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Tidal disruption of the Magellanic Clouds by the Milky Way

Author

Listed:
  • M. E. Putman

    (Mount Stromlo & Siding Spring Observatories, Australian National University)

  • B. K. Gibson

    (Mount Stromlo & Siding Spring Observatories, Australian National University)

  • L. Staveley-Smith

    (Australia Telescope National Facility, CSIRO)

  • G. Banks

    (University of Wales, Cardiff)

  • D. G. Barnes

    (Australia Telescope National Facility, CSIRO)

  • R. Bhatal

    (University of Western Sydney Macarthur)

  • M. J. Disney

    (University of Wales, Cardiff)

  • R. D. Ekers

    (Australia Telescope National Facility, CSIRO)

  • K. C. Freeman

    (Mount Stromlo & Siding Spring Observatories, Australian National University)

  • R. F. Haynes

    (Australia Telescope National Facility, CSIRO)

  • P. Henning

    (University of New Mexico)

  • H. Jerjen

    (Mount Stromlo & Siding Spring Observatories, Australian National University)

  • V. Kilborn

    (University of Melbourne, School of Physics)

  • B. Koribalski

    (Australia Telescope National Facility, CSIRO)

  • P. Knezek

    (The Johns Hopkins University)

  • D. F. Malin

    (Anglo-Australian Observatory)

  • J. R. Mould

    (Mount Stromlo & Siding Spring Observatories, Australian National University)

  • T. Oosterloo

    (Istituto di Fisica Cosmica)

  • R. M. Price

    (Australia Telescope National Facility, CSIRO)

  • S. D. Ryder

    (Joint Astronomy Center)

  • E. M. Sadler

    (University of Sydney, School of Physics)

  • I. Stewart

    (Australia Telescope National Facility, CSIRO)

  • F. Stootman

    (University of Western Sydney Macarthur)

  • R. A. Vaile

    (University of Western Sydney Macarthur)

  • R. L. Webster

    (University of Melbourne, School of Physics)

  • A. E. Wright

    (Australia Telescope National Facility, CSIRO)

Abstract

Interactions between galaxies are common, and influence physical properties such as the global morphology and star-formation rate1 (Hubble type). Galaxies can interact in many different ways: they can merge together; they can pass through each other, with gas being stripped from the smaller of the two and compressed in the larger; and they can interact gravitationally2 (including, for example, tides in clusters). The relative importance of these mechanisms is often not clear, as the strength of each depends on poorly known parameters such as the density, extent and nature of the dark-matter haloes that surround galaxies3. A nearby example of a galaxy interaction where the mechanism is controversial is that between our Galaxy and two of its neighbours, the Magellanic Clouds. Here we present the results of an atomic-hydrogen survey that help to elucidate this mechanism. Our data reveal a new stream of gas that lies in the opposite direction to the trailing Magellanic Stream and leads the motion of the Clouds. The existence of both leading and trailing streams supports a gravitational interaction whereby the streams are torn from the bodies of the Magellanic Clouds by tidal forces.

Suggested Citation

  • M. E. Putman & B. K. Gibson & L. Staveley-Smith & G. Banks & D. G. Barnes & R. Bhatal & M. J. Disney & R. D. Ekers & K. C. Freeman & R. F. Haynes & P. Henning & H. Jerjen & V. Kilborn & B. Koribalski , 1998. "Tidal disruption of the Magellanic Clouds by the Milky Way," Nature, Nature, vol. 394(6695), pages 752-754, August.
    • Handle: RePEc:nat:nature:v:394:y:1998:i:6695:d:10.1038_29466
    DOI: 10.1038/29466
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