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SN2006tf is the third most luminous SN discovered so far, after SN2005ap andSN2006gy. SN2006tf is valuable because it provides a link between two regimes:(1) luminous type IIn supernovae powered by emission directly from interactionwith circumstellar material (CSM), and (2) the most extremely luminous SNewhere the CSM interaction is so optically thick that energy must diffuse outfrom an opaque shocked shell. As SN2006tf evolves, it slowly transitions fromthe second to the first regime as the clumpy shell becomes more porous. Thislink suggests that the range in properties of the most luminous SNe is largelydetermined by the density and speed of H-rich material ejected shortly beforethey explode. The total energy radiated by SN2006tf was at least 7e50 ergs. Ifthe bulk of this luminosity came from the thermalization of shock kineticenergy, then the star needs to have ejected ~18 Msun in the 4-8 yr before corecollapse, and another 2-6 Msun in the decades before that. A Type Ia explosionis therefore excluded. From the H-alpha emission-line profile, we derive ablast-wave speed of 2,000 km/s that does not decelerate, and from the narrow PCygni absorption from pre-shock gas we deduce that the progenitor's wind speedwas ~190 km/s. This is reminiscent of the wind speeds of LBVs, but not of RSGsor WR stars. We propose that like SN2006gy, SN2006tf marked the death of a verymassive star that retained its H envelope until the end of its life, andsuffered extreme LBV-like mass loss in the decades before it exploded.

SN 2006tf: Precursor Eruptions and the Optically Thick Regime of Extremely Luminous Type IIn Supernovae