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Recent evidence has suggested that the supernova remnant (SNR) 0104-72.3 inthe Small Magellanic Cloud (SMC) may be the result of a prompt Type Ia SN basedon enhanced iron abundances and its association with a star-forming region. Inthis paper, we present evidence that SNR 0104-72.3 arose from a jet-drivenbipolar core-collapse SN. Specifically, we use serendipitous Chandra X-rayObservatory data of SNR 0104-72.3 taken due to its proximity to the calibrationsource SNR E0102-72.3. We analyze 56 Advanced CCD Imaging Spectrometer (ACIS)observations of SNR 0104-72.3 to produce imaging and spectra with an effectiveexposure of 528.6 ks. We demonstrate that SNR 0104-72.3 is highly ellipticalrelative to other nearby young SNRs, suggesting a core-collapse SN origin.Furthermore, we compare ejecta abundances derived from spectral fits tonucleosynthetic yields of Type Ia and core-collapse (CC) SNe, and we find thatthe iron, neon, and silicon abundances are consistent with either a sphericalCC SN of a 18-20 solar mass progenitor or an aspherical CC SN of a 25 solarmass progenitor. We show that the star-formation history at the site of SNR0104-72.3 is also consistent with a CC origin. Given the bipolar morphology ofthe SNR, we favor the aspherical CC SN scenario. This result may suggestjet-driven SNe occur frequently in the low-metallicity environment of the SMC,consistent with the observational and theoretical work on broad-line Type IcSNe and long-duration gamma-ray bursts.

astrophysical journal/the astrophysical journal

Identification of a Jet-Driven Supernova Remnant in the Small Magellanic  Cloud: Possible Evidence for the Enhancement of Bipolar Explosions at Low  Metallicity