Massive stars exploding in a He-rich circumstellar medium

We present optical and near-infrared observations of two Type Ibn supernovae (SNe), SN 2018jmt and SN 2019cj. Their light curves have rise times of about ten days, reaching an absolute peak magnitude of M g (SN 2018jmt) = −19.07 ± 0.37 and M V (SN 2019cj) = −18.94 ± 0.19 mag, respectively. The early-time spectra of SN 2018jmt are dominated by a blue continuum, accompanied by narrow (600−1000 km s −1 ) He I lines with the P-Cygni profile. At later epochs, the spectra become more similar to those of the prototypical SN Ibn 2006jc. At early phases, the spectra of SN 2019cj show flash ionisation emission lines of C III , N III , and He II superposed on a blue continuum. These features disappear after a few days, and then the spectra of SN 2019cj evolve similarly to those of SN 2018jmt. The spectra indicate that the two SNe exploded within a He-rich circumstellar medium (CSM) lost by the progenitors a short time before the explosion. We modelled the light curves of the two SNe Ibn to constrain the progenitor and the explosion parameters. The ejecta masses are consistent with either what is expected for a canonical SN Ib (∼2 M ⊙ ) or for a massive Wolf Rayet star (> ∼4 M ⊙ ), with the kinetic energy on the order of 10 51 erg. The lower limit on the ejecta mass (> ∼2 M ⊙ ) argues against a scenario involving a relatively low-mass progenitor (e.g. M ZAMS ∼ 10 M ⊙ ). We set a conservative upper limit of ∼0.1 M ⊙ for the 56 Ni masses in both SNe. From the light curve modelling, we determined a two-zone CSM distribution, with an inner, flat CSM component and an outer CSM with a steeper density profile. The physical properties of SN 2018jmt and SN 2019cj are consistent with those expected from the core collapse of relatively massive envelope-stripped stars.

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Journal
Astronomy and Astrophysics
Published
2024-09-14
DOI
https://doi.org/10.1051/0004-6361/202451131
Citations
2
Primary Topic
Gamma-ray bursts and supernovae
Type
article
Field-Weighted Citation Impact
0.66

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article

Massive stars exploding in a He-rich circumstellar medium

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2 citations
Astronomy and Astrophysics
Gamma-ray bursts and supernovae
0.66
article

Massive stars exploding in a He-rich circumstellar medium

Qinan Wang, R. Carini, Weiping Gan, Hsing Wen Lin, Qi Fang, A. Pastorello, L. Galbany, M. Bronikowski, F. Olivares, M. Pursiainen, Difu Shi, N. Elias-Rosa, M. Gromadzki, G. Terreran, G. Valerin, R. Roy, D. Hiramatsu, G. Pignata, Yongzhi Cai, D. R. Young, L. Tartaglia, S. Benetti, J.-J. Zhang, A. Gal-Yam, Maokai Hu, Jonathan Pineda-García, A. Reguitti, E. Cappellaro, Keiichi Maeda, R. Cartier, Bob Warwick, C. Inserra, J. Sollerman, D. A. H. Buckley, Fabio Ragosta, D. A. Howell, A. Gangopadhyay, C. McCully, Amar Aryan, M. Nicholl, Xiaofeng Wang, T. W. Chen, Zhenru Wang, Xuejun Zhu, T. Petrushevska, E. Concepcion, A. Melandri, Mauricio Ramírez, B. Wang, A. Rau, Shaung Wang
article en
2 citations

