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Massive stars exploding in a He-rich circumstellar medium $-$ X. Flash spectral features in the Type Ibn SN 2019cj and observations of SN 2018jmt

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Main Authors:	Wang, Z. -Y., Pastorello, A., Maeda, K., Reguitti, A., Cai, Y. -Z., Howell, D. Andrew, Benetti, S., Buckley, D., Cappellaro, E., Carini, R., Cartier, R., Chen, T. -W., Elias-Rosa, N., Fang, Q. -L., Gal-Yam, A., Gangopadhyay, A., Gromadzki, M., Gan, W. -P., Hiramatsu, D., Hu, M. -K., Inserra, C., McCully, C., Nicholl, M., Olivares, F. E., Pignata, G., Pineda-Garc'ia, J., Pursiainen, M., Ragosta, F., Rau, A., Roy, R., Sollerman, J., Tartaglia, L., Terreran, G., Valerin, G., Wang, Q., Wang, S. -Q., Young, D. R., Aryan, A., Bronikowski, M., Concepcion, E., Galbany, L., Lin, H., Melandri, A., Petrushevska, T., Ramirez, M., Shi, D. -D, Warwick, B., Zhang, J. -J., Wang, B., Wang, X. -F., Zhu, X. -J.
Format:	Preprint
Published:	2024
Subjects:	High Energy Astrophysical Phenomena Solar and Stellar Astrophysics
Online Access:	Acceder al recurso
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author	Wang, Z. -Y. Pastorello, A. Maeda, K. Reguitti, A. Cai, Y. -Z. Howell, D. Andrew Benetti, S. Buckley, D. Cappellaro, E. Carini, R. Cartier, R. Chen, T. -W. Elias-Rosa, N. Fang, Q. -L. Gal-Yam, A. Gangopadhyay, A. Gromadzki, M. Gan, W. -P. Hiramatsu, D. Hu, M. -K. Inserra, C. McCully, C. Nicholl, M. Olivares, F. E. Pignata, G. Pineda-Garc'ia, J. Pursiainen, M. Ragosta, F. Rau, A. Roy, R. Sollerman, J. Tartaglia, L. Terreran, G. Valerin, G. Wang, Q. Wang, S. -Q. Young, D. R. Aryan, A. Bronikowski, M. Concepcion, E. Galbany, L. Lin, H. Melandri, A. Petrushevska, T. Ramirez, M. Shi, D. -D Warwick, B. Zhang, J. -J. Wang, B. Wang, X. -F. Zhu, X. -J.
author_facet	Wang, Z. -Y. Pastorello, A. Maeda, K. Reguitti, A. Cai, Y. -Z. Howell, D. Andrew Benetti, S. Buckley, D. Cappellaro, E. Carini, R. Cartier, R. Chen, T. -W. Elias-Rosa, N. Fang, Q. -L. Gal-Yam, A. Gangopadhyay, A. Gromadzki, M. Gan, W. -P. Hiramatsu, D. Hu, M. -K. Inserra, C. McCully, C. Nicholl, M. Olivares, F. E. Pignata, G. Pineda-Garc'ia, J. Pursiainen, M. Ragosta, F. Rau, A. Roy, R. Sollerman, J. Tartaglia, L. Terreran, G. Valerin, G. Wang, Q. Wang, S. -Q. Young, D. R. Aryan, A. Bronikowski, M. Concepcion, E. Galbany, L. Lin, H. Melandri, A. Petrushevska, T. Ramirez, M. Shi, D. -D Warwick, B. Zhang, J. -J. Wang, B. Wang, X. -F. Zhu, X. -J.
