to be consistent with the H$\alpha$ luminosities of Group I shells. Our choice of B - V $\leq$ 0 was prompted by considering the following two factors. First, there are substantial uncertainties in the photometry from the Magnier catalog. Second, we have made no reddening corrections. Thus the color information on stars in the field is, unfortunately, crude. Note in Figure 4 that Group I shells with radii less than $\sim$40 pc generally contain one or two ionizing stars.

Rosado (1986) reported the radii of shells associated with (a) single WR stars, (b) single OB stars, and (c) multiple OB & WR stars in the LMC. The mean radii are, respectively, 15$\pm$7 pc, 27$\pm$4 pc, and 69$\pm$33 pc (Rosado 1986). Single massive stars in the LMC are surrounded by shells up to $\sim$30 pc in radius, consistent with the radius estimated above for Group I shells

We suggest, allowing for chance alignment, those shells containing one or two ionizing stars (including a WR star), or that are $\leq$ 40 pc in radius, are possibly of E- or W-type. There are 5 Group Ia shells that satisfy this criteria: ob69-F1, MS8, MS2, ob54wr1, and ob42wr1. All 7 inner Group Ib shells 