emission from the \[\]$\lambda\lambda$6548,6584 lines, and the ratio of \[\]/H$\alpha$ intensities was assumed to be be 0.3 in WB92, agreement between the data sets is satisfactory.

In order to easily locate the positions of WR stars within our images, the absolute orientation of the fields was determined using an astrometery routine within IDL. This program was interactively given the (X,Y) coordinates of several HST guide stars within our fields. The known ($\alpha$,$\delta$) coordinates of the guide stars were then used to determine a plate scale solution, giving each frame a positional accuracy of $\sim$1$\arcsec$ relative to the guide star reference frame.

IDENTIFICATION AND PHYSICAL OF PROPERTIES OF SHELLS
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We have classified the morphology of H$\alpha$ emission near WR stars into two groups. The first category (Group I shells) consists of shells, or shell fragments, in which the WR star is at or near the center of a single shell (Ia), or concentric limb brightened shells (Ib). We consider Group I shells as potentially being causally associated with a WR star. Note that the multiple shells presented here are probably not physically related to the multiple shells reported by Marston (1995), since the former are generally E-type shells, which are 