Testing the No-hair Theorem with Observations in the Electromagnetic Spectrum. II. Black Hole Images

• Published in: The Astrophysical journal Vol. 718; no. 1; pp. 446 - 454
• Main Authors: Johannsen, Tim, Psaltis, Dimitrios
• Format: Journal Article
• Language: English
• Published: Bristol IOP Publishing 20.07.2010; IOP
• Subjects: ACCRETION DISKS; Astronomy; ASTROPHYSICS; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASYMMETRY; BLACK HOLES; Earth, ocean, space; Exact sciences and technology; FLOW MODELS; GALAXIES; GRAVITATION; INCLINATION; MATHEMATICAL MODELS; PHYSICS; QUADRUPOLE MOMENTS; SPACE-TIME; stars: individual (Sgr A; Gravitation; Galaxies; black hole physics; Black holes; accretion, accretion disks; gravitational lensing: strong; Gravitational lensing; Cosmology; ); Accretion disks; Galaxy: center
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/718/1/446

According to the no-hair theorem, all astrophysical black holes are fully described by their masses and spins. This theorem can be tested observationally by measuring (at least) three different multipole moments of the spacetimes of black holes. In this paper, we analyze images of black holes within a framework that allows us to calculate observables in the electromagnetic spectrum as a function of the mass, spin, and, independently, the quadrupole moment of a black hole. We show that a deviation of the quadrupole moment from the expected Kerr value leads to images of black holes that are either prolate or oblate depending on the sign and magnitude of the deviation. In addition, there is a ring-like structure around the black hole shadow with a diameter of {approx}10 black hole masses that is substantially brighter than the image of the underlying accretion flow and that is independent of the astrophysical details of accretion flow models. We show that the shape of this ring depends directly on the mass, spin, and quadrupole moment of the black hole and can be used for an independent measurement of all three parameters. In particular, we demonstrate that this ring is highly circular for a Kerr black hole with a spin a {approx}< 0.9 M, independent of the observer's inclination, but becomes elliptical and asymmetric if the no-hair theorem is violated. Near-future very long baseline interferometric observations of Sgr A* will image this ring and may allow for an observational test of the no-hair theorem.