Pastorello, A.Benetti, S.Brown, P.J.Tsvetkov, D.Y.Inserra, C.Taubenberger, S.Tomasella, L.Fraser, M.Rich, D.J.Botticella, M.T.Bufano, F.Cappellaro, E.Ergon, M.Gorbovskoy, E.S.Harutyunyan, A.Huang, F.Kotak, R.Lipunov, V.M.Magill, L.Miluzio, M.Morrell, N.Ochner, P.Smartt, S.J.Sollerman, J.Spiro, S.Stritzinger, M.D.Turatto, M.Valenti, S.Wang, X.Wright, D.E.Yurkov, V.V.Zampieri, L.Zhang, L.2023-06-072023-06-072015-05Monthly Notices of the Royal Astronomical Society Volume 449, Issue 2, Pages 1921 - 194011 May 20150035-8711https://repositorio.unab.cl/xmlui/handle/ria/50412Indexación: ScopusWe present ultraviolet, optical and near-infrared data of the Type Ibn supernovae (SNe) 2010al and 2011hw. SN 2010al reaches an absolute magnitude at peak of MR = -18.86 ± 0.21. Its early light curve shows similarities with normal SNe Ib, with a rise to maximum slower than most SNe Ibn. The spectra are dominated by a blue continuum at early stages, with narrow P-Cygni He I lines indicating the presence of a slow-moving, He-rich circumstellar medium. At later epochs, the spectra well match those of the prototypical SN Ibn 2006jc, although the broader lines suggest that a significant amount of He was still present in the stellar envelope at the time of the explosion. SN 2011hw is somewhat different. It was discovered after the first maximum, but the light curve shows a double peak. The absolute magnitude at discovery is similar to that of the second peak (MR = -18.59 ± 0.25), and slightly fainter than the average of SNe Ibn. Though the spectra of SN 2011hw are similar to those of SN 2006jc, coronal lines and narrow Balmer lines are clearly detected. This indicates substantial interaction of the SN ejecta with He-rich, but not H-free, circumstellar material. The spectra of SN 2011hw suggest that it is a transitional SN Ibn/IIn event similar to SN 2005la. While for SN 2010al the spectrophotometric evolution favours a H-deprived Wolf-Rayet progenitor (of WN-type), we agree with the conclusion of Smith et al. that the precursor of SN 2011hw was likely in transition from a luminous blue variable to an early Wolf-Rayet (Ofpe/WN9) stage. © 2015 The Authors.enSupernovaegeneralSupernovaeindividualSN 2000erSupernovaeindividualSN 2005laSupernovaeindividualSN 2006jcSupernovaeindividualSN 2010alSupernovaeindividualSN 2011hwArtículoAtribución 4.0 Internacional (CC BY 4.0)10.1093/mnras/stu2745