Detection of the Red Supergiant Wind from the Progenitor of Cassiopeia A

Cassiopeia A (Cas A) is one of the best studied young Galactic supernova remnants. While it provides a rare opportunity to study in detail the remnant of a supernova (SN) type IIb, questions remain regarding the nature of its progenitor, its mass-loss history, and its pre-SN evolution. Here we present an optical investigation of the circumstellar environment around Cas A and find clumpy and filamentary H alpha emission nebulosities concentrated 10-15 pc (10 '-15 ') to the north and east. First reported by Minkowski as a faint H ii region, these nebulosities exhibit distinct morphological and spectroscopic properties relative to the surrounding diffuse emissions. Compared to neighboring H ii regions, these nebulae show stronger [N ii] 6548, 6583 A and [S ii] 6716, 6731 A emissions relative to H alpha. We show that Cas A's highest-velocity ejecta knots are interacting with some of the closest projected emission nebulae, thus providing strong evidence that these nebulae lie at the same distance as the remnant. We interpret these surrounding nebulosities to be the remains of the progenitor's red supergiant wind, which accumulated against the southern edge of a large extended H ii region located north of Cas A. Our findings are consistent with the view that Cas A's progenitor underwent considerable mass loss, first from a fast main-sequence wind, then from a slower, clumpy red supergiant wind, and finally from a brief high-velocity wind, like that from a yellow supergiant.