An Upper Limit on the Charge of the Black Hole Sgr A* from EHT Observations

Abstract

The Event Horizon Telescope (EHT) recently released an image of the supermassive black hole Sgr A* showing an angular shadow diameter $d_{sh}=48.7\pm 7\mu$as and Schwarzschild shadow deviation $\delta =-0.08_{-0.09}^{+0.09}\text{(VLTI)},-0.04_{-0.10}^{+0.09}\text{(Keck)}$ using a black hole mass $M=4.0_{-0.6}^{+1.1}\times 10^6{M}_{\odot }$. The EHT image of Sgr A* is consistent with a Kerr black hole's expected appearance, and the results directly prove the existence of a supermassive black hole at the center of the Milky Way. Here, we use the EHT observational results for Sgr A* to investigate the constraints on its charge with the aid of Kerr-like black holes, paying attention to three leading rotating models, namely Kerr--Newman, Horndeski, and hairy black holes. Modeling the supermassive black hole Sgr A* as these Kerr-like black holes, we observe that the EHT results of Sgr A* place more strict upper limits on the parameter space of Kerr--Newman and Horndeski black holes than those placed by the EHT results for M87*. A systematic bias analysis reveals that, observational results of future EHT experiments place more precise limits on the charge of black hole Sgr A*. Thus, the Kerr-like black holes and Kerr black holes are indiscernible in a substantial region of the EHT-constrained parameter space; the claim is substantiated by our bias analysis.

12 pages, 8 figures, 1 table. Matched to the published version

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