The EHT's trick is a technique called very long baseline array interferometry (VLBI).

EHT 的技巧一种称为超线阵列干涉测量法 (VLBI) 的技术。

And this time, LIGO also has the support of KAGRA,   a new interferometry observatory in Hida, Japan.

这次，LIGO 还得到了位于日本飞驒市的新干涉测量天文台 KAGRA 的支持。

This is essentially  what the interferometer measures with light.

这本质干涉仪用光测量的内容。

Ye then launched her VLBI project at the observatory, but the research funding would not stretch to the 25-metre radio telescope that was needed.

叶老师随后在天文台启动了她的线干涉测量项目，但研究资金不会延伸到所需的 25 米射电望远镜。

This squeezing  minimizes the light's phase noise and squeezes it into amplitude noise, which the interferometer  doesn't measure.

这种挤压最大限度地减少了光的相位噪声，并将其挤压成干涉仪无法测量的振幅噪声。

We're interfering waves together, that's what interferometry means and so if those waves move back and forth a little bit when you interfere them they destructively interfere and you lose your signal.

我们正在一起干扰波，这干涉测量法的意思，所以如果这些波在你干扰它们时来回移动一点点，它们会破坏性地干扰，你会失去信号。

The EHT gets around this by linking together 15-20 telescopes. It uses a technique known as interferometry, in which astronomers on different continents simultaneously observe the same object, then combine the collected data on a supercomputer.

而 EHT 通过连接 15-20 个望远镜来巧妙地应对这一问题。它使用了一种被称为" 干涉测量术" 的技术，用这种技术，在不同大陆的天文学家可以同时观测同一目标，然后将收集到的数据组合在一台超级计算机。