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The 2012 brightening of SN 2009ip was dominated by emission from theinteraction of ejecta with the surrounding circumstellar material (CSM)produced by episodic mass loss from the progenitor, complicating the diagnosisof whether the underlying explosion was a true supernova or a nonterminaleruption of a massive star. In this paper, we contribute a time series ofoptical photometric and spectroscopic observations for SN 2009ip from 1 to 3years after the 2012 outburst, collected at the Las Cumbres Observatory and theKeck Observatory. We find that the brightness of SN 2009ip continues to declinewith no deviations from a linear slope of $0.0030\pm0.0005$ $\rm mag\ day^{-1}$in the $r^{\prime}$ band, and demonstrate that this is similar to bothobservations and models of CSM-ejecta interaction. We show that the late-timespectra continue to be dominated by the signature features of CSM interaction,and that the large ratio of $L_{\rm H\alpha}/L_{\rm H\beta}\approx40$ impliesthat the material remains optically thick to Balmer photons ("Case C"recombination). We combine our late-time photometry and spectra with early-timedata for SN 2009ip and provide a comprehensive discussion that incorporatesrecently published models and observations for transient phenomena dominated byCSM-ejecta interaction, and conclude that the presence of broad H$\alpha$ atearly times remains among the best evidence that a terminal supernova hasoccurred. Finally, we compare our late-time spectra to those of Type IIn SNeand SN impostors at late phases and find that although SN 2009ip has somesimilarities with both types, it has more differences with late-time impostorspectra.

Clues to the Nature of SN 2009ip II: The Continuing Photometric and Spectroscopic Evolution to 1000 Days