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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

Observational signatures of Kerr black hole lensing

  • Thomas P Kling1
  • Lia Troy2
  • Shannon Harding3
  • Timothy O’Leary1
  1. 1Department of Physics, Photonics and Optical Engineering, Bridgewater State University , Bridgewater, MA 02325 ,
  2. 2Department of Mathematics, University of Chicago , Chicago, IL 60637 ,
  3. 3Department of Physics and Applied Physics, University of Massachusetts-Lowell , Lowell, MA 01814 ,
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Abstract

Gravitational lensing by rotating black holes is modelled, and the null geodesic equations in the strong field regime are integrated numerically. Observational signatures of the black hole spin parameter are identified by comparing image locations and shapes of extended sources at different a values. For the black hole at the centre of our Galaxy, angular resolutions of the order of hundreds of µas are needed to distinguish between the true source position and gravitationally lensed image position. Angular resolution below 1 µas is needed to determine the spin parameter of the Galactic black hole using gravitational lensing.

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Cite

BibTeXRIS
BibTeX
@article{kling2026observational,
  title = {{Observational signatures of Kerr black hole lensing}},
  author = {Thomas P Kling and Lia Troy and Shannon Harding and Timothy O’Leary},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = oct,
  doi = {10.1093/mnras/stag1890},
  url = {https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1890/8869230},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Observational signatures of Kerr black hole lensing
AU  - Thomas P Kling
AU  - Lia Troy
AU  - Shannon Harding
AU  - Timothy O’Leary
PY  - 2026
DA  - 2026/10/06
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag1890
UR  - https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1890/8869230
AB  - Gravitational lensing by rotating black holes is modelled, and the null geodesic equations in the strong field regime are integrated numerically. Observational signatures of the black hole spin parameter are identified by comparing image locations and shapes of extended sources at different a values. For the black hole at the centre of our Galaxy, angular resolutions of the order of hundreds of µas are needed to distinguish between the true source position and gravitationally lensed image position. Angular resolution below 1 µas is needed to determine the spin parameter of the Galactic black hole using gravitational lensing.
SN  - 0035-8711
SN  - 1365-2966
ER  -