Gutiérrez C.P.Pastorello A.Jerkstrand A.Galbany L.Sullivan M.Anderson J.P.Taubenberger S.Kuncarayakti H.González-Gaitán S.Wiseman P.Inserra C.Fraser M.Maguire K.Smartt S.Müller-Bravo T.E.Arcavi I.Benetti S.Bersier D.Bose S.Bostroem K.A.Burke J.Chen P.Chen T.-W.Della Valle M.Dong S.Gal-Yam A.Gromadzki M.Hiramatsu D.Holoien T.W.-S.Hosseinzadeh G.Howell D.A.Kankare E.Kochanek C.S.McCully C.Nicholl M.Pignata G.Prieto J.L.Shappee B.Taggart K.Tomasella L.Valenti S.Young D.R.2021-10-272021-10-272020-11Monthly Notices of the Royal Astronomical Society, Volume 499, Issue 1, Pages 974 - 9921 November 202000358711http://repositorio.unab.cl/xmlui/handle/ria/20654Indexación ScopusWe present the photometric and spectroscopic evolution of the Type II supernova (SN II) SN 2017ivv (also known as ASASSN- 17qp). Located in an extremely faint galaxy (Mr =-10.3 mag), SN 2017ivv shows an unprecedented evolution during the 2 yr of observations. At early times, the light curve shows a fast rise (~6-8 d) to a peak of Mmaxg = -17.84 mag, followed by a very rapid decline of 7.94 ± 0.48 mag per 100 d in the V band. The extensive photometric coverage at late phases shows that the radioactive tail has two slopes, one steeper than that expected from the decay of 56Co (between 100 and 350 d), and another slower (after 450 d), probably produced by an additional energy source. From the bolometric light curve, we estimated that the amount of ejected 56Ni is ~0.059 ± 0.003M⊙. The nebular spectra of SN 2017ivv show a remarkable transformation that allows the evolution to be split into three phases: (1) Ha strong phase ([removed]500 d).We find that the nebular analysis favours a binary progenitor and an asymmetric explosion. Finally, comparing the nebular spectra of SN 2017ivv to models suggests a progenitor with a zero-age main-sequence mass of 15-17M⊙. © 2020 The Author(s).enSupernovaeLight CurveWolf-Rayet StarsArtículo10.1093/mnras/staa2763