SN2017ckj: A linearly declining Type IIb supernova with a relatively massive hydrogen envelope
Fuente:
arXiv
Guardado en:
| Autores principales: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Formato: | Preprint |
| Publicado: |
2025
|
| Materias: | |
| Acceso en línea: | |
| Etiquetas: |
Agregar Etiqueta
Sin Etiquetas, Sea el primero en etiquetar este registro!
|
| _version_ | 1866918287733948416 |
|---|---|
| author | Li, L. -H. Benetti, S. Cai, Y. -Z. Wang, B. Pastorello, A. Elias-Rosa, N. Reguitti, A. Borsato, L. Cappellaro, E. Fiore, A. Fraser, M. Gromadzki, M. Harmanen, J. Isern, J. Kangas, T. Kankare, E. Lundqvist, P. Mattila, S. Ochner, P. Peng, Z. -H. Reynolds, T. M. Salmaso, I. Srivastav, S. Stritzinger, M. D. Tomasella, L. Valerin, G. Wang, Z. -Y. Zhang, J. -J. Wu, C. -Y. |
| author_facet | Li, L. -H. Benetti, S. Cai, Y. -Z. Wang, B. Pastorello, A. Elias-Rosa, N. Reguitti, A. Borsato, L. Cappellaro, E. Fiore, A. Fraser, M. Gromadzki, M. Harmanen, J. Isern, J. Kangas, T. Kankare, E. Lundqvist, P. Mattila, S. Ochner, P. Peng, Z. -H. Reynolds, T. M. Salmaso, I. Srivastav, S. Stritzinger, M. D. Tomasella, L. Valerin, G. Wang, Z. -Y. Zhang, J. -J. Wu, C. -Y. |
| contents | We present optical observations of the Type IIb supernova (SN) 2017ckj, covering approximately 180 days after the explosion. Its early-time multi-band light curves display no clear evidence of a shock-cooling tail, resembling the behavior of SN2008ax. The $V$-band light curve exhibits a short rise time of about 5 days and reaches an absolute fitted peak magnitude of $M_{\rm V}=-18.49\pm0.18\mathrm{mag}$. The late-time multi-band light curves reveal a linear decline. We modelled the bolometric light curve of SN2017ckj to constrain the progenitor and the explosion parameters. We estimated a total mass of $\rm ^{56}Ni$ synthesized by SN2017ckj of $M_{\rm Ni} = 0.21^{+0.05}_{-0.03}\ M_\odot$, with a massive H-rich envelope of $M_{\rm env} = 0.4^{+0.1}_{-0.1}\ M_\odot$. Both the $\rm ^{56}Ni$ mass and the envelope mass of SN2017ckj are higher than those of typical SNe IIb, in agreement with its peculiar light curve evolution. The early-time spectra of SN2017ckj are dominated by a blue continuum, accompanied by narrow $\rm H_α$ and \Heii emission lines. The earliest spectrum exhibits flash ionization features, from which we estimated a progenitor mass-loss rate of $\sim 3\times10^{-4}M_\odot \mathrm{yr}^{-1}$. At later epochs, the spectra develop broad P-Cygni profiles and become increasingly similar to those of SNe IIb, especially SN2018gk. The late-time spectrum at around 139 days does not show a distinct decline in the strength of $\rm H_α$ emission profile, also indicating a relatively massive envelope of its progenitor. Aside from the $\rm H_α$ feature, the nebular spectrum exhibits prominent emission lines of \Oi, \Caii, [\Caii], and \Mgi], which are consistent with the prototypical SN1993J. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_22989 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | SN2017ckj: A linearly declining Type IIb supernova with a relatively massive hydrogen envelope Li, L. -H. Benetti, S. Cai, Y. -Z. Wang, B. Pastorello, A. Elias-Rosa, N. Reguitti, A. Borsato, L. Cappellaro, E. Fiore, A. Fraser, M. Gromadzki, M. Harmanen, J. Isern, J. Kangas, T. Kankare, E. Lundqvist, P. Mattila, S. Ochner, P. Peng, Z. -H. Reynolds, T. M. Salmaso, I. Srivastav, S. Stritzinger, M. D. Tomasella, L. Valerin, G. Wang, Z. -Y. Zhang, J. -J. Wu, C. -Y. Solar and Stellar Astrophysics High Energy Astrophysical Phenomena We present optical observations of the Type IIb supernova (SN) 2017ckj, covering approximately 180 days after the explosion. Its early-time multi-band light curves display no clear evidence of a shock-cooling tail, resembling the behavior of SN2008ax. The $V$-band light curve exhibits a short rise time of about 5 days and reaches an absolute fitted peak magnitude of $M_{\rm V}=-18.49\pm0.18\mathrm{mag}$. The late-time multi-band light curves reveal a linear decline. We modelled the bolometric light curve of SN2017ckj to constrain the progenitor and the explosion parameters. We estimated a total mass of $\rm ^{56}Ni$ synthesized by SN2017ckj of $M_{\rm Ni} = 0.21^{+0.05}_{-0.03}\ M_\odot$, with a massive H-rich envelope of $M_{\rm env} = 0.4^{+0.1}_{-0.1}\ M_\odot$. Both the $\rm ^{56}Ni$ mass and the envelope mass of SN2017ckj are higher than those of typical SNe IIb, in agreement with its peculiar light curve evolution. The early-time spectra of SN2017ckj are dominated by a blue continuum, accompanied by narrow $\rm H_α$ and \Heii emission lines. The earliest spectrum exhibits flash ionization features, from which we estimated a progenitor mass-loss rate of $\sim 3\times10^{-4}M_\odot \mathrm{yr}^{-1}$. At later epochs, the spectra develop broad P-Cygni profiles and become increasingly similar to those of SNe IIb, especially SN2018gk. The late-time spectrum at around 139 days does not show a distinct decline in the strength of $\rm H_α$ emission profile, also indicating a relatively massive envelope of its progenitor. Aside from the $\rm H_α$ feature, the nebular spectrum exhibits prominent emission lines of \Oi, \Caii, [\Caii], and \Mgi], which are consistent with the prototypical SN1993J. |
| title | SN2017ckj: A linearly declining Type IIb supernova with a relatively massive hydrogen envelope |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2510.22989 |