通过X射线反射光谱测量黑洞自旋：质量标准与学界建议
Black-Hole Spin Measurements from X-ray Reflection Spectroscopy: Quality Criteria and Community Recommendations
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中文总结 AI 辅助
基于X射线反射光谱测量黑洞自旋存在系统误差，本文基于2025年研讨会讨论，提出实用框架，依可探测性、唯一性、稳健性原则转化为评估标准等，目标是建立可靠黑洞自旋测量的可重复路径。
中文摘要 AI 辅助
X射线反射光谱是测量吸积黑洞无量纲自旋最强大的电磁方法之一，已用于约束X射线双星中恒星质量黑洞及活动星系核中超大质量黑洞的自旋，对当前和未来X射线天文台的科学目标至关重要。但该技术存在观测和建模系统误差，包括连续谱-反射简并等。基于2025年维克森林研讨会讨论，提出评估已发表基于反射的自旋测量是否可靠、临时或无法根据现有信息评估的实用框架，该框架基于可探测性、唯一性和稳健性三个原则，并转化为评估标准、质量分类方案和报告清单，目标是为X射线天文学的高通量、高分辨率时代建立可靠黑洞自旋测量的可重复路径。
英文摘要
X-ray reflection spectroscopy provides one of the most powerful electromagnetic methods for measuring the dimensionless spin of accreting black holes. It has yielded spin constraints for stellar-mass black holes in X-ray binaries and supermassive black holes in active galactic nuclei, and is central to the science goals of current and future X-ray observatories. However, the technique is subject to observational and modeling systematics, including continuum-reflection degeneracy, limited spectral coverage, unresolved distant reflection or absorption, detector effects, source variability, accretion-state dependence, and assumptions inherent to reflection models. Motivated by discussions at the 2025 Wake Forest workshop *Recent Progress on Black Hole Spin Measurements Across the Electromagnetic and Gravitational Spectra*, we propose a practical framework for evaluating whether published reflection-based spin measurements should be considered robust, provisional, or not assessable from the available information. The framework is built on three principles: **detectability**, requiring an unambiguous relativistic reflection signal; **uniqueness**, requiring that the relativistic component be distinguishable from the continuum, distant reflection, absorption, and instrumental effects; and **robustness**, requiring that the inferred spin remain stable against reasonable changes in model assumptions, data selection, and accretion-state treatment. We translate these principles into assessment criteria, a quality-classification scheme, and a reporting checklist for future studies. Calibration of these criteria through dedicated simulations is outlined here and deferred to a companion paper. Our goal is to establish a reproducible path toward a community-maintained compilation of reliable black hole spin measurements for the high-throughput, high-resolution era of X-ray astronomy.