contents	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 10 days, reaching an absolute peak magnitude of $M_g$(SN 2018jmt) = $-$19.07 $\pm$ 0.37 and $M_V$(SN 2019cj) = $-$18.94 $\pm$ 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}$) He I lines with P-Cygni profile. At later epochs, the spectra become more similar to those of the prototypical SN Ibn 2006jc. At early phases, the spectra of SN 2019cj show flash ionisation emission lines of C III, N III and He II superposed on a blue continuum. These features disappear after a few days, and then the spectra of SN 2019cj evolve similarly to those of SN 2018jmt. The spectra indicate that the two SNe exploded within a He-rich circumstellar medium (CSM) lost by the progenitors a short time before the explosion. We model the light curves of the two SNe Ibn to constrain the progenitor and the explosion parameters. The ejecta masses are consistent with either that expected for a canonical SN Ib ($\sim$ 2 M$_{\odot}$) or those from a massive WR star ($>$ $\sim$ 4 M$_{\odot}$), with the kinetic energy on the order of $10^{51}$ erg. The lower limit on the ejecta mass ($>$ $\sim$ 2 M$_{\odot}$) argues against a scenario involving a relatively low-mass progenitor (e.g., $M_{ZAMS}$ $\sim$ 10 M$_{\odot}$). We set a conservative upper limit of $\sim$0.1 M$_{\odot}$ for the $^{56}$Ni masses in both SNe. From the light curve modelling, we determine 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, stripped-envelope (SE) stars.
format	Preprint
id	arxiv_https___arxiv_org_abs_2408_12393
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	Massive stars exploding in a He-rich circumstellar medium $-$ X. Flash spectral features in the Type Ibn SN 2019cj and observations of SN 2018jmt Wang, Z. -Y. Pastorello, A. Maeda, K. Reguitti, A. Cai, Y. -Z. Howell, D. Andrew Benetti, S. Buckley, D. Cappellaro, E. Carini, R. Cartier, R. Chen, T. -W. Elias-Rosa, N. Fang, Q. -L. Gal-Yam, A. Gangopadhyay, A. Gromadzki, M. Gan, W. -P. Hiramatsu, D. Hu, M. -K. Inserra, C. McCully, C. Nicholl, M. Olivares, F. E. Pignata, G. Pineda-Garc'ia, J. Pursiainen, M. Ragosta, F. Rau, A. Roy, R. Sollerman, J. Tartaglia, L. Terreran, G. Valerin, G. Wang, Q. Wang, S. -Q. Young, D. R. Aryan, A. Bronikowski, M. Concepcion, E. Galbany, L. Lin, H. Melandri, A. Petrushevska, T. Ramirez, M. Shi, D. -D Warwick, B. Zhang, J. -J. Wang, B. Wang, X. -F. Zhu, X. -J. High Energy Astrophysical Phenomena Solar and Stellar Astrophysics 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 10 days, reaching an absolute peak magnitude of $M_g$(SN 2018jmt) = $-$19.07 $\pm$ 0.37 and $M_V$(SN 2019cj) = $-$18.94 $\pm$ 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}$) He I lines with P-Cygni profile. At later epochs, the spectra become more similar to those of the prototypical SN Ibn 2006jc. At early phases, the spectra of SN 2019cj show flash ionisation emission lines of C III, N III and He II superposed on a blue continuum. These features disappear after a few days, and then the spectra of SN 2019cj evolve similarly to those of SN 2018jmt. The spectra indicate that the two SNe exploded within a He-rich circumstellar medium (CSM) lost by the progenitors a short time before the explosion. We model the light curves of the two SNe Ibn to constrain the progenitor and the explosion parameters. The ejecta masses are consistent with either that expected for a canonical SN Ib ($\sim$ 2 M$_{\odot}$) or those from a massive WR star ($>$ $\sim$ 4 M$_{\odot}$), with the kinetic energy on the order of $10^{51}$ erg. The lower limit on the ejecta mass ($>$ $\sim$ 2 M$_{\odot}$) argues against a scenario involving a relatively low-mass progenitor (e.g., $M_{ZAMS}$ $\sim$ 10 M$_{\odot}$). We set a conservative upper limit of $\sim$0.1 M$_{\odot}$ for the $^{56}$Ni masses in both SNe. From the light curve modelling, we determine 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, stripped-envelope (SE) stars.
title	Massive stars exploding in a He-rich circumstellar medium $-$ X. Flash spectral features in the Type Ibn SN 2019cj and observations of SN 2018jmt
topic	High Energy Astrophysical Phenomena Solar and Stellar Astrophysics
url	https://arxiv.org/abs/2408.12393