Type Ibn supernovae (SNe) are characterized by narrow helium () lines from photons produced by the unshocked circumstellar material (CSM). About 80 SNe Ibn have been discovered to date and only a handful of them have extensive observational records. Thus, many open questions remain regarding the progenitor system and the origin of CSM. He i Here, we investigate potential correlations between the spectral features of the prominent łambda 5876 Å line and the optical and X-ray light curve properties of Type Ibn SNe (SNe Ibn). He i We compiled the largest sample of 61 SNe Ibn to date, of which 24 SNe have photometric and spectroscopic data available from the Young Supernova Experiment and 37 SNe benefit from archival datasets. We fit 24 SNe Ibn with sufficient photometric coverage (B to z bands) using semi-analytical models from. We demonstrate that the light curves of SNe Ibn are more diverse than previous analyses suggest, with absolute r-band peak magnitudes (r_̊m max) of -19. 4± 0. 6 mag, along with rise (from -10 days to peak, γ_-10) and decay rates (from peak to +10 days; γ_+10) of -0. 08 ± 0. 06 and 0. 08± 0. 03 mag/day, respectively. We find that the majority of SNe Ibn in the subsample are consistent with a low-energy explosion (<10⁵1 erg) of a star with a compact envelope surrounded by ∼0. 1 of helium-rich CSM. The inferred ejecta masses are small (M_ ej ∼ 1 lines, associated with the CSM, peaks at ∼ 1100 km/s. and expand with a velocity of ∼5000 km/s. Our spectroscopic analysis shows that the mean velocity of the narrow component of the The mean CSM and ejecta masses inferred for a subsample of SNe Ibn indicate that their progenitors are not massive (sim10 single stars at the moment of explosion; rather, they are likely to be binary systems. This finding is in agreement with detections of potential companion stars of SNe Ibn progenitors and inferred CSM properties from stellar evolution models.
Farias et al. (2026) studied this question.