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
(He II, C III, N III). 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 day−1
) are consistent with SNe Ibn but less than the fast
transients. On the other hand, the Δm15 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 among the fast transients sample. The
peculiar color evolution places it between SNe Ib and the most extreme SNe Ibn. The bolometric light-curve
modeling shows resemblance with SN 2019uo with ejecta masses consistent with SNe Ib. SN 2019wep belongs to
the P cygni subclass of SNe Ibn and shows faster evolution in line velocities as compared to the emission subclass.
The post-maximum spectra show close resemblance with ASASSN-15ed hinting it to be of SN Ib nature. The low
He I CSM velocities and residual Hα further justifies it and provide evidence of an intermittent progenitor between
Wolf-Rayet and LBV stars.
