The image of a supermassive black hole surrounded by an optically-thin, radiatively-inefficient accretion flow, like that observed with the Event Horizon Telescope, is characterized by a bright ring
of emission surrounding the black-hole shadow. In the Kerr spacetime this bright ring, when narrow,
closely traces the boundary of the shadow and can, with appropriate calibration, serve as its proxy.
The present paper expands the validity of this statement by considering two particular spacetime geometries: a solution to the field equations of a modified gravity theory and another that parametrically
deviates from Kerr but recovers the Kerr spacetime when its deviation parameters vanish. A covariant,
axisymmetric analytic model of the accretion flow based on conservation laws and spanning a broad
range of plasma conditions is utilized to calculate synthetic non-Kerr black-hole images, which are
then analysed and characterized. We find that in all spacetimes: (i) it is the gravitationally-lensed
unstable photon orbit that plays the critical role in establishing the diameter of the rings observed
in black-hole images, not the event horizon or the innermost stable circular orbit, (ii) bright rings in
these images scale in size with, and encompass, the boundaries of the black-hole shadows, even when
deviating significantly from Kerr, and (iii) uncertainties in the physical properties of the accreting
plasma introduce subdominant corrections to the relation between the diameter of the image and the
diameter of the black-hole shadow. These results provide theoretical justification for using black-hole
images to probe and test the spacetimes of supermassive black holes.
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First Sagittarius A* Event Horizon Telescope Results. VI. Testing the Black Hole Metric
Abstract Astrophysical black holes are expected to be described by the Kerr metric. This is the only stationary, vacuum, axisymmetric metric, without electromagnetic charge, that satisfies Einstein’s equations and does not have pathologies outside of the event horizon. We present new constraints on potential deviations from the Kerr prediction based on 2017 EHT observations of Sagittarius A* (Sgr A*). We calibrate the relationship between the geometrically defined black hole shadow and the observed size of the ring-like images using a library that includes both Kerr and non-Kerr simulations. We use the exquisite prior constraints on the mass-to-distance ratio for Sgr A* to show that the observed image size is within ∼10% of the Kerr predictions. We use these bounds to constrain metrics that are parametrically different from Kerr, as well as the charges of several known spacetimes. To consider alternatives to the presence of an event horizon, we explore the possibility that Sgr A* is a compact object with a surface that either absorbs and thermally reemits incident radiation or partially reflects it. Using the observed image size and the broadband spectrum of Sgr A*, we conclude that a thermal surface can be ruled out and a fully reflective one is unlikely. We compare our results to the broader landscape of gravitational tests. Together with the bounds found for stellar-mass black holes and the M87 black hole, our observations provide further support that the external spacetimes of all black holes are described by the Kerr metric, independent of their mass.
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- NSF-PAR ID:
- 10330546
- Author(s) / Creator(s):
- ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; more »
- Date Published:
- Journal Name:
- The Astrophysical Journal Letters
- Volume:
- 930
- Issue:
- 2
- ISSN:
- 2041-8205
- Page Range / eLocation ID:
- L17
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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- Free Publicly Accessible Full Text
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Accepted Manuscript1.0
- Journal Article:
- https://doi.org/10.3847/2041-8213/ac6756
