Pian, E.Mazzali, P.A.Moriya, T.J.Rubin, A.Gal-Yam, A.Arcavi, I.Ben-Ami, S.Blagorodnova Mujortova, NadejdaBufano, F.Filippenko, A.V.Kasliwal, M.Kulkarni, S.R.Lunnan, R.Manulis, I.Matheson, T.Nugent, P.E.Ofek, E.Perley, D.A.Prentice, S.J.Yaron, O.2025-06-252025-06-2520200035-8711https://hdl.handle.net/2445/221759The hydrogen-poor supernova (SN) PTF11rka (z = 0.0744), reported by the Palomar Transient Factory, was observed with various telescopes starting a few days after the estimated explosion time of 2011 December 5 UT and up to 432 rest-frame days thereafter. The rising part of the light curve was monitored only in the RPTF filter band, and maximum in this band was reached ∼30 rest-frame days after the estimated explosion time. The light curve and spectra of PTF11rka are consistent with the core-collapse explosion of a ∼10 M carbon–oxygen core evolved from a progenitor of main-sequence mass 25–40 M, that liberated a kinetic energy Ek≈4 × 1051 erg, expelled ∼8 M of ejecta, and synthesized ∼0.5 M of 56Ni. The photospheric spectra of PTF11rka are characterized by narrow absorption lines that point to suppression of the highest ejecta velocities ( 15 000 km s−1). This would be expected if the ejecta impacted a dense, clumpy circumstellar medium. This in turn caused them to lose a fraction of their energy (∼5 × 1050 erg), less than 2 per cent of which was converted into radiation that sustained the light curve before maximum brightness. This is reminiscent of the superluminous SN 2007bi, the light-curve shape and spectra of which are very similar to those of PTF11rka, although the latter is a factor of 10 less luminous and evolves faster in time. PTF11rka is in fact more similar to gamma-ray burst SNe in luminosity, although it has a lower energy and a lower Ek/Mej ratio.15 p.application/pdfeng(c) Pian, E. et al., 2020Formació de les galàxiesTransferència radiativaEstelsGalaxy formationRadiative transferStarsinfo:eu-repo/semantics/article7570662025-06-25info:eu-repo/semantics/openAccess