The X-ray Luminous Type Ibn SN 2022ablq: Estimates of Pre-explosion Mass Loss and Constraints on Precursor Emission
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| Main Authors: | , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| author | Pellegrino, C. Modjaz, M. Takei, Y. Tsuna, D. Newsome, M. Pritchard, T. Baer-Way, R. Bostroem, K. A. Chandra, P. Charalampopoulos, P. Dong, Y. Farah, J. Howell, D. A. McCully, C. Mohamed, S. Gonzalez, E. Padilla Terreran, G. |
| author_facet | Pellegrino, C. Modjaz, M. Takei, Y. Tsuna, D. Newsome, M. Pritchard, T. Baer-Way, R. Bostroem, K. A. Chandra, P. Charalampopoulos, P. Dong, Y. Farah, J. Howell, D. A. McCully, C. Mohamed, S. Gonzalez, E. Padilla Terreran, G. |
| contents | Type Ibn supernovae (SNe Ibn) are rare stellar explosions powered primarily by interaction between the SN ejecta and H-poor, He-rich material lost by their progenitor stars. Multi-wavelength observations, particularly in the X-rays, of SNe Ibn constrain their poorly-understood progenitor channels and mass-loss mechanisms. Here we present Swift X-ray, ultraviolet, and ground-based optical observations of the Type Ibn SN 2022ablq -- only the second SN Ibn with X-ray detections to date. While similar to the prototypical Type Ibn SN 2006jc in the optical, SN 2022ablq is roughly an order of magnitude more luminous in the X-rays, reaching unabsorbed luminosities $L_X$ $\sim$ 3$\times$10$^{40}$ erg s$^{-1}$ between 0.2 - 10 keV. From these X-ray observations we infer time-varying mass-loss rates between 0.05 - 0.5 $M_\odot$ yr$^{-1}$ peaking 0.5 - 2 yr before explosion. This complex mass-loss history and circumstellar environment disfavor steady-state winds as the primary progenitor mass-loss mechanism. We also search for precursor emission from alternative mass-loss mechanisms, such as eruptive outbursts, in forced photometry during the two years before explosion. We find no statistically significant detections brighter than M $\approx$ -14 -- too shallow to rule out precursor events similar to those observed for other SNe Ibn. Finally, numerical models of the explosion of a $\sim$15 $M_\odot$ helium star that undergoes an eruptive outburst $\approx$1.8 years before explosion are consistent with the observed bolometric light curve. We conclude that our observations disfavor a Wolf-Rayet star progenitor losing He-rich material via stellar winds and instead favor lower-mass progenitor models, including Roche-lobe overflow in helium stars with compact binary companions or stars that undergo eruptive outbursts during late-stage nucleosynthesis stages. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_18291 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The X-ray Luminous Type Ibn SN 2022ablq: Estimates of Pre-explosion Mass Loss and Constraints on Precursor Emission Pellegrino, C. Modjaz, M. Takei, Y. Tsuna, D. Newsome, M. Pritchard, T. Baer-Way, R. Bostroem, K. A. Chandra, P. Charalampopoulos, P. Dong, Y. Farah, J. Howell, D. A. McCully, C. Mohamed, S. Gonzalez, E. Padilla Terreran, G. High Energy Astrophysical Phenomena Type Ibn supernovae (SNe Ibn) are rare stellar explosions powered primarily by interaction between the SN ejecta and H-poor, He-rich material lost by their progenitor stars. Multi-wavelength observations, particularly in the X-rays, of SNe Ibn constrain their poorly-understood progenitor channels and mass-loss mechanisms. Here we present Swift X-ray, ultraviolet, and ground-based optical observations of the Type Ibn SN 2022ablq -- only the second SN Ibn with X-ray detections to date. While similar to the prototypical Type Ibn SN 2006jc in the optical, SN 2022ablq is roughly an order of magnitude more luminous in the X-rays, reaching unabsorbed luminosities $L_X$ $\sim$ 3$\times$10$^{40}$ erg s$^{-1}$ between 0.2 - 10 keV. From these X-ray observations we infer time-varying mass-loss rates between 0.05 - 0.5 $M_\odot$ yr$^{-1}$ peaking 0.5 - 2 yr before explosion. This complex mass-loss history and circumstellar environment disfavor steady-state winds as the primary progenitor mass-loss mechanism. We also search for precursor emission from alternative mass-loss mechanisms, such as eruptive outbursts, in forced photometry during the two years before explosion. We find no statistically significant detections brighter than M $\approx$ -14 -- too shallow to rule out precursor events similar to those observed for other SNe Ibn. Finally, numerical models of the explosion of a $\sim$15 $M_\odot$ helium star that undergoes an eruptive outburst $\approx$1.8 years before explosion are consistent with the observed bolometric light curve. We conclude that our observations disfavor a Wolf-Rayet star progenitor losing He-rich material via stellar winds and instead favor lower-mass progenitor models, including Roche-lobe overflow in helium stars with compact binary companions or stars that undergo eruptive outbursts during late-stage nucleosynthesis stages. |
| title | The X-ray Luminous Type Ibn SN 2022ablq: Estimates of Pre-explosion Mass Loss and Constraints on Precursor Emission |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2407.18291 |