Horizon-scale tests of gravity theories and fundamental physics from the Event Horizon Telescope image of Sagittarius A$^*$

Abstract

Horizon-scale images of black holes (BHs) and their shadows have opened an unprecedented window onto tests of gravity and fundamental physics in the strong-field regime, allowing us to test whether the Kerr metric provides a good description of the space-time in the vicinity of the event horizons of supermassive BHs. We consider a wide range of well-motivated deviations from classical General Relativity solutions, and constrain them using the Event Horizon Telescope (EHT) observations of Sagittarius A * (SgrA * ), connecting the size of the bright ring of emission to that of the underlying BH shadow and exploiting high-precision measurements of SgrA * 's mass-to-distance ratio. The scenarios we consider, and whose fundamental parameters we constrain, include various regular BH models, string-and non-linear electrodynamics-inspired space-times, scalar field-driven violations of the no-hair theorem, alternative theories of gravity, new ingredients such as the generalized uncertainty principle and Barrow entropy, and BH mimickers including examples of wormholes and naked singularities. We demonstrate that SgrA * 's image places particularly stringent constraints on models predicting a shadow size which is larger than that of a Schwarzschild BH of a given mass: for instance, in the case of Barrow entropy we derive constraints which are significantly tighter than the cosmological ones. Our results are among the first tests of fundamental physics from the shadow of SgrA * and, while the latter appears to be in excellent agreement with the predictions of General Relativity, we have shown that various well-motivated alternative scenarios (including BH mimickers) are far from being ruled out at present.

Probing the Lorentz Symmetry Violation Using the First Image of Sagittarius A*: Constraints on Standard-Model Extension Coefficients

“…In other words, if the uncertainties reported by the Keck and VLTI measurements on δ were merely limited to negative values, then the metric in question would certainly be ruled out. To have unified upper bounds from Keck and VLTI measurements for the LVCs, we take their average (δ = −0.06 ± 0.063 [71]) and compare the predicted theoretical fractional deviation from the Schwarzschild at hand with it. In Fig.…”

“…In Ref. [71] one can find a list of reasons for evaluating the theories via Sgr A*'s shadow, in addition to its counterpart M87*. As a result, upon the recent release of updated and new information on the near-horizon image of Sgr A*, we are faced a spectrum of observational evaluations of different metrics [71]- [83].…”

Sign Switching Dark Energy from a Running Barrow Entropy

“…( 2), in line with most literature. Cosmological and black hole shadow constraints (assuming a fixed δ) has put an upper bound on δ, which is typically δ O(10 −3 ) or O(10 −4 ) [4][5][6][7][8][9].…”

How Barrow Entropy Modifies Gravity: With Comments on Tsallis Entropy

“…Depending on the number of spheres added at each iteration and the scaling factor, the fractal dimension of the resulting sphereflake would be different. Since it is often much more convenient to have an explicit metric to work with, a spherically symmetric black hole metric in the usual coordinates {t, r, θ, φ} that incorporates such an entropy correction was introduced and analyzed in the literature [2,3]. However, this immediately raised a question: in what sense does such a metric describe the underlying geometry?…”