2020/11/30 by Cosimo Bambi, Laura W. Brenneman, Thomas Dauser +14 · 1 citation
Physics and Astronomy · #astro-ph.HE #gr-qc
paper · pdf · doi:10.1007/s11214-021-00841-8
published as Space Sci. Rev. 217, 65 (2021) · 64 pages, 23 figures. Prepared within the ISSI International Team project "Can We Use X-Ray Reflection Spectroscopy For Precision Measurements Of Accreting Black Holes?". v3: refereed version
arxiv created 2021/07/20 · arxiv updated 2021/07/21
Relativistic reflection features are commonly observed in the X-ray spectra of accreting black holes. In the presence of high quality data and with the correct astrophysical model, X-ray reflection spectroscopy can be quite a powerful tool to probe the strong gravity region, study the morphology of the accreting matter, measure black hole spins, and possibly test Einstein's theory of general relativity in the strong field regime. In the last decade, there has been significant progress in the development of the analysis of these features, thanks to more sophisticated astrophysical models and new observational facilities. Here we review the state-of-the-art in relativistic reflection modeling, listing assumptions and simplifications that may affect, at some level, the final measurements and may be investigated better in the future. We review black hole spin measurements and the most recent efforts to use X-ray reflection spectroscopy for testing fundamental physics.