Observability of the innermost stable circular orbit in a near-extremal Kerr black hole

Abstract

We consider the escape probability of a photon emitted from the innermost stable circular orbit (ISCO) of a rapidly rotating black hole. As an isotropically emitting light source on a circular orbit reduces its orbital radius, the escape probability of a photon emitted from it decreases monotonically. The escape probability evaluated at the ISCO also decreases monotonically as the black hole spin increases. When the dimensionless Kerr parameter $a$ is at the Thorne limit $a=0.998$, the escape probability from the ISCO is $58.8\%$. In the extremal case $a=1$, even if the orbital radius of the light source is arbitrarily close to the ISCO radius, which coincides with the horizon radius, the escape probability remains at $54.6\%$. We also show that such photons that have escaped from the vicinity of the horizon reach infinity with sufficient energy to be potentially observed because Doppler blueshift due to relativistic beaming can overcome the gravitational redshift. Our findings indicate that signs of the near-horizon physics of a rapidly rotating black hole will be detectable on the edge of its shadow.

arXiv comment17 pages, 6 figures; v2: published version in PRD

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• Complete classification of photon escape in the Kerr black hole spacetime
• Escape probability of particle from Kerr-Sen black hole
• Photon emission from inside the innermost stable circular orbit
• Photon emissions from near-horizon extremal and near-extremal Kerr equatorial emitters
• High spin expansion for null geodesics
• Observability of Zero-angular-momentum Sources Near Kerr Black Holes
• Photon escape in the extremal Kerr black hole spacetime
• Signatures of particle collisions near extreme black holes
• Can the Near-Horizon Black Hole Memory be detected through Binary Inspirals?