2018/07/31 by Yerong Xu, Sourabh Nampalliwar, Askar B. Abdikamalov +6 · 1 citation
Physics and Astronomy · #Accretion (finance) #Alpha (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Einstein #General relativity #Gravitation #Kerr metric #Mathematical physics #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Relativity and Gravitational Theory #Rotating black hole #Schwarzschild metric #Spacetime #Statistics #Strong gravity #astro-ph.HE #gr-qc
paper · pdf · doi:10.3847/1538-4357/aadb9d
published as Astrophys.J. 865: 134 (2018) · 6 pages, 3 figures. v2: refereed version
arxiv created 2018/10/01 · openalex publication_date 2018/10/01 · arxiv updated 2018/10/02 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
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.