stars in M31. Our results are based on new and previously published H$\alpha$, H$\alpha$+\[\], and \[\] imaging data of M31 obtained at Kitt Peak National Observatory. M31 is attractive for this type of study due its proximity (nebulae are resolvable down to radii of $\sim$7 pc) and the fact that it provides a uniform sample of WR stars at a well known distance (690 kpc). Surveys for WR stars in M31, while not complete, have resulted in a catalog of 48 WR stars (Massey & Johnson 1998). Another WR star has recently been discovered by Galarza, Walterbos, & Braun (1999).

We present H$\alpha$ and B images of the 48 of these 49 WR stars which fell within the area we imaged, and compile a catalog of ionized hydrogen nebular “shells” in their vicinity. Deciding when an shell is physically associated with a WR star (i.e. an E- or W-type shell) is not easy, since most WR stars are located close to other massive stars and near classical regions. Given the small size of Galactic E-shells we can barely resolve the larger shells of this type, but can easily resolve W- and R-type shells. Although we cannot distinguish W- and R-type 