Through a spectroscope, you see what's called an absorption spectrum.

通过分光镜，你可以看到所谓的吸收光谱。

It was an absorption spectrum, and it had a bunch of the same dark lines Fraunhofer had seen in our sun's spectrum.

这是一个吸收光谱，它有一堆和弗劳恩霍夫在太阳光谱中看到的一样的黑线。

While we’re observing these stars, we can use a spectrometer, the device that separates wavelengths, to reveal the star’s absorption spectrum and its elemental composition.

在观察这些恒星时，我们可以使用分光计（一种分离波长的设备）来揭示恒星的吸收光谱及其元素组成。

But when we study very distant bodies, we find that their absorption spectrum is slightly different from what we’d expect, given our knowledge of typical star compositions.

但是当我们研究非常遥远的天体时，我们发现它们的吸收光谱与我们预期的略有不同，这是基于我们对典型恒星组成的了解。

But when we study very distant bodies, we find that their absorption spectrum is slightly different from what we'd expect, given our knowledge of typical star compositions.

但是当我们研究非常遥远的天体时，我们发现它们的吸收光谱与我们预期的略有不同，因为我们对典型恒星组成的了解。