Testing the Galactic Centre potential with S-stars

TL;DR

This paper evaluates the RAR dark matter core-halo model against observational data of stars near the Galactic Centre, finding it inconsistent with the elliptical star trajectories observed, unlike the conventional black hole model.

Contribution

The study critically tests the RAR dark matter model's predictions against star trajectory data, highlighting its inconsistencies with observations.

Findings

RAR model predicts star orbits with centers at the Galactic Center, conflicting with observations.

Orbital periods in the RAR model are independent of semi-major axes, unlike real star trajectories.

Conventional black hole models better fit the observed elliptical star orbits.

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.