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We present a study of the Galactic supernova remnant (SNR) G292.0+1.8, aclassic example of a core-collapse SNR that contains oxygen-rich ejecta,circumstellar material, a rapidly moving pulsar, and a pulsar wind nebula(PWN). We use hydrodynamic simulations of the remnant evolution to show thatthe SNR reverse shock is interacting with the PWN and has most likely shockedthe majority of supernova ejecta. In our models, such a scenario requires atotal ejecta mass of $\lesssim 3\: \rm M_{\odot}$ and implies that there is nosignificant quantity of cold ejecta in the interior of the reverse shock. Inlight of these results, we compare the estimated elemental masses and abundanceratios in the reverse-shocked ejecta to nucleosynthesis models and find thatthey are consistent with a progenitor star with an initial mass of 12-16 $\:\rm M_{\odot}$. We conclude that the progenitor of G292.0+1.8 was likely arelatively low mass star that experienced significant mass loss through abinary interaction and would have produced a stripped-envelope supernovaexplosion. We also argue that the region known as the "spur" in G292.0+1.8arises as a result of the pulsar's motion through the supernova ejecta and thatits dynamical properties may suggest a line-of-sight component to the pulsar'svelocity, leading to a total space velocity of $\sim 600\: \rm km\:s^{-1}$ andimplying a significant natal kick. Finally, we discuss binary mass lossscenarios relevant to G292.0+1.8 and their implications for the binarycompanion properties and future searches.

SNR G292.0+1.8: A Remnant of a Low-Mass Progenitor Stripped-Envelope Supernova