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Type Ibn Supernovae (SNe Ibn) show signatures of strong interaction betweenthe SN ejecta and hydrogen-poor circumstellar matter (CSM). Deriving the ejectaand CSM properties of SNe Ibn provides a great opportunity to study the finalevolution of massive stars. In the present work, we present a light curve (LC)model for the ejecta-CSM interaction, taking into account the processes inwhich the high-energy photons originally created at the forward and reverseshocks are converted to the observed emission in the optical. The model isapplied to a sample of SNe Ibn and `SN Ibn' rapidly evolving transients. Weshow that the characteristic post-peak behavior commonly seen in the SN IbnLCs, where a slow decay is followed by a rapid decay, is naturally explained bythe transition of the forward-shock property from cooling to adiabatic regimewithout introducing a change in the CSM density distribution. The(commonly-found) slope in the rapid decay phase indicates a steep CSM densitygradient (rho_CSM ~ r^{-3}), inferring a rapid increase in the mass-loss ratetoward the SN as a generic properties of the SN Ibn progenitors. From thederived ejecta and CSM properties, we argue that massive Wolf-Rayet stars withthe initial mass of >~ 18 Msun can be a potential class of the progenitors. Thepresent work also indicates existence of currently missing population ofUV-bright rapid transients for which the final mass-loss rate is lower than theoptical SNe Ibn, which can be efficiently probed by future UV missions.

Properties of Type Ibn Supernovae: Implications for the Progenitor Evolution and the Origin of a Population of Rapid Transients