The first radio view of a type Ibn supernova in SN 2023fyq: Understanding the mass-loss history in the last decade before the explosion. Baer-Way, R., Nayana, A. J., Jacobson-Galan, W., Chandra, P., Modjaz, M., Wu, S. C., Tsuna, D., Margutti, R., Chornock, R., Pellegrino, C., Dong, Y., Drout, M. R., Kilpatrick, C. D., Milisavljevic, D., Patnaude, D., & Stauffer, C. September, 2025. arXiv:2509.07080 [astro-ph]
The first radio view of a type Ibn supernova in SN 2023fyq: Understanding the mass-loss history in the last decade before the explosion [link]Paper  doi  abstract   bibtex   
Supernovae that interact with hydrogen-poor, helium-rich circumstellar material (CSM), known as Type Ibn supernovae (SNe Ibn), present a unique opportunity to probe mass-loss processes in massive stars. In this work, we report the first radio detection of a SN Ibn, SN 2023fyq, and characterize the mass-loss history of its stellar progenitor using the radio and X-ray observations obtained over 18 months post-explosion. We find that the radio emission from 58–185 days is best modeled by synchrotron radiation attenuated by free-free absorption from a CSM of density ∼ 10−18 g/cm3 (∼ 106ρISM) at a radius of 1016 cm, corresponding to a mass-loss rate of ∼ 4 × 10−3 M⊙ yr−1 (for a wind velocity of 1700 km/s from optical spectroscopy) from 0.7 to 3 years before the explosion. This timescale is consistent with the time frame over which pre-explosion optical outbursts were observed. However, our late-time observations at 525 days post-explosion yield non-detections, and the 3σ upper limits (along with an X-ray non-detection) allow us to infer lower-density CSM at 2 × 1016 cm with ˙M \textless 2.5 × 10−3 M⊙ yr−1. These results suggest a shell-like CSM from at most 4 × 1015 to 2 × 1016 cm (∼ 105R⊙) with an elevated CSM density (0.004 M⊙ yr−1) that is roughly consistent with predictions from a merger model for this object. Future radio observations of a larger sample of SNe Ibn will provide key details on the extent and density of their helium-rich CSM.
@misc{baer-way_first_2025,
	title = {The first radio view of a type {Ibn} supernova in {SN} 2023fyq: {Understanding} the mass-loss history in the last decade before the explosion},
	shorttitle = {The first radio view of a type {Ibn} supernova in {SN} 2023fyq},
	url = {http://arxiv.org/abs/2509.07080},
	doi = {10.48550/arXiv.2509.07080},
	abstract = {Supernovae that interact with hydrogen-poor, helium-rich circumstellar material (CSM), known as Type Ibn supernovae (SNe Ibn), present a unique opportunity to probe mass-loss processes in massive stars. In this work, we report the first radio detection of a SN Ibn, SN 2023fyq, and characterize the mass-loss history of its stellar progenitor using the radio and X-ray observations obtained over 18 months post-explosion. We find that the radio emission from 58–185 days is best modeled by synchrotron radiation attenuated by free-free absorption from a CSM of density ∼ 10−18 g/cm3 (∼ 106ρISM) at a radius of 1016 cm, corresponding to a mass-loss rate of ∼ 4 × 10−3 M⊙ yr−1 (for a wind velocity of 1700 km/s from optical spectroscopy) from 0.7 to 3 years before the explosion. This timescale is consistent with the time frame over which pre-explosion optical outbursts were observed. However, our late-time observations at 525 days post-explosion yield non-detections, and the 3σ upper limits (along with an X-ray non-detection) allow us to infer lower-density CSM at 2 × 1016 cm with ˙M {\textless} 2.5 × 10−3 M⊙ yr−1. These results suggest a shell-like CSM from at most 4 × 1015 to 2 × 1016 cm (∼ 105R⊙) with an elevated CSM density (0.004 M⊙ yr−1) that is roughly consistent with predictions from a merger model for this object. Future radio observations of a larger sample of SNe Ibn will provide key details on the extent and density of their helium-rich CSM.},
	language = {en},
	urldate = {2025-09-18},
	publisher = {arXiv},
	author = {Baer-Way, Raphael and Nayana, A. J. and Jacobson-Galan, Wynn and Chandra, Poonam and Modjaz, Maryam and Wu, Samantha C. and Tsuna, Daichi and Margutti, Raffaella and Chornock, Ryan and Pellegrino, Craig and Dong, Yize and Drout, Maria R. and Kilpatrick, Charles D. and Milisavljevic, Dan and Patnaude, Daniel and Stauffer, Candice},
	month = sep,
	year = {2025},
	note = {arXiv:2509.07080 [astro-ph]},
	keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics},
}
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