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The geometric structure of supernova remnants (SNR) provides a clue tounveiling the pre-explosion evolution of their progenitors. Here we present anX-ray study of N103B (0509-68.7), a Type Ia SNR in the Large Magellanic Cloud,that is known to be interacting with dense circumstellar matter (CSM). Applyingour novel method for feature extraction to deep Chandra observations, we havesuccessfully resolved the CSM, Fe-rich ejecta, and intermediate-mass element(IME) ejecta components, and revealed each of their spatial distribution.Remarkably, the IME ejecta component exhibits a double-ring structure, implyingthat the SNR expands into an hourglass-shape cavity and thus forms bipolarbubbles of the ejecta. This interpretation is supported by more quantitativespectroscopy that reveals a clear bimodality in the distribution of theionization state of the IME ejecta. These observational results can benaturally explained if the progenitor binary system had formed a dense CSMtorus on the orbital plane prior to the explosion, providing further evidencethat the SNR N103B originates from a single-degenerate progenitor.

Discovery of Double-Ring Structure in the Supernova Remnant N103B: Evidence for Bipolar Winds from a Type Ia Supernova Progenitor