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We present optical photometry and spectroscopy of SN2005ip for the first 3yrafter discovery, showing an underlying Type II-L SN interacting with a steadywind to yield an unusual Type IIn spectrum. For the first 160d, it had a fastlinear decline from a modest peak absolute magnitude of about -17.4(unfiltered), followed by a plateau at roughly -14.8 for more than 2yr.Initially having a normal broad-lined spectrum superposed with sparse narrowlines from the photoionized CSM, it quickly developed signs of strong CSMinteraction with a spectrum similar to that of SN1988Z. As the underlyingSNII-L faded, SN2005ip exhibited a rich high-ionization spectrum with a denseforest of narrow coronal lines, unprecedented among SNe but reminiscent of someactive galactic nuclei. The line-profile evolution of SN 2005ip confirms thatdust formation caused its recently reported infrared excess, but these linesreveal that it is the first SN to show clear evidence for dust in both the fastSN ejecta and the slower post-shock gas. SN2005ip's complex spectrum confirmsthe origin of the strange blue continuum in SN2006jc, which also had post-shockdust formation. We suggest that SN2005ip's late-time plateau and coronalspectrum result from rejuvenated CSM interaction between a sustained fast shockand a clumpy stellar wind, where X-rays escape through the optically thininterclump regions to heat the pre-shock CSM to coronal temperatures.

Coronal lines and dust formation in SN 2005ip: Not the brightest, but the hottest Type IIn supernova