Abstract

We present optical and near-infrared observations of two Type Ibn supernovae (SNe), SN 2018jmt and SN 2019cj. Their light curves have rise times of about ten days, reaching an absolute peak magnitude of M g (SN 2018jmt) = −19.07 ± 0.37 and M V (SN 2019cj) = −18.94 ± 0.19 mag, respectively. The early-time spectra of SN 2018jmt are dominated by a blue continuum, accompanied by narrow (600−1000 km s −1 ) He I lines with the P-Cygni profile. At later epochs, the spectra become more similar to those of the prototypical SN Ibn 2006jc. At early phases, the spectra of SN 2019cj show flash ionisation emission lines of C III , N III , and He II superposed on a blue continuum. These features disappear after a few days, and then the spectra of SN 2019cj evolve similarly to those of SN 2018jmt. The spectra indicate that the two SNe exploded within a He-rich circumstellar medium (CSM) lost by the progenitors a short time before the explosion. We modelled the light curves of the two SNe Ibn to constrain the progenitor and the explosion parameters. The ejecta masses are consistent with either what is expected for a canonical SN Ib (∼2 M ⊙ ) or for a massive Wolf Rayet star (> ∼4 M ⊙ ), with the kinetic energy on the order of 10 51 erg. The lower limit on the ejecta mass (> ∼2 M ⊙ ) argues against a scenario involving a relatively low-mass progenitor (e.g. M ZAMS ∼ 10 M ⊙ ). We set a conservative upper limit of ∼0.1 M ⊙ for the 56 Ni masses in both SNe. From the light curve modelling, we determined a two-zone CSM distribution, with an inner, flat CSM component and an outer CSM with a steeper density profile. The physical properties of SN 2018jmt and SN 2019cj are consistent with those expected from the core collapse of relatively massive envelope-stripped stars.

Astronomy and AstrophysicsVol. 691
Queen's University Belfast (GB), Las Cumbres Observatory Global Telescope Network (US), Institute of Space Sciences (ES), Universidad Andrés Bello (CL), Johns Hopkins University (US), Guangxi University (CN), University of California, Santa Barbara (US), University of Cape Town (ZA), Stockholm University (SE), Manipal Academy of Higher Education (IN), Anhui University of Science and Technology (CN), University of Tarapacá (CL), University of Nova Gorica (SI), Chinese Academy of Sciences (CN), National Central University (TW), Kyoto University (JP), Beijing Normal University (CN), University of the Free State (ZA), Astronomical Observatory of Rome (IT), Agenzia Spaziale Italiana (IT), Yunnan Observatories (CN), Brera Astronomical Observatory (IT), Purple Mountain Observatory (CN), University of Warwick (GB), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), Millennium Institute of Astrophysics (CL), South African Radio Astronomy Observatory (ZA), East Asian Observatory (US), Université Bourgogne Franche-Comté (FR), Center for Astrophysics Harvard & Smithsonian (US), Collurania Teramo Observatory (IT), AlbaNova (SE), Osservatorio Astronomico di Padova (IT), The NSF AI Institute for Artificial Intelligence and Fundamental Interactions (US), University of Warsaw (PL), Weizmann Institute of Science (IL), Cardiff University (GB), Universidad Diego Portales (CL), Tsinghua University (CN)
National Science Foundation, Smithsonian Institution, National Aeronautics and Space Administration, Alfred P. Sloan Foundation, Gordon and Betty Moore Foundation, Yale University, Carnegie Institution of Washington, Vanderbilt University, Ohio State University, California Institute of Technology, University of Washington, Johns Hopkins University, Carnegie Mellon University, University of Notre Dame, Villum Fonden, University of Portsmouth, New Mexico State University, Tencent, Chinese Academy of Sciences South America Center for Astronomy, York University, University of Oxford, Deutsche Forschungsgemeinschaft, National Natural Science Foundation of China, Chinese Academy of Sciences, Ministério da Ciência, Tecnologia e Inovação, European Southern Observatory, Universidad Nacional Autónoma de México, Max-Planck-Institut für Astrophysik, Max-Planck-Institut für Astronomie, Instituto de Astrofísica de Canarias, University of Colorado Boulder, Center for Cosmology and Astroparticle Physics, Ohio State University, Science Mission Directorate, Science and Technology Facilities Council, Leibniz-Gemeinschaft, Fundamental Research Funds for the Central Universities, Lawrence Berkeley National Laboratory
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Gamma-ray bursts and supernovae
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