used to compute the shell fluxes are indicated. The B images serve as finder charts and illustrate the spatial distribution of surrounding luminous stars. Figure 1b is the same as Figure 1a, but contains images of Group Ia shells from WB92. The H$\alpha$ images lack contribution from \[\]$\lambda\lambda$6548,6584 emission in this case. Group Ib shells are shown in Figure 1c from the 1997 data set and in Figure 1d from WB92. We note that the Group Ia shell surrounding MS11 appears in Figure 1c, due to its proximity with MS12, which is surrounded by a Group Ib shell. The names of the WR star(s) appearing in the images are written above the blue images. The central WR star name appears first whenever there is more than one WR star per image. Tables 1 & 2 contain a listing of the properties of the shells presented in Figure 1, including the spectral subtype of the central star and its coordinates, radii of the shells, and integrated H$\alpha$ luminosities (uncorrected for possible extinction).

Images of Group IIa stars are shown in Figure 2a, from the 1997 data set, and Figure 2b, from WB92. Due to the proximity of ob33wr3 and ob33wr2, the 