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The Andromeda Stream

Published online by Cambridge University Press:  05 March 2013

G. F. Lewis ,
R. A. Ibata ,
S. C. Chapman ,
A. M. N. Ferguson ,
A. W. McConnachie ,
M. J. Irwin  and
N. Tanvir
G. F. Lewis*
Affiliation:
School of Physics, University of Sydney, Sydney NSW 2006, Australia
R. A. Ibata
Affiliation:
Observatoire de Strasbourg, 67000 Strasbourg, France
S. C. Chapman
Affiliation:
California Institute of Technology, Pasadena, CA 91125, USA
A. M. N. Ferguson
Affiliation:
Max-Planck-Institut für Astrophysik, 85741 Garching, Germany
A. W. McConnachie
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
M. J. Irwin
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
N. Tanvir
Affiliation:
Physical Sciences, University of Hertfordshire, Hatfield AL10 9AB, UK
*
7E-mail: gfl@physics.usyd.edu.au
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Abstract

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The existence of a stream of tidally stripped stars from the Sagittarius dwarf galaxy demonstrates that the Milky Way is still in the process of accreting mass. More recently, an extensive stream of stars has been uncovered in the halo of the Andromeda galaxy (M31), revealing that it too is cannibalising a small companion. This paper reports the recent observations of this stream, determining its spatial and kinematic properties, and tracing its three-dimensional structure, as well as describing future observations and what we may learn about the Andromeda galaxy from this giant tidal stream.

Keywords

Galaxy: kinematics and dynamicsmethods: N-body simulations
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 21 , Issue 2: The Fifth Workshop on Galactic Chemodynamics , 2004 , pp. 203 - 206
Copyright
Copyright © Astronomical Society of Australia 2004

References

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