The HI supergiant shells in the large Magellanic cloud

Details The HI supergiant shells in the large Magellanic cloud The HI supergiant shells in the large Magellanic cloud

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..393..582k&link_type=abstract

The seventh astrophysical conference: Star formation, near and far. AIP Conference Proceedings, Volume 393, pp. 582-585 (1997).

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Magellanic Clouds And Other Irregular Galaxies, Hii Regions, Emission And Reflection Nebulae

Scientific paper

We present the results of an HI aperture synthesis mosaic of the Large Magellanic Cloud (LMC), made recently with the Australian Telescope Compact Array (ATCA). The resolution of the mosaicked images is 1'0 (15 pc, using a distance to the LMC of 50 kpc). In contrast with its appearance at other wavelengths, the LMC is remarkably symmetric in HI on the largest scales, with the bulk of the HI residing in a disk of diameter 8°4 (7.3 kpc). Outer spiral structure is clearly seen, though the features appear to be caused by differential rotation, therefore transient in nature. On small to medium scales, the combined action of numerous shells and supershells dominates the structures and motions of the HI in the LMC. Some supergiant shells show good correlation between HI and Hα structures. We compare the results with a new wide-field Hα image.

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