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The Magellanic Stream∗

Published online by Cambridge University Press:  14 August 2015

D. S. Mathewson ,
M. N. Cleary  and
J. D. Murray
D. S. Mathewson
Affiliation:
Mount Stromlo and Siding Spring Observatory, Australian National University, Australia
M. N. Cleary
Affiliation:
Mount Stromlo and Siding Spring Observatory, Australian National University, Australia
J. D. Murray
Affiliation:
Division of Radiophysics, CSIRO, Australia

Abstract

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A southern sky survey of H I in the velocity range — 340 km s−1 to +380 km s−1 has shown that a long filament of H I extends from the Small Magellanic Cloud (SMC) region down to the South Galactic Pole and connects with the long H I filament discovered recently by Wannier and Wrixon (1972) and van Kuilenburg (1972). There is also some evidence that the feature continues on the other side of the Magellanic Clouds and crosses the galactic plane at l = 306°. The whole filament, which follows very closely a great circle over its entire 180° length, is given the name ‘The Magellanic Stream’. It may have been produced by gravitational interaction between the SMC and the Galaxy during a close passage (20 kpc) of the SMC some 5 × 108 yr ago although it is impossible to account for the observed radial velocities along the Stream unless some force other than gravity is invoked to act on the Stream as well.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 58: The Formation and Dynamics of Galaxies , 1974 , pp. 367 - 374
Copyright
Copyright © Reidel 1974 

References

Bok, B. J.: 1966, Ann. Rev. Astron. Astrophys. 4, 95.Google Scholar
Clutton-Brock, M.: 1972, Astrophys. Space Sci. 17, 292.Google Scholar
de Vaucouleurs, G.: 1954, Observatory 74, 23.Google Scholar
Dieter, N. H.: 1965, Astron. J. 70, 552.Google Scholar
Gascoigne, S. C. B. and Lyngå, G.: 1963, Observatory 83, 38.Google Scholar
Hindman, J. V., Kerr, F. J., and McGee, R. X.: 1963, Australian J. Phys. 16, 570.Google Scholar
Hulsbosch, A. N. M. and Raimond, E.: 1966, Bull. Astron. Inst. Neth. 18, 413.Google Scholar
Hulsbosch, A. N. M.: 1972, Studies on High-Velocity Clouds, , Leiden University.Google Scholar
Kerr, F. J. and Sullivan, W. T.: 1969, Astrophys. J. 158, 115.Google Scholar
Mirabel, I. F. and Turner, K. C.: 1973, Astron. Astrophys. 22, 437.Google Scholar
Oort, J. H.: 1970, Astron. Astrophys. 7, 381.Google Scholar
Turner, K. C.: 1968, Annual Report of the Director, Dept. of Terrestrial Magnetism 1967-68, Carnegie Institution of Washington, Washington, D.C., p. 291.Google Scholar
van Kuilenburg, J.: 1972, Astron. Astrophys. 16, 276.Google Scholar
Wannier, P. and Wrixon, G. T.: 1972, Astrophys. J. Letters 173, L119.Google Scholar
Wannier, P., Wrixon, G. T., and Wilson, R. W.: 1972, Astron. Astrophys. 18, 224.Google Scholar