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We report on our discovery and observations of the Pan-STARRS1 supernova (SN)PS1-12sk, a transient with properties that indicate atypical star formation inits host galaxy cluster or pose a challenge to popular progenitor system modelsfor this class of explosion. The optical spectra of PS1-12sk classify it as aType Ibn SN (c.f. SN 2006jc), dominated by intermediate-width (3x10^3 km/s) andtime variable He I emission. Our multi-wavelength monitoring establishes therise time dt = 9-23 days and shows an NUV-NIR SED with temperature > 17x10^3 Kand a peak rise magnitude of Mz = -18.9 mag. SN Ibn spectroscopic propertiesare commonly interpreted as the signature of a massive star (17 - 100 M_sun)explosion within a He-enriched circumstellar medium. However, unlike previousType Ibn supernovae, PS1-12sk is associated with an elliptical brightestcluster galaxy, CGCG 208-042 (z = 0.054) in cluster RXC J0844.9+4258. Theexpected probability of an event like PS1-12sk in such environments is lowgiven the measured infrequency of core-collapse SNe in red sequence galaxiescompounded by the low volumetric rate of SN Ibn. Furthermore, we find noevidence of star formation at the explosion site to sensitive limits (SigmaHalpha < 2x10^-3 M_sun/yr/kpc^2). We therefore discuss white dwarf binarysystems as a possible progenitor channel for SNe Ibn. We conclude that PS1-12skrepresents either a fortuitous and statistically unlikely discovery, evidencefor a top-heavy IMF in galaxy cluster cooling flow filaments, or the first cluesuggesting an alternate progenitor channel for Type Ibn SNe.

PS1-12sk is a Peculiar Supernova From a He-rich Progenitor System in a Brightest Cluster Galaxy Environment