Evolution of A Peculiar Type Ibn Supernova SN 2019wep

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$^{-1}$) are consistent with SNe Ibn but less than the fast transients. On the other hand, the $\Delta$m$_{15}$ 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 bolometric light curve modelling shows resemblance with SN 2019uo with ejecta masses consistent with SNe Ib. SN 2019wep belongs to the "P cygni" sub-class of SNe Ibn and shows faster evolution in line velocities as compared to the "emission" sub-class. The post-maximum spectra show close resemblance with ASASSN-15ed hinting it to be of SN Ib nature. The low \ion{He}{1} CSM velocities and residual H$\alpha$ further justifies it and gives evidence of an intermittent progenitor between WR and LBV star.