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We present nebular phase optical and near-infrared spectroscopy of the TypeIIP supernova SN 2012aw combined with NLTE radiative transfer calculationsapplied to ejecta from stellar evolution/explosion models. Our spectralsynthesis models generally show good agreement with the ejecta from a MZAMS =15 Msun progenitor star. The emission lines of oxygen, sodium, and magnesiumare all consistent with the nucleosynthesis in a progenitor in the 14 - 18 Msunrange. We also demonstrate how the evolution of the oxygen cooling lines of [OI] 5577 A, [O I] 6300 A, and [O I] 6364 A can be used to constrain the mass ofoxygen in the non-molecularly cooled ashes to < 1 Msun, independent of themixing in the ejecta. This constraint implies that any progenitor model ofinitial mass greater than 20 Msun would be difficult to reconcile with theobserved line strengths. A stellar progenitor of around MZAMS = 15 Msun canconsistently explain the directly measured luminosity of the progenitor star,the observed nebular spectra, and the inferred pre-supernova mass-loss rate. Weconclude that there is still no convincing example of a Type IIP explosionshowing the nucleosynthesis expected from a MZAMS > 20 Msun progenitor.

The nebular spectra of SN 2012aw and constraints on stellar nucleosynthesis from oxygen emission lines