利用空-地干涉仪观测黑洞阴影
Black Hole Shadow Observations with Space-Ground Interferometers
摘要：
我们考虑了未来空间甚大基线干涉测量（VLBI）任务中可以通过数据处理和图像恢复程序恢复的黑洞（BH）阴影图像。对于质量为SgrA*、M87* 和M31* 的Kerr黑洞，在其背后光源的照射下，我们考虑了三种观测方式：地基干涉仪（类似于事件视界望远镜）、卫星位于地心轨道的天地干涉仪和卫星位于拉格朗日点$L_2$的天地干涉仪。地面望远镜单独成像与加入低轨道卫星的空间VLBI成像之间的显著差异是由基线增加和（u，v）覆盖范围的改善引起的。在所考虑的情况中，用于观测BH阴影的射电干涉仪的近地配置对于BH阴影观测是最优选的。随着轨道半径的进一步增加，直到拉格朗日点$L_2$，（u，v）填充的密度减小，结果似乎不太可靠。所有的情况下，模型图像。
英文摘要：
We consider the black hole (BH) shadow images which can be restored by data processing and image recovery procedures in future space Very Large Baseline Interferometry (VLBI) missions. For Kerr BHs with masses and coordinates of SgrA*, M87* and M31*, illuminated by light source behind them, we consider three kinds of observation: the ground-based interferometer (similar to the Event Horizon Telescope), space-ground interferometer with a satellite in geocentric orbit and space-ground interferometer with a satellite located in Lagrange point $L_2$. The significant difference between the images produced by the ground-based telescope alone and the one of the space VLBI with an added low-orbit satellite is caused by both the increased baseline and the improved of (u,v) coverage. The near-Earth configuration of the radio interferometer for the observation of BH shadows is the most preferable for the BH shadow observations among considered cases. With further increasing the orbit radius up to the Lagrange point $L_2$ the density of the (u,v) filling decreases and the results appear less reliable. Model images for all the cases are presented.
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