Kangas, T.Mattila, S.Kankare, E.Lundqvist, P.Väisänen, P.Childress, M.Pignata, G.McCully, C.Valenti, S.Vinkó, J.Pastorello, A.Elias-Rosa, N.Fraser, M.Gal-Yam, A.Kotak, R.Kotilainen, J. K.Smartt, S. J.Galbany, L.Harmanen, J.Howell, D. A.Inserra, C.Marion, G. H.Quimby, R. M.Silverman, J. M.Szalai, T.Wheeler, J. C.Ashall, C.Benetti, S.Romero-Cañizales, C.Smith, K. W.Sullivan, M.Takáts, K.Young, D. R.2017-08-182017-08-182016-02Monthly Notices of the Royal Astronomical Society Volume 456, Issue 1, 2016, Pages 323-3460035-8711https://doi.org/10.1093/mnras/stv2567http://repositorio.unab.cl/xmlui/handle/ria/3973Indexación: Web of Science; Scopus.We 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 Co-56 decay with full. gamma-ray trapping. Initially, the spectrum was blue and featureless. Later on, a strong broad (similar to 8000 km s(-1)) H alpha 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(V) = 2.9 +/- 0.2 mag and an age of 10(+ 3) (- 2) 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.enSupernovae: general2013fc-galaxies; starburstArtículo