Testing loop quantum gravity through EHT observations of M87* and Sgr A* using rotating holonomy-corrected black holes
Abstract
The Event Horizon Telescope (EHT) has provided a new tool for testing the strong-field regime of gravity by imaging the shadows of M87* and Sgr A*. These observations provide the first real opportunity to test whether quantum gravity, specifically loop quantum gravity, leaves observable imprints on spacetime. We use the EHT observations of M87* and Sgr A* to examine the observational signs of rotating holonomy--corrected black holes (RHCBHs). We discover that, in comparison to the typical Kerr black hole, the quantum correction parameter b increases the size of the black hole shadow. As the deviation parameter b increases in RHCBH, the prograde photon orbits shift outward, indicating a weaker effective gravitational field near the central region. We find that photon rings continue to exist in the parameter range bE ≤ b ≤ bp, due to the presence of unstable circular photon orbits. We apply the Kumar--Ghosh method based on the shadow observables: the shadow area A and the oblateness D that together allow a unique determination of the spin parameter a and the quantum correction parameter b. At θo=17\textdegree~, the angular diameter bound of M87* yields b ≤ 0.1319 M at a = 0 and b ≤ 0.421 M at a = 0.784 M, while at θo=50\textdegree~, the angular diameter bound of Sgr A* yields b ≤ 0.5764 M at a = 0 and b ≤ 0.7482 M at a = 0.6253 M the Sgr~A*. Our results show that nonzero values of the holonomy correction parameter are consistent with current EHT data, indicating that RHCBHs provide viable alternatives to the classical Kerr geometry in the strong-gravity regime and are strong astrophysical black hole candidates.
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BibTeX
@misc{ali2026testing,
title = {{Testing loop quantum gravity through EHT observations of M87* and Sgr A* using rotating holonomy-corrected black holes}},
author = {Heena Ali and Sushant G. Ghosh},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2605.28871},
eprint = {2605.28871},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2605.28871},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Testing loop quantum gravity through EHT observations of M87* and Sgr A* using rotating holonomy-corrected black holes
AU - Heena Ali
AU - Sushant G. Ghosh
PY - 2026
DA - 2026/10/08
PB - arXiv
DO - 10.48550/arxiv.2605.28871
UR - https://arxiv.org/abs/2605.28871
AB - The Event Horizon Telescope (EHT) has provided a new tool for testing the strong-field regime of gravity by imaging the shadows of M87* and Sgr A*. These observations provide the first real opportunity to test whether quantum gravity, specifically loop quantum gravity, leaves observable imprints on spacetime. We use the EHT observations of M87* and Sgr A* to examine the observational signs of rotating holonomy--corrected black holes (RHCBHs). We discover that, in comparison to the typical Kerr black hole, the quantum correction parameter b increases the size of the black hole shadow. As the deviation parameter b increases in RHCBH, the prograde photon orbits shift outward, indicating a weaker effective gravitational field near the central region. We find that photon rings continue to exist in the parameter range b_E ≤ b ≤ b_p, due to the presence of unstable circular photon orbits. We apply the Kumar--Ghosh method based on the shadow observables: the shadow area A and the oblateness D that together allow a unique determination of the spin parameter a and the quantum correction parameter b. At θ_o=17\textdegree~, the angular diameter bound of M87^* yields b ≤ 0.1319 M at a = 0 and b ≤ 0.421 M at a = 0.784 M, while at θ_o=50\textdegree~, the angular diameter bound of Sgr A^* yields b ≤ 0.5764 M at a = 0 and b ≤ 0.7482 M at a = 0.6253 M the Sgr~A^*. Our results show that nonzero values of the holonomy correction parameter are consistent with current EHT data, indicating that RHCBHs provide viable alternatives to the classical Kerr geometry in the strong-gravity regime and are strong astrophysical black hole candidates.
ER -