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.

相对论反射特征通常在吸积黑洞的 X 射线光谱中观察到。在有高质量数据和正确的天体物理模型的情况下，X 射线反射光谱可以成为探测强引力区、研究吸积物质的形态、测量黑洞自旋以及可能检验爱因斯坦理论的有力工具强场域中的广义相对论。在过去十年中，由于更复杂的天体物理模型和新的观测设施，这些特征的分析发展取得了重大进展。在这里，我们回顾了相对论反射建模的最新技术，列出了可能在某种程度上影响最终测量并在未来进行更好研究的假设和简化。