Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-26T05:17:54.707Z Has data issue: false hasContentIssue false
  • English
  • Français

The HI Supergiant Shells in the Large Magellanic Cloud

Published online by Cambridge University Press:  12 April 2016

S. Kim ,
L. Staveley-Smith ,
R.J. Sault ,
M.J. Kesteven ,
D. McConnell ,
M.A. Dopita  and
M. Bessell
S. Kim
Affiliation:
Mount Stromlo and Siding Spring Observatories, Weston Creek PO. ACT 2611, Australia
L. Staveley-Smith
Affiliation:
Australia Telescope National Facility, CSIRO, 76 Epping, NSW 2121, Australia
R.J. Sault
Affiliation:
Australia Telescope National Facility, CSIRO, 76 Epping, NSW 2121, Australia
M.J. Kesteven
Affiliation:
Australia Telescope National Facility, CSIRO, 76 Epping, NSW 2121, Australia
D. McConnell
Affiliation:
Australia Telescope National Facility, CSIRO, 76 Epping, NSW 2121, Australia
M.A. Dopita
Affiliation:
Mount Stromlo and Siding Spring Observatories, Weston Creek PO. ACT 2611, Australia
M. Bessell
Affiliation:
Mount Stromlo and Siding Spring Observatories, Weston Creek PO. ACT 2611, Australia

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present the result of an HI aperture synthesis mosaic of the Large Magellanic cloud (LMC), made recently with the Australia Telescope Compact Array (ATCA). The resolution of the mosaiced images is l′.0 (15 pc, using a distance to the LMC of 50 kpc). In contrast to its appearance at other wavelengths, the LMC is remarkably symmetrical 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 due to differential rotation, therefore transient in nature. On small to medium scales, the combined action of numerous shells and supershells dominate the structures and motions of the HI gas in the LMC. A good correlation is seen between supershells previously identified in Hα (e.g. Meaburn 1980) and HI structures. We compare the results with a new wide-field Hα image.

Type
Part VIII High-Velocity Clouds, Galactic Halo Models, Observations of the LMC
Information
International Astronomical Union Colloquium , Volume 166: The Local Bubble and Beyond , 1997 , pp. 521 - 524
Copyright
Copyright © Springer-Verlag 1998

References

de Vaucouleurs, G. and Freeman, K.C. (1972): Vistas in Astronomy 14, 163 Google Scholar
Kim, S., Staveley-Smith, L., Sault, R.J., Kesteven, M.J., Mcconnell, D.(1997):A&A, to be submittedGoogle Scholar
Luks, T., & Rohlfs, K. (1992): A&A 263, 41 Google Scholar
McGee, R.X., & Milton, J.A. (1966): Aust.J.Phys. 19, 343 Google Scholar
Meaburn, J. (1980): MNRAS 192, 365 Google Scholar
Rohlfs, K. et al.(1984): A&A 137, 343 Google Scholar
Weaver, R., McCray, R., Castor, J., Shapiro, R, Moore, R. (1977): ApJ 218, 377 Google Scholar