How black holes are formed remains an open and fundamental question in astrophysics. Despite theoretical predictions, it lacks observations to understand whether the black hole formation experiences a supernova explosion. Here we report the discovery of an X-ray shell north of the Galactic microquasar SS 433 harboring a stellar-mass black hole spatially associated with radio continuum and polarization emissions and an H i cloud. Its spectrum can be reproduced by a 1 keV underionized plasma, from which the shell is inferred to have been created by a supernova explosion 20–30 kyr ago, and its properties constitute evidence for canonical supernova explosions to create some black holes. Our analysis precludes other possible origins including heated by jets or blown by disk winds. According to the lower mass limit of the compact object in SS 433, we roughly deduced that the progenitor should be more massive than 25 M _⊙. The existence of such a young remnant in SS 433 can also lead to new insights into the supercritical accretion in young microquasars and the γ-ray emission of this system. The fallback ejecta may provide accretion materials within tens of thousands of years, while the shock of the supernova remnant may play a crucial role in the cosmic-ray (re)acceleration.

中文翻译：

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X 射线壳揭示了银河系微类星体 SS 433 的超新星爆炸


黑洞是如何形成的仍然是天体物理学中一个悬而未决的基本问题。尽管有理论预测，但它缺乏观测来了解黑洞的形成是否经历过超新星爆炸。在这里，我们报告了在银河微类星体 SS 433 以北发现的一个 X 射线壳，其中包含一个在空间上与射电连续谱和极化发射相关的恒星质量黑洞和一个 H i 云。它的光谱可以用 1 keV 的欠电离等离子体再现，从中可以推断出外壳是由 20-30 kyr 前的超新星爆炸产生的，其特性构成了典型超新星爆炸产生一些黑洞的证据。我们的分析排除了其他可能的来源，包括被喷流加热或被盘风吹动。根据 SS 433 中致密物体的质量下限，我们粗略推断出其祖先的质量应该大于 25 _M⊙。SS 433 中存在这样一个年轻的残余物，也可以为年轻的微类星体中的超临界吸积和该系统的γ射线发射带来新的见解。后备喷出物可能在数万年内提供吸积材料，而超新星残余物的冲击可能在宇宙射线（再）加速中起关键作用。