Abstract

The study explores black hole (BH) shadow images which can be restored by data processing and image recovery procedures during space Very Large Baseline Interferometry (VLBI) missions in the future. For Kerr BHs with masses and coordinates of SgrA*, M87*, and M31*, all illuminated by a light source behind them, three kinds of observation are considered: 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 one from the space VLBI with an added low-orbit satellite is caused by both the increased baseline and the improved \((u,{v})\) coverage. The near-Earth configuration of the radio interferometer for BH shadow observations is the most preferable among the considered cases. As the orbit radius increases 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.

中文翻译：

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太空干涉仪的黑洞阴影观测

摘要

这项研究探索了黑洞（BH）阴影图像，该图像可在未来的太空超大型基线干涉测量（VLBI）任务期间通过数据处理和图像恢复程序来恢复。对于质量和坐标分别为SgrA *，M87 *和M31 *的Kerr BH，它们都被它们后面的光源照亮，可以考虑三种观察方法：基于地面的干涉仪（类似于Event Horizo​​n Telescope），具有位于地心轨道中的卫星的地面干涉仪和位于Lagrange点\（{{L} _ {2}} \）中的卫星的空地干涉仪。单独增加的低基线卫星和改进的\（（u，{v}）\）导致单独由地面望远镜产生的图像和来自太空VLBI的图像以及增加的低轨道卫星产生的图像之间的显着差异。覆盖范围。在所考虑的情况中，用于BH阴影观察的无线电干涉仪的近地配置是最可取的。随着轨道半径增加到拉格朗日点\（{{L} _ {2}} \），\（（u，{v}）\）填充的密度降低，结果显得不太可靠。给出了所有案例的模型图像。