Testing the Galactic Centre potential with S-stars

Abstract

Two groups of astronomers used the large telescopes Keck and VLT for decades to observe trajectories of bright stars near the Galactic Centre. Based on results of their observations the astronomers concluded that trajectories of the stars are roughly elliptical and foci of the orbits are approximately coincide with the Galactic Centre position. In a last few years a self-gravitating dark matter core--halo distribution was suggested by Ruffini, Arguelles, Rueda (RAR) and this model was actively used in consequent studies. In particular, recently it has been claimed that the RAR-model provides a better fit of trajectories of bright stars in comparison to the conventional model with a supermassive black hole. The dark matter distribution with a dense core having a constant density as it was suggested in the RAR-model leaves trajectories of stars elliptical like in Kepler's two-body problem. However, in this case not the foci of the ellipses coincide with the Galactic Center but their centers while the orbital periods do not depend on semi-major axes. These properties are not consistent with the observational data for trajectories of bright stars.

4 pages, a number of corrections were done in accordance with a version accepted in MNRAS Letters

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Cited by in corpus (9)

• Constraints on self-dual black hole in loop quantum gravity with S0-2 star in the Galactic Center
• Estimating the Parameters of Extended Gravity Theories with the Schwarzschild Precession of S2 Star
• Constraints on Yukawa gravity parameters from observations of bright stars
• The Galactic Center as a laboratory for theories of gravity and dark matter
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• Shadows near supermassive black holes: from a theoretical concept to GR test
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• Unscreening of f(R) gravity near the galactic center black hole: Testability through pericenter shift below S0-2's orbit
• Neural Network Analysis of S2-Star Dynamics: Extended mass