2008/10/20 by Sascha Trippe, S. Trippe, S. Gillessen +12
Medicine · Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Cluster (spacecraft) #Computer science #Galactic Center #Galaxy #Kinematics #Medicine #Milky Way #Physics #Population #Star cluster #Stars #Stellar dynamics #Stellar kinematics #Stellar, planetary, and galactic studies #Supermassive black hole #astro-ph
paper · pdf · doi:10.1051/0004-6361:200810191
23 pages, 20 figures, accepted by A&A. This versions corresponds to the one to be printed. Some language editing done, one figure in Sect. 5.6 replaced by a table, a few bugs and typos corrected
arxiv created 2008/10/20 · openalex publication_date 2008/10/27 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Aims. We aim at a detailed description of the kinematic properties of the old, (several Gyrs) late-type CO-absorption star population among the Galactic centre (GC) cluster stars. This cluster is composed of a central supermassive black hole (Sgr A*) and a self-gravitating system of stars. Understanding its kinematics thus offers the opportunity to understand the dynamical interaction between a central point mass and the surrounding stars in general, especially in view of understanding other galactic nuclei.