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Models for the progenitor systems of Type Ia supernovae can be divided intodouble-degenerate systems, which contain two white dwarfs, andsingle-degenerate systems, which contain one white dwarf plus one companionstar (either a red giant, a subgiant, or a >1.16 M_sol main sequence star). Thewhite dwarf is destroyed in the supernova explosion, but any non-degeneratecompanion remains intact. We present the results of a search for anex-companion star in SNR 0519-69.0, located in the Large Magellanic Cloud,based on images taken with the Hubble Space Telescope with a limiting magnitudeof V = 26.05. SNR 0519-69.0 is confidently known to be from a Type Ia supernovabased on its light echoes and X-ray spectra. The geometric center of theremnant (based on the H-alpha and X-ray shell) is at 05:19:34.83, -69:02:06.92(J2000). Accounting for the measurement uncertainties, the orbital velocity,and the kick velocity, any ex-companion star must be within 4.7" of thisposition at the 99.73% confidence level. This circle contains 27 main sequencestars brighter than V = 22.7, any one of which could be the ex-companion starleft over from a supersoft source progenitor system. The circle contains nopost-main sequence stars, and this rules out the possibility of all otherpublished single-degenerate progenitor classes (including symbiotic stars,recurrent novae, helium donors, and the spin-up/spin-down models) for thisparticular supernova. The only remaining possibility is that SNR 0519-69.0 wasformed from either a supersoft source or a double-degenerate progenitor system.

The Progenitor of the Type Ia Supernova that created SNR 0519-69.0 in the Large Magellanic Cloud