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Massive stars exploding in a He-rich circumstellar medium XII. SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features

Fuente: arXiv

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Hauptverfasser:	Cai, Y. -Z., Pastorello, A., Maeda, K., Zhao, J. -W., Wang, Z. -Y., Peng, Z. -H., Reguitti, A., Tartaglia, L., Filippenko, A. V., Pan, Y., Valerin, G., Kumar, B., Wang, Z., Fraser, M., Anderson, J. P., Benetti, S., Bose, S., Brink, T. G., Cappellaro, E., Chen, T. -W., Chen, X. -L., Elias-Rosa, N., Esamdin, A., Gal-Yam, A., González-Bañuelos, M., Gromadzki, M., Gutiérrez, C. P., Iskandar, A., Inserra, C., Kangas, T., Kankare, E., Kravtsov, T., Kuncarayakti, H., Li, L. -P., Liu, C. -X., Liu, X. -K., Lundqvist, P., Matilainen, K., Mattila, S., Moran, S., Müller-Bravo, T. E., Nagao, T., Petrushevska, T., Pignata, G., Salmaso, I., Smartt, S. J., Sollerman, J., Stritzinger, M. D., Srivastav, S., Wang, L. -T., Yan, S. -Y., Yang, Y., Yang, Y. -P., Zheng, W., Zou, X. -Z., Chen, L. -Y., Du, X. -L., Fang, Q. -L., Fiore, A., Ragosta, F., Zha, S., Zhang, J. -J., Liu, X. -W., Bai, J. -M., Wang, B., Wang, X. -F.
Format:	Preprint
Veröffentlicht:	2025
Schlagworte:	Solar and Stellar Astrophysics High Energy Astrophysical Phenomena
Online-Zugang:	Acceder al recurso
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author	Cai, Y. -Z. Pastorello, A. Maeda, K. Zhao, J. -W. Wang, Z. -Y. Peng, Z. -H. Reguitti, A. Tartaglia, L. Filippenko, A. V. Pan, Y. Valerin, G. Kumar, B. Wang, Z. Fraser, M. Anderson, J. P. Benetti, S. Bose, S. Brink, T. G. Cappellaro, E. Chen, T. -W. Chen, X. -L. Elias-Rosa, N. Esamdin, A. Gal-Yam, A. González-Bañuelos, M. Gromadzki, M. Gutiérrez, C. P. Iskandar, A. Inserra, C. Kangas, T. Kankare, E. Kravtsov, T. Kuncarayakti, H. Li, L. -P. Liu, C. -X. Liu, X. -K. Lundqvist, P. Matilainen, K. Mattila, S. Moran, S. Müller-Bravo, T. E. Nagao, T. Petrushevska, T. Pignata, G. Salmaso, I. Smartt, S. J. Sollerman, J. Stritzinger, M. D. Srivastav, S. Wang, L. -T. Yan, S. -Y. Yang, Y. Yang, Y. -P. Zheng, W. Zou, X. -Z. Chen, L. -Y. Du, X. -L. Fang, Q. -L. Fiore, A. Ragosta, F. Zha, S. Zhang, J. -J. Liu, X. -W. Bai, J. -M. Wang, B. Wang, X. -F.
author_facet	Cai, Y. -Z. Pastorello, A. Maeda, K. Zhao, J. -W. Wang, Z. -Y. Peng, Z. -H. Reguitti, A. Tartaglia, L. Filippenko, A. V. Pan, Y. Valerin, G. Kumar, B. Wang, Z. Fraser, M. Anderson, J. P. Benetti, S. Bose, S. Brink, T. G. Cappellaro, E. Chen, T. -W. Chen, X. -L. Elias-Rosa, N. Esamdin, A. Gal-Yam, A. González-Bañuelos, M. Gromadzki, M. Gutiérrez, C. P. Iskandar, A. Inserra, C. Kangas, T. Kankare, E. Kravtsov, T. Kuncarayakti, H. Li, L. -P. Liu, C. -X. Liu, X. -K. Lundqvist, P. Matilainen, K. Mattila, S. Moran, S. Müller-Bravo, T. E. Nagao, T. Petrushevska, T. Pignata, G. Salmaso, I. Smartt, S. J. Sollerman, J. Stritzinger, M. D. Srivastav, S. Wang, L. -T. Yan, S. -Y. Yang, Y. Yang, Y. -P. Zheng, W. Zou, X. -Z. Chen, L. -Y. Du, X. -L. Fang, Q. -L. Fiore, A. Ragosta, F. Zha, S. Zhang, J. -J. Liu, X. -W. Bai, J. -M. Wang, B. Wang, X. -F.
