2004/01/01 by Masashi Chiba, Arihiro Mizutani · 5 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Debris #Galactic corona #Galactic halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Globular cluster #Halo #Kinematics #Physics #Satellite galaxy #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1071/as04002
published in Publications of the Astronomical Society of Australia 21(2), 237-241 (Cambridge University Press) · 5 pages including 4 figures, to appear in PASA (Refereed contribution to the 5th Galactic Chemodynamics conference held in Swinburne, July 2003)
openalex publication_date 2004/01/01 · arxiv created 2004/02/06 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract 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.