Despite the wealth of observational data available for Cassiopeia A, the
suggestions for its progenitor span a wide array of stellar types. We
compare a suite of 3D explosion calculations and stellar models
incorporating advanced physics with observational constraints on the
progenitor. We consider binary and single stars from 16 to 40 \sol with a
range of explosion energies and geometries. The parameter space allowed by
observations of nitrogen rich high velocity ejecta, ejecta mass, compact
remnant mass, and $^{44}$Ti and $^{56}$Ni abundances individually and as an
ensemble is considered. A progenitor of 15-25 \sol which loses its hydrogen
envelope to a binaryinteraction and undergoes an energetic explosion can match all the
observational constraints.
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