期刊
PHYSICAL REVIEW LETTERS
卷 116, 期 3, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevLett.116.031101
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资金
- Perimeter Institute for Theoretical Physics
- Natural Sciences and Engineering Research Council of Canada
- Government of Canada through Industry Canada
- Province of Ontario through the Ministry of Research and Innovation
- National Science Foundation
- Gordon and Betty Moore Foundation [GBMF-3561]
- Smithsonian Institution
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1126433, 1310896] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1337663] Funding Source: National Science Foundation
In general relativity, the angular radius of the shadow of a black hole is primarily determined by its mass-to-distance ratio and depends only weakly on its spin and inclination. If general relativity is violated, however, the shadow size may also depend strongly on parametric deviations from the Kerr metric. Based on a reconstructed image of Sagittarius A* (Sgr A*) from a simulated one-day observing run of a seven-station Event Horizon Telescope (EHT) array, we employ a Markov chain Monte Carlo algorithm to demonstrate that such an observation can measure the angular radius of the shadow of Sgr A* with an uncertainty of similar to 1.5 mu as (6%). We show that existing mass and distance measurements can be improved significantly when combined with upcoming EHT measurements of the shadow size and that tight constraints on potential deviations from the Kerr metric can be obtained.
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