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 20 Group IIa stars, and 4 Group IIb stars. Of the 48 WR stars in our sample, 24 are surrounded by Group I shells (50$\%$) and 24 are Group II stars (50$\%$).

We suspect that Group I shells which contain one or two massive stars, or are $\leq$ 40 pc in radius, may be E- or W-type shells. There are 5 Group Ia shells that satisfy this criteria: ob69-F1, MS8, MS2, ob54wr1, and ob42wr1. All 7 inner Group Ib shells satisfy these criteria, although the outer shells for MS14 and MS4 do not. Therefore, 12 of the 24 WR stars within Group I shells (or 25$\%$ of the sample of 48) appear surrounded by resolved E- or W-type shells.

There are 12 WR stars (25$\%$ of the sample) that have excess emission within the H$\alpha$ bandpass (one WR star with excess emission is in common with the 12 WR stars surrounded by putative E- or W-type shells). The excess H$\alpha$ emission may arise from unresolved E- or W-type shells, or in an extended outer envelope 