Evolution of A Peculiar Type Ibn Supernova SN 2019wep
Anjasha Gangopadhyay, Kuntal Misra, Griffin Hosseinzadeh, Iair Arcavi,, Craig Pellegrino, Xiaofeng Wang, D. Andrew Howell, Jamison Burke, Jujia, Zhang, Koji Kawabata, Mridweeka Singh, Raya Dastidar, Daichi Hiramatsu,, Curtis McCully, Jun Mo, Zhihao Chen, Danfeng Xiang

TL;DR
This paper presents detailed photometric and spectroscopic observations of the peculiar Type Ibn supernova SN 2019wep, revealing its unique features and evolutionary behavior compared to other SNe Ibn and fast transients.
Contribution
It provides the first high-cadence monitoring of SN 2019wep, identifying its peculiar properties and classifying it within the 'P cygni' sub-class, with insights into its progenitor characteristics.
Findings
SN 2019wep shows signatures of flash ionization.
Its decline rates are consistent with SNe Ibn but slower than fast transients.
Spectral analysis suggests a progenitor between WR and LBV stars.
Abstract
We present a high-cadence short term photometric and spectroscopic monitoring campaign of a type Ibn SN 2019wep, which is one of the rare SN Ibn after SNe 2010al and 2019uo to display signatures of flash ionization (\ion{He}{2}, \ion{C}{3}, \ion{N}{3}). We compare the decline rates and rise time of SN 2019wep with other SNe Ibn and fast transients. The post-peak decline in all bands (0.1 mag d) are consistent with SNe Ibn but less than the fast transients. On the other hand, the m values are slightly lower than the average values for SNe Ibn but consistent with the fast transients. The rise time is typically shorter than SNe Ibn but longer than fast transients. SN 2019wep lies at the fainter end of SNe Ibn but possesses an average luminosity amongst the fast transients sample. The peculiar color evolution places it between SNe Ib and the most extreme SNe Ibn. The…
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