& Smith (1997) find that four LMC WN9-11 stars show nebular H$\alpha$ emission lines (equivalent widths ranging from 32 to 83 ${\rm \AA}$) superimposed on their stellar spectra, which is circumstellar and not from an underlying region.

WR WIND-ISM INTERACTIONS
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Figure 1c contains an image of the Group Ia shell surrounding MS11 and the Group Ib shell surrounding MS12. The bright star near the top of the B-band image is a foreground star. MS11 is off-set from the center of a large, limb-brightened bubble, and is part of a chain of OB stars. To the south-west of MS11 is a multiple shell surrounding the WR star MS12. MS12 is at the center of a small inner shell, and offset to the west from the center of the outer shell. MS12 is the only nearby ionizing star, which is supported by the flux of ionizing photons implied by the H$\alpha$ luminosity of the surrounding shells.

Interestingly, there is morphological evidence that the shells surrounding these stars may be interacting. Pointing radially away from MS11 is a faint loop of H$\alpha$ emission. Perhaps not coincidentally, the outer shell surrounding MS12 appears to be impinging on the shell surrounding MS11, directly south 