Kangas, T.T.KangasMattila, S.S.MattilaKankare, E.E.KankareLundqvist, P.P.LundqvistVäisänen, P.P.VäisänenChildress, M.M.ChildressPignata, G.G.PignataMcCully, C.C.McCullyValenti, S.S.ValentiVinkó, J.J.VinkóPASTORELLO, AndreaAndreaPASTORELLOELIAS DE LA ROSA, NANCY DEL CARMENNANCY DEL CARMENELIAS DE LA ROSAFraser, M.M.FraserGal-Yam, A.A.Gal-YamKotak, R.R.KotakKotilainen, J. K.J. K.KotilainenSmartt, S. J.S. J.SmarttGalbany, L.L.GalbanyHarmanen, J.J.HarmanenHowell, D. A.D. A.HowellInserra, C.C.InserraMarion, G. H.G. H.MarionQuimby, R. M.R. M.QuimbySilverman, J. M.J. M.SilvermanSzalai, T.T.SzalaiWheeler, J. C.J. C.WheelerAshall, C.C.AshallBENETTI, StefanoStefanoBENETTIRomero-Cañizales, C.C.Romero-CañizalesSmith, K. W.K. W.SmithSullivan, M.M.SullivanTakáts, K.K.TakátsYoung, D. R.D. R.Young2020-05-072020-05-0720160035-8711http://hdl.handle.net/20.500.12386/24615We present photometric and spectroscopic observations of SN 2013fc, a bright type II supernova (SN) in a circumnuclear star-forming ring in the luminous infrared galaxy ESO 154-G010, observed as part of the Public ESO Spectroscopic Survey of Transient Objects. SN 2013fc is both photometrically and spectroscopically similar to the well-studied type IIn SN 1998S and to the bright type II-L SN 1979C. It exhibits an initial linear decline, followed by a short plateau phase and a tail phase with a decline too fast for <SUP>56</SUP>Co decay with full γ-ray trapping. Initially, the spectrum was blue and featureless. Later on, a strong broad (∼8000 km s<SUP>-1</SUP>) H α emission profile became prominent. We apply a STARLIGHT stellar population model fit to the SN location (observed when the SN had faded) to estimate a high extinction of A<SUB>V</SUB> = 2.9 ± 0.2 mag and an age of 10_{-2}^{+3} Myr for the underlying cluster. We compare the SN to SNe 1998S and 1979C and discuss its possible progenitor star considering the similarities to these events. With a peak brightness of B = -20.46 ± 0.21 mag, SN 2013fc is 0.9 mag brighter than SN 1998S and of comparable brightness to SN 1979C. We suggest that SN 2013fc was consistent with a massive red supergiant (RSG) progenitor. Recent mass loss probably due to a strong RSG wind created the circumstellar matter illuminated through its interaction with the SN ejecta. We also observe a near-infrared excess, possibly due to newly condensed dust.STAMPAenArticle10.1093/mnras/stv25672-s2.0-849595149960003680100000592016MNRAS.456..323KFIS/05 - ASTRONOMIA E ASTROFISICA