  Recent evidence has suggested that the supernova remnant (SNR) 0104-72.3 in
the Small Magellanic Cloud (SMC) may be the result of a prompt Type Ia SN based
on enhanced iron abundances and its association with a star-forming region. In
this paper, we present evidence that SNR 0104-72.3 arose from a jet-driven
bipolar core-collapse SN. Specifically, we use serendipitous Chandra X-ray
Observatory data of SNR 0104-72.3 taken due to its proximity to the calibration
source 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 effective
exposure of 528.6 ks. We demonstrate that SNR 0104-72.3 is highly elliptical
relative to other nearby young SNRs, suggesting a core-collapse SN origin.
Furthermore, we compare ejecta abundances derived from spectral fits to
nucleosynthetic yields of Type Ia and core-collapse (CC) SNe, and we find that
the iron, neon, and silicon abundances are consistent with either a spherical
CC SN of a 18-20 solar mass progenitor or an aspherical CC SN of a 25 solar
mass progenitor. We show that the star-formation history at the site of SNR
0104-72.3 is also consistent with a CC origin. Given the bipolar morphology of
the SNR, we favor the aspherical CC SN scenario. This result may suggest
jet-driven SNe occur frequently in the low-metallicity environment of the SMC,
consistent with the observational and theoretical work on broad-line Type Ic
SNe and long-duration gamma-ray bursts.
