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SN 2004et is one of the nearest and best-observed Type IIP supernovae, with aprogenitor detection as well as good photometric and spectroscopicobservational coverage well into the nebular phase. Based on nucleosynthesisfrom stellar evolution/explosion models we apply spectral modeling to analyzeits 140-700 day evolution from ultraviolet to mid-infrared. We find a M_ZAMS=15 Msun progenitor star (with an oxygen mass of 0.8 Msun) to satisfactorilyreproduce [O I] 6300, 6364 {\AA} and other emission lines of carbon, sodium,magnesium, and silicon, while 12 Msun and 19 Msun models under- and overproducemost of these lines, respectively. This result is in fair agreement with themass derived from the progenitor detection, but in disagreement withhydrodynamical modeling of the early-time light curve. From modeling of themid-infrared iron-group emission lines, we determine the density of the"Ni-bubble" to rho(t) = 7E-14*(t/100d)^-3 g cm^-3, corresponding to a fillingfactor of f = 0.15 in the metal core region (V = 1800 km/s). We also confirmthat silicate dust, CO, and SiO emission are all present in the spectra.

The progenitor mass of the Type IIP supernova SN 2004et from late-time spectral modeling