Abstract
Abstract
We present the first systematic, spatially resolved X-ray spectroscopic study of a largely thermonuclear (Type Ia) sample of supernova remnants (SNRs), aimed at probing the explosion properties and progenitors through a comparison to a suite of nucleosynthesis models available in the literature. Our sample focuses on Galactic and Large Magellanic Cloud ejecta-dominated SNRs believed to be, or otherwise assumed to be, of thermonuclear origin. Using archival XMM-Newton observations (and Chandra for G1.9+0.3), we extract spectra from adaptively binned regions across each remnant and model the emission to constrain the plasma temperature, ionization timescale, and ejecta abundances. We then compare abundance ratios (relative to Si) to a library of 335 individual models spanning 11 commonly used supernova nucleosynthesis simulation sets from the literature, including seven thermonuclear and four core-collapse sets. Across the sample, we find that individual remnants can be well matched by subsets of models, but no single model reproduces all measured elemental ratios at once. As a result, the best fit model for a given object is typically set by a selection of well-fitted abundance ratios, highlighting both the strength and limitations in yield-based model determination. For some SNRs, the abundance comparisons show better agreement with particular families of Type Ia supernova explosions, including near-Chandrasekhar-mass delayed detonations, sub-Chandrasekhar-mass explosions, and dynamically driven double detonations, although these interpretations are not unique. Finally, we outline the need for model improvements, including refined nuclear reaction rates, higher dimensional treatment of mixing and turbulence, expanded metallicity coverage, and the exploration of nonstandard SN explosion energies.