2012A&A...546A..28J

SN 2004et is one of the nearest and best-observed Type IIP supernovae, with a progenitor detection as well as good photometric and spectroscopic observational coverage well into the nebular phase. Based on nucleosynthesis from stellar evolution/explosion models we apply spectral modeling to analyze its 140-700 day evolution from ultraviolet to mid-infrared. We find a M_ZAMS=15M_☉ progenitor star (with an oxygen mass of 0.8M_☉) to satisfactorily reproduce [OI] λλ6300, 6364 and other emission lines of carbon, sodium, magnesium, and silicon, while 12M_☉ and 19M_☉ models under- and overproduce most of these lines, respectively. This result is in fair agreement with the mass derived from the progenitor detection, but in disagreement with hydrodynamical modeling of the early-time light curve. From modeling of the mid-infrared iron-group emission lines, we determine the density of the ``Ni-bubble'' to ρ(t)≃7x10^–14x(t/100 d)^–3g/cm3, corresponding to a filling factor of f=0.15 in the metal core region (V=1800km/s). We also confirm that silicate dust, CO, and SiO emission are all present in the spectra.