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On the Kinematics of Tidal Debris from Omega Cen's Progenitor Galaxy

Published online by Cambridge University Press:  05 March 2013

Masashi Chiba  and
Arihiro Mizutani
Masashi Chiba*
Affiliation:
Astronomical Institute, Tohoku University, Sendai 980-8578, Japan
Arihiro Mizutani
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
*
3E-mail: [email protected]
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Abstract

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The kinematic properties of tidal debris from an orbiting Galactic satellite is presented, on the assumption that its central part once contained the most massive Galactic globular cluster, ω Cen. We simulate dynamical evolution of a satellite galaxy that follows the present-day and likely past orbits of ω Cen, and analyse the kinematic nature of their tidal debris and randomly generated Galactic stars comprising spheroidal halo and flat disk components. It is found that the debris stars show a retrograde rotation at ∼–100 km s–1, which may accord with a recently discovered stellar stream at a radial velocity of ∼300 km s–1 towards the Galactic longitude of ∼270°. These stars also contribute, only in part, to a reported retrograde motion of the outer halo in the north Galactic pole direction, without significantly modifying local halo kinematics near the Sun. The prospects for future debris searches and the implications for the early evolution of the Galaxy are briefly presented.

Keywords

Galaxy: formationglobular clusters: individual (ω Cen)stars: kinematicsstars: Population II
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 21 , Issue 2: The Fifth Workshop on Galactic Chemodynamics , 2004 , pp. 237 - 241
Copyright
Copyright © Astronomical Society of Australia 2004

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