Benetti, S.Chugai, N.N.Utrobin, V.P.Cappellaro, E.Patat, F.Pastorello, A.Turatto, M.Cupani, G.Neuhäuser, R.Caldwell, N.Pignata, G.Tomasella, L.2023-11-102023-11-102016-03Monthly Notices of the Royal Astronomical Society. Volume 456, Issue 3, Pages 3296 - 3317. 1 March 20160035-8711https://repositorio.unab.cl/xmlui/handle/ria/53896Indexación: Scopus.Spectrophotometry of SN 1996al carried out throughout 15 yr is presented. The early pho tometry suggests that SN 1996al is a linear Type II supernova, with an absolute peak of MV ∼ −18.2 mag. Early spectra present broad asymmetric Balmer emissions, with superim posed narrow lines with P-Cygni profile, and He I features with asymmetric broad emission components. The analysis of the line profiles shows that the H and He broad components form in the same region of the ejecta. By day +142, the Hα profile dramatically changes: the narrow P-Cygni profile disappears, and the Hα is fitted by three emission components that will be detected over the remaining 15 yr of the supernova (SN) monitoring campaign. Instead, the He I emissions become progressively narrower and symmetric. A sudden increase in flux of all He I lines is observed between 300 and 600 d. Models show that the SN luminosity is sustained by the interaction of low-mass (∼1.15 M ) ejecta, expelled in a low kinetic energy (∼1.6 × 1050 erg) explosion, with highly asymmetric circumstellar medium. The detection of Hα emission in pre-explosion archive images suggests that the progenitor was most likely a massive star (∼25 M ZAMS) that had lost a large fraction of its hydrogen envelope be fore explosion, and was hence embedded in a H-rich cocoon. The low-mass ejecta and modest kinetic energy of the explosion are explained with massive fallback of material into the compact remnant, a 7–8-M black hole.enSupernovae: GeneralArtículo10.1093/mnras/stv2811