Photometry of SN 2002ic and implications for the progenitor mass-loss history

We present new premaximum and late-time optical photometry of the Type Ia/IIn supernova 2002ic. These observations are combined with the published V-band magnitudes of Hamuy and coauthors and the VLT spectrophotometry of Wang and coauthors to construct the most extensive light curve to date of this unusual supernova. The observed flux at late time is significantly higher relative to the flux at maximum than that of any other observed Type Ia supernova and continues to fade very slowly a year after the explosion. Our analysis of the light curve suggests that a non-Type Ia supernova component becomes prominent similar to20 days after explosion. Modeling of the non-Type Ia supernova component as heating from the shock interaction of the supernova ejecta with preexisting circumstellar material suggests the presence of a similar to1.7x10(15) cm gap or trough between the progenitor system and the surrounding circumstellar material. This gap could be due to significantly lower mass loss similar to15(v(w)/10 km s(-1))(-1) yr prior to explosion or evacuation of the circumstellar material by a low-density fast wind. The latter is consistent with observed properties of protoplanetary nebulae and with models of white dwarf+asymptotic giant branch star progenitor systems with the asymptotic giant branch star in the protoplanetary nebula phase.