Kinematic Structure of the Galactic Center S-cluster

Abstract

We present a detailed analysis of the kinematics of 112 stars that mostly comprise the high velocity S-cluster and orbit the super massive black hole SgrA* at the center of the Milky Way. For 39 of them orbital elements are known, for the remainder we know proper motions. The distribution of inclinations, and proper motion flight directions deviate significantly from a uniform distribution which one expects if the orientation of the orbits are random. Across the central arcseconds the S-cluster stars are arranged in two almost edge on disks that are located at a position angle approximately +-45 o with respect to the Galactic plane. The angular momentum vectors for stars in each disk point in both directions, i.e. the stars in a given disk rotate in opposite ways. The poles of this structure are located only about 25 o from the line of sight. This structure may be the result of a resonance process that started with the formation of the young B-dwarf stars in the cluster about 6 Myr ago. Alternatively, it indicated the presence of a disturber at a distance from the center comparable to the distance of the compact stellar association IRS13.

published in Astrophysical Journal 23 pages, 6 tabels, 16 figures, ENHANCED GRAPHICS in ApJ in fullorbits.gif circularized.gif normalized.gif

References in corpus (17)

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• The Second Galactic Center Black Hole?; A Possible Detection of Ionized Gas Orbiting around an IMBH embedded in the Galactic Center IRS13E complex
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Cited by in corpus (4)

• S62 and S4711: Indications of a population of faint fast moving stars inside the S2 orbit -- S4711 on a 7.6 year orbit around Sgr~A*
• An upper limit on the spin of SgrA${}^{\ast }$ based on stellar orbits in its vicinity
• First observed interaction of the circumstellar envelope of an S-star with the environment of Sgr A*
• Observation of the apoapsis of S62 in 2019 with NIRC2 and SINFONI