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The nebular spectra of SN 2012aw and constraints on stellar nucleosynthesis from oxygen emission lines
Stockholm University, Faculty of Science, Department of Astronomy.
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2014 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 439, no 4, 3694-3703 p.Article in journal (Refereed) Published
Abstract [en]

We present nebular-phase optical and near-infrared spectroscopy of the Type IIP supernova SN 2012aw combined with non-local thermodynamic equilibrium radiative transfer calculations applied to ejecta from stellar evolution/explosion models. Our spectral synthesis models generally show good agreement with the ejecta from a M-ZAMS = 15 M-circle dot progenitor star. The emission lines of oxygen, sodium, and magnesium are all consistent with the nucleosynthesis in a progenitor in the 14-18 M-circle dot range. We also demonstrate how the evolution of the oxygen cooling lines of [O i] lambda 5577, [O i] lambda 6300, and [O i] lambda 6364 can be used to constrain the mass of oxygen in the non-molecularly cooled ashes to < 1 M-circle dot, independent of the mixing in the ejecta. This constraint implies that any progenitor model of initial mass greater than 20 M-circle dot would be difficult to reconcile with the observed line strengths. A stellar progenitor of around M-ZAMS = 15 M-circle dot can consistently explain the directly measured luminosity of the progenitor star, the observed nebular spectra, and the inferred pre-supernova mass-loss rate. We conclude that there is still no convincing example of a Type IIP supernova showing the nucleosynthesis products expected from an M-ZAMS > 20 M-circle dot progenitor.

Place, publisher, year, edition, pages
2014. Vol. 439, no 4, 3694-3703 p.
Keyword [en]
radiative transfer, stars: evolution, supernovae: general, supernovae: individual: SN 2012aw
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:su:diva-104571DOI: 10.1093/mnras/stu221ISI: 000334115400038OAI: diva2:724348


Available from: 2014-06-12 Created: 2014-06-11 Last updated: 2014-06-13Bibliographically approved

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Fransson, ClaesSollerman, JesperTaddia, Francesco
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