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Fitting Complex, High-Signal SNR Spectra: Estimating Systematics & Ejecta Mass Ratios in Kepler’s SNR

Presentation #201.03 in the session Stellar/Compact I.

Published onMay 03, 2024
Fitting Complex, High-Signal SNR Spectra: Estimating Systematics & Ejecta Mass Ratios in Kepler’s SNR

The exact origins of many Type Ia supernovae—progenitor scenarios and explosive mechanisms—remain uncertain. In this work, we analyzed the global X-Ray emission of Kepler’s supernova remnant, comparing observed ejecta mass ratios to the predictions of Ia simulations. Given the high signal-to-noise of this data, the Suzaku telescope effective area calibration uncertainties of 5-20% dominated over the Poisson photon uncertainties and thus needed to be included. We generated 100 mock effective area curves and used Markov-Chain Monte Carlo based fitting to produce 100 fits, the spread of which reflects the true best-fit parameter uncertainties. Additionally, we characterized the uncertainties from assumptions made about the emitting volumes of each model plasma component and find that these uncertainties can be the dominant source of error. Our mass ratio estimates require a 90% attenuated 12C+16O reaction rate and are potentially consistent with both near- and sub-MCh progenitors for Kepler’s SNR, but are inconsistent with the dynamically stable double detonation origin scenario and only marginally consistent with the dynamically unstable dynamically-driven double-degenerate double detonation (D6) scenario. We suggest a range of progenitor and explosion property combinations—in particular, this attenuated reaction rate—for use in future Type Ia SNe simulations to place stricter constraints on Kepler’s SNR and investigate other SNRs.

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