Spatial coverage of the S³MC data, overlaid on the Hα "parking lot camera" image of the SMC (Kennicutt et al. 1995). The white outline indicates the coverage of the IRAC observations, while the gray outline shows the coverage for MIPS. Note that this is only approximate, since the placement of the cameras on the Spitzer focal plane results in slightly different areas of the sky mapped for the different wave bands. The SMC bar is the region where the bulk of the star formation (indicated by Hα emission) takes place, extending roughly from (﹩01^{\mathrm{h}\,}15^{\mathrm{m}\,}﹩, −73°30^{﹩\arcmin﹩}) to (﹩00^{\mathrm{h}\,}54^{\mathrm{m}\,}﹩, −72°00^{﹩\arcmin﹩}). The wing region, notable in H I but with very little diffuse Hα emission, is approximately perpendicular to the bar and extends eastward from (﹩01^{\mathrm{h}\,}00^{\mathrm{m}\,}﹩, −72°45^{﹩\arcmin﹩}) to (﹩00^{\mathrm{h}\,}45^{\mathrm{m}\,}﹩, −73°15^{﹩\arcmin﹩}) and beyond.