Moran S.Fraser M.Kotak R.Pastorello A.Benetti S.Brennan S.J.Gutiérrez C.P.Kankare E.Kuncarayakti H.Mattila S.Reynolds T.M.Anderson J.P.Brown P.J.Campana S.Chambers K.C.Chen T.-W.Della Valle M.Dennefeld M.Elias-Rosa N.Galbany L.Galindo-Guil F.J.Gromadzki M.Hiramatsu D.Inserra C.Leloudas G.Müller-Bravo T.E.Nicholl M.Reguitti A.Shahbandeh M.Smartt S.J.Tartaglia L.Young D.R.2024-03-272024-03-272023-01Astronomy and Astrophysics. Volume 669. 1 January 2023. Article number A510004-6361https://repositorio.unab.cl/handle/ria/55363Indexación: Scopus.In this study we present the results of a five-year follow-up campaign of the long-lived type IIn supernova SN 2017hcc, found in a spiral dwarf host of near-solar metallicity. The long rise time (57 ± 2 days, ATLAS o band) and high luminosity (peaking at -20.78 ± 0.01 mag in the ATLAS o band) point towards an interaction of massive ejecta with massive and dense circumstellar material (CSM). The evolution of SN 2017hcc is slow, both spectroscopically and photometrically, reminiscent of the long-lived type IIn, SN 2010jl. An infrared (IR) excess was apparent soon after the peak, and blueshifts were noticeable in the Balmer lines starting from a few hundred days, but appeared to be fading by around +1200 d. We posit that an IR light echo from pre-existing dust dominates at early times, with some possible condensation of new dust grains occurring at epochs ≳;+800 d. © The Authors 2023.enSupernovae: generalSupernovae: individual: ATLAS17lsnSupernovae: individual: PS17fraSupernovae: individual: SN 2017hccArtículoCC BY 4.0 DEED Attribution 4.0 International10.1051/0004-6361/202244565