Fig. 1. Halpha image of the supergiant shell LMC 4. A number of superbubbles, bubbles, and SNRs are located along the periphery of LMC 4. The field of view is 1600 pc × 1800 pc. This Halpha image is reproduced from a PDS scan of Kennicutt & Hodge's (1986) Curtis Schmidt plate

Fig. 2. X-ray image of the LMC in the R5 band (0.56-1.21 keV). This ROSAT PSPC mosaic was made by Snowden & Petre (1994). Courtesy of Steve Snowden

Fig. 3. Halpha image of the LMC. The field of view is the same as that of Fig. 2. Courtesy of Sungeun Kim (1998)

Fig. 4. Top: A mosaic of the HRI survey data centered on the 30 Doradus region. The field of view is 140' × 110', or 2100 pc × 1650 pc.
Bottom: An Halpha image of the same field, reproduced from a PDS scan of Kennicutt & Hodge's (1986) Curtis Schmidt plate

Fig. 5 Halpha (left) and X-ray (right) images of the SNR DEM L 316, presented by Williams et al. (1997). The Halpha image was taken with the Curtis Schmidt Telescope by Chris Smith. The X-ray image is extracted from the ROSAT HRI observation rh500232 in the 0.1-2.0 keV band

Fig. 6. HST WFPC2 Halpha image of the SNR N63A overlaid by X-ray contour. The X-ray contours are derived from the ROSAT HRI observation rh500173

Fig. 7. Halpha (left) and X-ray (right) images of N44. The Halpha image was taken with the Curtis Schmidt Telescope by Chris Smith. The X-ray image is extracted from the ROSAT PSPC observation rp500093 in the 0.1-2.4 keV band

Fig. 8. Left: X-ray image of the central 9' × 9' of 30 Dor, extracted from the ROSAT PSPC observation rp500131 in the 0.1-2.4 keV band. The bright point source at the center is within a few arcsec from R136.
Right: Long-slit Halpha echellograms of the same region, reproduced from Chu & Kennicutt (1994). The wavelength increases upwards. The separation between adjacent slits corresponds to 45" in sky or 600 km s^-1 in velocity