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A Study of the Strong Gravity Region of the Black Hole in GS 1354–645

Yerong XuCenter for Field Theory and Particle Physics and Department of Physics, Fudan University, 200438 Shanghai, People's Republic of China; [email protected]Sourabh NampalliwarTheoretical Astrophysics, Eberhard-Karls Universität Tübingen, D-72076 Tübingen, GermanyAskar B. AbdikamalovCenter for Field Theory and Particle Physics and Department of Physics, Fudan University, 200438 Shanghai, People's Republic of China; [email protected]Dimitry AyzenbergCenter for Field Theory and Particle Physics and Department of Physics, Fudan University, 200438 Shanghai, People's Republic of China; [email protected]Cosimo BambiCenter for Field Theory and Particle Physics and Department of Physics, Fudan University, 200438 Shanghai, People's Republic of China; [email protected]Thomas DauserRemeis Observatory & ECAP, Universität Erlangen-Nürnberg, D-96049 Bamberg, GermanyJavier A. GarcíaCahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USAJiachen JiangInstitute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UK

2018en

ABI

Annotatsiya

Abstract It is thought that the spacetime metric around astrophysical black holes is well described by the Kerr solution of Einstein’s gravity. However, robust observational evidence of the Kerr nature of these objects is still lacking. Here we fit the X-ray spectrum of the stellar-mass black hole in GS 1354–645 with a disk reflection model beyond Einstein’s gravity in order test the Kerr black hole hypothesis. We consider the Johannsen metric with the deformation parameters α 13 and α 22 . The Kerr metric is recovered for . For α 22 = 0, our measurements of the black hole spin and of the deformation parameter α 13 are and −0.34 < α 13 < 0.16, respectively. For α 13 = 0, we find a * > 0.975 and −0.09 < α 22 < 0.42. All the reported uncertainties are at 99% of confidence level for two relevant parameters.

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DOI: 10.3847/1538-4357/aadb9d

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