barely resolved in our data. The second category (Group II stars) consists of WR stars where there is no clear causal relation with nearby H$\alpha$ emission (IIa), or a lack of nearby H$\alpha$ emission (IIb). Group IIa consists of WR stars that are either near amorphous, diffuse H$\alpha$ emission, or on the edge of regions, and therefore have no preferred location with respect to an shell. There are 17 WR stars surrounded by Group Ia shells, 7 stars surrounded by Group Ib shells, 20 Group IIa stars, and 4 Group IIb stars.

H$\alpha$ fluxes were computed for Group I shells, but not for nebular emission near Group II stars. Polygonal masks (shown in Figure 1, see below) used to compute the fluxes were chosen such that they most likely contain all emission from a given shell. Regions for Group Ia shells are generally circular or elliptical in shape. The multiple polygons for Group Ib shells are concentric in nature. The interior polygons defined for Group Ib shells are used to compute the fluxes of the inner shells, and the outer polygons are used to compute the fluxes of the inner+outer shells. Outer shell fluxes then are obtained as the difference 