contents	We present a photometric and spectroscopic analysis of the Type Ibn supernova (SN) 2024acyl. It rises to an absolute magnitude peak of about -17.58 mag in 10.6 days, and displays a rapid linear post-peak light-curve decline in all bands, similar to most SNe Ibn. The optical pseudobolometric light curve peaks at $(3.5\pm0.8) \times 10^{42}$ erg s$^{-1}$, with a total radiated energy of $(5.0\pm0.4) \times 10^{48}$ erg. The spectra are dominated by a blue continuum at early stages, with narrow P Cygni He I lines and flash-ionisation emission lines of C III, N III, and He II. The P Cygni He I features gradually evolve and become emission-dominated in late-time spectra. Our multi-band light-curve modelling yields estimates of the ejecta mass of $M_{\rm ej} = 0.49^{+0.11}_{-0.09}$ M$_\odot$ with a kinetic energy of $E_{\rm k} = 0.06^{+0.01}_{-0.01} \times 10^{51}$ erg, and a $^{56}$Ni mass of $M_{\rm Ni} = 0.018$ M$_\odot$. The inferred CSM properties are characterised by a mass of $M_{\rm CSM} = 0.51^{+0.05}_{-0.04}$ M$_\odot$, an inner radius of $R_0 = 17.8^{+3.6}_{-3.0}$ AU, and a density of $ρ_{\rm CSM} =(8.3_{-1.2}^{+2.7})\times10^{-12}$ g cm$^{-3}$. The multi-epoch spectra are well reproduced by the CMFGEN/he4p0 model, corresponding to a He-ZAMS mass of 4 M$_\odot$ (H-ZAMS mass 18.11 M$_\odot$, pre-SN mass 3.16 M$_\odot$). These findings are consistent with a scenario of an SN powered by ejecta-CSM interaction, originating from a low-mass helium star that evolved within an interacting binary system where the CSM with some residual hydrogen may originate from the mass-transfer process. In addition, a channel of core-collapse explosion of a late-type Wolf-Rayet star with H, or an Ofpe/WN9 star with fallback accretion, cannot be entirely ruled out.
format	Preprint
id	arxiv_https___arxiv_org_abs_2511_04337
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	Massive stars exploding in a He-rich circumstellar medium XII. SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features Cai, Y. -Z. Pastorello, A. Maeda, K. Zhao, J. -W. Wang, Z. -Y. Peng, Z. -H. Reguitti, A. Tartaglia, L. Filippenko, A. V. Pan, Y. Valerin, G. Kumar, B. Wang, Z. Fraser, M. Anderson, J. P. Benetti, S. Bose, S. Brink, T. G. Cappellaro, E. Chen, T. -W. Chen, X. -L. Elias-Rosa, N. Esamdin, A. Gal-Yam, A. González-Bañuelos, M. Gromadzki, M. Gutiérrez, C. P. Iskandar, A. Inserra, C. Kangas, T. Kankare, E. Kravtsov, T. Kuncarayakti, H. Li, L. -P. Liu, C. -X. Liu, X. -K. Lundqvist, P. Matilainen, K. Mattila, S. Moran, S. Müller-Bravo, T. E. Nagao, T. Petrushevska, T. Pignata, G. Salmaso, I. Smartt, S. J. Sollerman, J. Stritzinger, M. D. Srivastav, S. Wang, L. -T. Yan, S. -Y. Yang, Y. Yang, Y. -P. Zheng, W. Zou, X. -Z. Chen, L. -Y. Du, X. -L. Fang, Q. -L. Fiore, A. Ragosta, F. Zha, S. Zhang, J. -J. Liu, X. -W. Bai, J. -M. Wang, B. Wang, X. -F. Solar and Stellar Astrophysics High Energy Astrophysical Phenomena We present a photometric and spectroscopic analysis of the Type Ibn supernova (SN) 2024acyl. It rises to an absolute magnitude peak of about -17.58 mag in 10.6 days, and displays a rapid linear post-peak light-curve decline in all bands, similar to most SNe Ibn. The optical pseudobolometric light curve peaks at $(3.5\pm0.8) \times 10^{42}$ erg s$^{-1}$, with a total radiated energy of $(5.0\pm0.4) \times 10^{48}$ erg. The spectra are dominated by a blue continuum at early stages, with narrow P Cygni He I lines and flash-ionisation emission lines of C III, N III, and He II. The P Cygni He I features gradually evolve and become emission-dominated in late-time spectra. Our multi-band light-curve modelling yields estimates of the ejecta mass of $M_{\rm ej} = 0.49^{+0.11}_{-0.09}$ M$_\odot$ with a kinetic energy of $E_{\rm k} = 0.06^{+0.01}_{-0.01} \times 10^{51}$ erg, and a $^{56}$Ni mass of $M_{\rm Ni} = 0.018$ M$_\odot$. The inferred CSM properties are characterised by a mass of $M_{\rm CSM} = 0.51^{+0.05}_{-0.04}$ M$_\odot$, an inner radius of $R_0 = 17.8^{+3.6}_{-3.0}$ AU, and a density of $ρ_{\rm CSM} =(8.3_{-1.2}^{+2.7})\times10^{-12}$ g cm$^{-3}$. The multi-epoch spectra are well reproduced by the CMFGEN/he4p0 model, corresponding to a He-ZAMS mass of 4 M$_\odot$ (H-ZAMS mass 18.11 M$_\odot$, pre-SN mass 3.16 M$_\odot$). These findings are consistent with a scenario of an SN powered by ejecta-CSM interaction, originating from a low-mass helium star that evolved within an interacting binary system where the CSM with some residual hydrogen may originate from the mass-transfer process. In addition, a channel of core-collapse explosion of a late-type Wolf-Rayet star with H, or an Ofpe/WN9 star with fallback accretion, cannot be entirely ruled out.
title	Massive stars exploding in a He-rich circumstellar medium XII. SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features
topic	Solar and Stellar Astrophysics High Energy Astrophysical Phenomena
url	https://arxiv.org/abs/2511.04337