Weighing of the Dark Matter at the Center of the Galaxy

Abstract

A promising method for measuring the total mass of the dark matter near a supermassive black hole at the center of the Galaxy based on observations of nonrelativistic precession of the orbits of fast S0 stars together with constraints on the annihilation signal from the dark matter particles has been discussed. An analytical expression for the precession angle has been obtained under the assumption of a power-law profile of the dark matter density. In the near future, modern telescopes will be able to measure the precession of the orbits of S0 stars or to obtain a strong bound on it. The mass of the dark matter necessary for the explanation of the observed excess of gamma radiation owing to the annihilation of the dark matter particles has been calculated with allowance for the Sommerfeld effect.

5 pages, 3 figures

References in corpus (5)

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• Galactic Center Gamma-Ray Excess from Dark Matter Annihilation: Is There A Black Hole Spike?
• Constraining the range of Yukawa gravity interaction from S2 star orbits
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Cited by in corpus (21)

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• To see invisible: image of the event horizon within the black hole shadow
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• Influence of bulk mass distribution on orbital precession of S2 star in Yukawa gravity
• Estimating the parameters of Hybrid Palatini gravity model with the Schwarzschild precession of S2, S38 and S55 stars: case of bulk mass distribution
• Tests of gravity theories with Galactic Center observations
• Null and Timelike Geodesics Near the Throats of Phantom Scalar Field Wormholes
• Constraints on alternative theories of gravity with observations of the Galactic Center
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• Crossing the dark matter soliton core: a possible reversed orbital precession
• Generalized Einstein-Rosen bridge inside black holes
• Visible shapes of black holes M87* and SgrA*