十种新黑洞自旋的系统观
A Systematic View of Ten New Black Hole Spins
摘要：
NuSTAR的发射和越来越多的通过引力波（GW）观测发现的二元黑洞（BBH）合并，以指数方式推进了我们对黑洞的理解。尽管由于其质量和角动量的充分描述而变得简单，但黑洞仍然是探索宇宙中最极端环境的神秘实验室。虽然最近十年取得了重大进展，但黑洞中自旋的分布尚未被理解。在这项工作中，我们提供了一个系统的分析，所有已知的黑洞在X射线双星系统（XB），以前已被观察到的NuSTAR，但尚未有一个自旋测量使用的“相对论反射”的方法从该数据获得。通过查看这些来源的所有可用档案NuSTAR数据，我们测量了十个新的黑洞自旋：IGR J17454-2919 - $a=0.97^{+0.03}_{-0.17}$ ; GRS 1758-258 -$a=0.991^{+0.007}_{-0.019}$ ; MAXI J1727-203 - $a=0.986^{+0.012}_{-0.159}$ ; MAXI J 0637 -430 -$a=0.97\pm0.02$ ; Swift J1753.5-0127 - $a=0.997^{+0.001}_{-0.003}$ ; V4641 Sgr -- $a=0.86^{+0.04}_{-0.06}$ ; 4U 1543-47 -- $a=0.98^{+0.01}_{-0.02}$ ; 4U 1957+11 -- $a=0.95^{+0.02}_{-0.04}$ ; H 1743-322 -- $a=0.98^{+0.01}_{-0.02}$ ; MAXI J1820+070 -- $a=0.988^{+0.006}_{-0.028}$（所有不确定度均在$1σ$置信水平）。我们讨论的影响，我们的测量对整个分布的恒星质量的黑洞自旋在XB，我们比较，与自旋分布在BBH，发现这两个分布是明显的不一致。此外，我们还讨论了这项工作对我们理解“相对论反射”自旋测量技术的影响，并讨论了可能导致测量偏差的系统不确定性的可能来源。
英文摘要：
The launch of NuSTAR and the increasing number of binary black hole (BBH) mergers detected through gravitational wave (GW) observations have exponentially advanced our understanding of black holes. Despite the simplicity owed to being fully described by their mass and angular momentum, black holes have remained mysterious laboratories that probe the most extreme environments in the Universe. While significant progress has been made in the recent decade, the distribution of spin in black holes has not yet been understood. In this work, we provide a systematic analysis of all known black holes in X-ray binary systems (XB) that have previously been observed by NuSTAR, but have not yet had a spin measurement using the "relativistic reflection" method obtained from that data. By looking at all the available archival NuSTAR data of these sources, we measure ten new black hole spins: IGR J17454-2919 -- $a=0.97^{+0.03}_{-0.17}$; GRS 1758-258 -- $a=0.991^{+0.007}_{-0.019}$; MAXI J1727-203 -- $a=0.986^{+0.012}_{-0.159}$; MAXI J0637-430 -- $a=0.97\pm0.02$; Swift J1753.5-0127 -- $a=0.997^{+0.001}_{-0.003}$; V4641 Sgr -- $a=0.86^{+0.04}_{-0.06}$; 4U 1543-47 -- $a=0.98^{+0.01}_{-0.02}$; 4U 1957+11 -- $a=0.95^{+0.02}_{-0.04}$; H 1743-322 -- $a=0.98^{+0.01}_{-0.02}$; MAXI J1820+070 -- $a=0.988^{+0.006}_{-0.028}$ (all uncertainties are at the $1σ$ confidence level). We discuss the implications of our measurements on the entire distribution of stellar mass black hole spins in XB, and we compare that with the spin distribution in BBH, finding that the two distributions are clearly in disagreement. Additionally, we discuss the implications of this work on our understanding of how the "relativistic reflection" spin measurement technique works, and discuss possible sources of systematic uncertainty that can bias our measurements.
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