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We present the photometric and spectroscopic evolution of the Type IIsupernova (SN II) SN 2017ivv (also known as ASASSN-17qp). Located in anextremely faint galaxy (M$_r=-10.3$ mag), SN 2017ivv shows an unprecedentedevolution during the two years of observations. At early times, the light curveshows a fast rise ($\sim6-8$ days) to a peak of ${\rm M}^{\rm max}_{g}= -17.84$mag, followed by a very rapid decline of $7.94\pm0.48$ mag per 100 days in the$V-$band. The extensive photometric coverage at late phases shows that theradioactive tail has two slopes, one steeper than that expected from the decayof $^{56}$Co (between 100 and 350 days), and another slower (after 450 days),probably produced by an additional energy source. From the bolometric lightcurve, we estimated that the amount of ejected $^{56}$Ni is $\sim0.059\pm0.003$M$\odot$. The nebular spectra of SN 2017ivv show a remarkable transformationthat allows the evolution to be split into three phases: (1) H$\alpha$ strongphase ($<200$ days); (2) H$\alpha$ weak phase (between 200 and 350 days); and(3) H$\alpha$ broad phase ($>500$ days). We find that the nebular analysisfavours a binary progenitor and an asymmetric explosion. Finally, comparing thenebular spectra of SN 2017ivv to models suggests a progenitor with a zero-agemain-sequence mass of 15 -- 17 \Msun.

SN 2017ivv: two years of evolution of a transitional Type II supernova