nebulae of larger size than WN stars (Miller & Chu 1993; Marston 1997; Dopita et al. 1994), possibly indicating an evolutionary sequence. We compared the size distribution of the shells surrounding WN stars with those surrounding WC stars in M31. In light of the discussion above, we restricted our comparison to shells $\leq$40 pc in radius, and containing one or two massive stars (i.e. those shells thought to be causally related to a single WR star). For this particular subset of shells (3 contain WN stars and 14 contain WC stars) we found that shells containing a WN star were on average smaller than those containing a WC star. If true, this supports the evolutionary sequence, WN $\rightarrow$ WC (Marston 1997). However, given the small number of shells (in particular those containing WN stars), our result is not statistically significant. Further, considering all shells in our sample, there are as many WN stars within small shells (putative E- or W-type) as big shells (putative R-type), as can be seen from Tables 1 & 2. We therefore caution that this result should be viewed as preliminary.

We conclude this section by discussing the excess point source H$\alpha$ emission associated with a 