Abstract
Abstract
The Event Horizon Telescope (EHT) collaboration’s image of the compact object at the Galactic center is the first direct evidence of the supermassive black hole (BH) Sgr A*. The shadow of Sgr A* has an angular diameter d
sh = 48.7 ± 7 μas with fractional deviation from the Schwarzschild BH shadow diameter
δ
=
−
0.08
−
0.09
+
0.09
,
−
0.04
−
0.10
+
0.09
(for the VLTI and Keck mass-to-distance ratios). Sgr A*'s shadow size is within 10% of Kerr predictions, equipping us with yet another tool to analyze gravity in the strong-field regime, including testing loop quantum gravity (LQG). We use Sgr A*'s shadow to constrain the metrics of two well-motivated LQG-inspired rotating BH (LIRBH) models characterized by an additional deviation parameter L
q
, which recover the Kerr spacetime in the absence of quantum effects (L
q
→ 0). When increasing the quantum effects through L
q
, the shadow size increases monotonically, while the shape gets more distorted, allowing us to constrain the fundamental parameter L
q
. We use the astrophysical observables shadow area A and oblateness D to estimate the BH parameters. It may be useful in extracting additional information about LIRBHs. While the EHT observational results completely rule out the wormhole region in LIRBH-2, a substantial parameter region of the generic BHs in both models agrees with the EHT results. We find that the upper bounds on L
q
obtained from the shadow of Sgr A*—L
q
≲ 0.0423 and L
q
≲ 0.0821 for the two LIRBHs, respectively—are more stringent than those obtained from the EHT image of M87*.
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
25 articles.
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