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Massive binaries play an important role in fields ranging from gravitationalwave astronomy to stellar evolution. We provide several lines of evidence thatclassical OBe stars in the Small Magellanic Cloud (SMC) obtain their rapidrotation from mass and angular momentum transfer in massive binaries, whichpredicts that the subsequent supernovae should often eject OBe stars into thefield. We find that (1) OBe stars have a higher field frequency than OB stars;(2) our cumulative distribution function (CDF) of stellar distances from Ostars shows that OBe stars are indeed much more isolated than ordinary OB starsof corresponding spectral types; (3) the CDFs of OBe stars approach that ofhigh-mass X-ray binaries (HMXBs), which are confirmed post-supernova objects;and (4) Oe stars are as isolated from clusters as Be stars, implying that theirfinal masses are relatively independent of their initial masses, consistentwith major mass transfer. Lastly, we also find that the spatial distribution ofsupergiant OBe stars differs from that of classical OBe stars, consistent withthe different mechanism responsible for their emission-line spectra.

Classical OBe Stars as Post-Supernova Runaways: Confirming Binary Origins