subset of WR stars in the 1997 and WB92 data. There are 12 stars with possible excess emission in the H$\alpha$ passband. Tables 1 & 2 list the luminosities and equivalent widths of the excess emission for those WR stars within Group I shells, and Table 3 for those stars in Group IIa. No stars within Group IIb have excess emission. Excess H$\alpha$ emission associated with WR stars might indicate unresolved E- or W-shells, or emission from a WR stellar wind. We note that a small contribution from stellar $\lambda$6562 may also be present in the H$\alpha$ passband, but not enough to explain the equivalent widths of the excess emission. The luminosities of the excess emission range from 3 to 10 $\times$ 10$^{\rm 34}$ ergs s$^{\rm -1}$, the equivalent widths from 5 to 240 ${\rm \AA}$. By way of comparison, the Galactic stellar ejecta nebula RCW 58 has an H$\alpha$ luminosity of 1 $\times$ 10$^{\rm 35}$ ergs s$^{\rm -1}$ (Drissen et al. 1991), and WNL 313846 has a broad H$\alpha$ emission line, with an equivalent width of 23 ${\rm \AA}$, interpreted as arising in an extended outer envelop and indicative of a strong stellar wind (Crowther & Bohannan 1997). Crowther 