing an instability-induced merger with a black hole companion.
format	Preprint
id	arxiv_https___arxiv_org_abs_2502_19469
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	Evidence for an Instability-Induced Binary Merger in the Double-Peaked, Helium-Rich Type IIn Supernova 2023zkd Gagliano, A. Villar, V. A. Matsumoto, T. Jones, D. O. Ransome, C. L. Nugent, A. E. Hiramatsu, D. Auchettl, K. Tsuna, D. Dong, Y. Gomez, S. Aleo, P. D. Angus, C. de Boer, T. Bostroem, K. A. Chambers, K. C. Coulter, D. A. Davis, K. W. Fairlamb, J. R. Farah, J. Farias, D. Foley, R. J. Gall, C. Gao, H. Gonzalez, E. P. Howell, D. A. Huber, M. E. Kilpatrick, C. D. Lin, C. -C. MacLeod, M. E. Magnier, E. A. McCully, C. Minguez, P. Narayan, G. Newsome, M. Patra, K. C. Rest, A. Rest, S. Smartt, S. Smith, K. W. Terreran, G. Wainscoat, R. J. Wang, Q. Yadavalli, S. K. Zenati, Y. High Energy Astrophysical Phenomena We present ultraviolet to infrared observations of the extraordinary Type IIn supernova 2023zkd (SN 2023zkd). Photometrically, it exhibits persistent and luminous precursor emission spanning $\sim$4 years preceding discovery ($M_r\approx-15$ mag, 1,500~days in the observer frame), followed by a secondary stage of gradual brightening in its final year. Post-discovery, it exhibits two photometric peaks of comparable brightness ($M_r\lesssim-18.7$ mag and $M_r\approx-18.4$ mag, respectively) separated by 240 days. Spectroscopically, SN 2023zkd exhibits highly asymmetric and multi-component Balmer and He I profiles that we attribute to ejecta interaction with fast-moving ($1,\!000-2,\!000\;\mathrm{km}\;\mathrm{s}^{-1}$) He-rich polar material and slow-moving ($\sim$$400\;\mathrm{km}\;\mathrm{s}^{-1}$) equatorially-distributed H-rich material. He II features also appear during the second light curve peak and evolve rapidly. Shock-driven models fit to the multi-band photometry suggest that the event is powered by interaction with $\sim$$5-6\;M_{\odot}$ of CSM, with $2-3\;M_{\odot}$ associated with each light curve peak, expelled during mass-loss episodes $\sim$$3-4$ and $\sim$$1-2$ years prior to explosion. The observed precursor emission, combined with the extreme mass-loss rates required to power each light curve peak, favors either super-Eddington accretion onto a black hole or multiple long-lived eruptions from a massive star to luminosities that have not been previously observed. We consider multiple progenitor scenarios for SN 2023zkd, and find that the brightening optical precursor and inferred explosion properties are most consistent with a massive ($M_{\mathrm{ZAMS}}\geq30\;M_{\odot}$) and partially-stripped He star undergoing an instability-induced merger with a black hole companion.
title	Evidence for an Instability-Induced Binary Merger in the Double-Peaked, Helium-Rich Type IIn Supernova 2023zkd
topic	High Energy Astrophysical Phenomena
url	https://arxiv.org/abs/2502.19469