After the nuclear epics,about 380,000 years from the big bang, the temperature continues to cool, and electrons are captured by protons and nucleus to form hydrogen atoms and helium atoms. This period is called the compound period.
核子时代之后，距离大爆炸约38万年，温度持续冷却，电子开始被质子和氦核子捕获，形成氢原子和氦原子，这个时期称为复合时期。
After the compound is over, most of the protons in the universe become neutral atoms. Therefore, the photons are no longer disturbed and can travel freely in the universe. This cosmic event is called photon decoupling.
复合结束后，宇宙中的大部分质子变成了氢原子，因此，光子不再受到干扰，可以在宇宙中自由穿行，这个宇宙事件称为光子退耦。
Before decoupling occurs,most photons interact with electrons and protons in the photon-baryon fluid,resulting in an opaque or “foggy” universe.
在退耦发生之前，宇宙中多数的光子都与电子和质子在光子-重子液中进行交互作用，其结果是宇宙是不透明或处在“大雾”之中。
At this point, the universe began to become transparent. The first undisturbed photons arrived at us after a long period of time and distance. As the space expands, the wavelength increases with time, the light becomes weaker and the energy is lower.
至此，宇宙开始变得透明。第一批不受干扰的光子再经过漫长的时间和距离后到达我们这里，由于空间膨胀，导致波长随着时间的推移而增加，光线越来越微弱，能量也越来越低。
Finally, these light from the depths of the universe become microwave noise with a wavelength of 7.35 cm, and their temperature in the black body radiation spectrum is about 3K. This is the microwave background radiation we are familiar with.
最后，这些来自宇宙深处的光变成了波长为7.35厘米的微波噪声，它们在黑体辐射光谱的温度约为3K。这就是我们熟知的微波背景辐射。
In order to detect these microwave background radiation, WMAP came into being.
为了探测这些微波背景辐射，WMAP应运而生。
This is the Wilkinson Microwave Anisotropy Probe,or”WMAP”
这就是威尔金微波各向异性探测器（WMAP）。
It was launched to scan the early universe for the find-scale origins of this cosmin atlas.
它被用来扫描电磁波，寻找精细的早期宇宙图。
WMAP traveled beyond any interference from Earth,to a posion balanced between the Earth and the Sun.
WMAP远离了地球的干扰，到达了地球和太阳之间。
There,for two years,its detectors took in the pristine light of deep space.
在那里，两年来，它的探测器接收了深空中未被污染的光。
This is what WMAP saw!
这就是WMAP所见！
A pattern consistent with the filaments and voids that had evolved in the universe at large.
一种与宇宙大纤维结构相一致的图案。
It came 38000 years after the big bang.
它来自于大爆炸后38万年。
This is Cosmic microwave background radiation(CMB or CMBR)
这就是宇宙微波背景辐射。
It is an important source of data on the early universe because it is the oldest electromagnetic radiation in the universe, dating to the epoch of recombination.
宇宙微波背景是宇宙学的基础，因其为宇宙中最古老的光，可追溯至再复合时期。
With a traditional optical telescope, the space between stars and galaxies (the background) is completely dark. However, a sufficiently sensitive radio telescope shows a faint background noise, or glow, almost isotropic, that is not associated with any star, galaxy, or other object.
利用传统的光学望远镜，恒星和星系之间的空间（背景）是一片漆黑。然而，利用灵敏的辐射望远镜却可发现微弱的背景辉光，且在各个方向上几乎一模一样，与任何恒星，星系或其他对象都毫无关系。
In this image, the temperature of the cosmic microwave background in the blackbody radiation spectrum is 2.72548± 0.00057k, which means that the brightest and darkest regions in the image are only about 0.00114k apart, revealing a profound principle: the universe is homogeneous and isotropic under large-scale observation.
在这张图片中，宇宙微波背景在黑体辐射光谱的温度为2.72548±0.00057 K，即图片中最亮的区域与最暗的区域仅仅只差了约0.00114K，这揭示了一个影响深刻的原则：在大尺度的观测下，宇宙是均质与各向同性的。
One of the winners of this year’s Nobel Prize in Physics is related to CMB.
今年的诺贝尔物理学奖中，有一名得主和CMB有关。
Peebles has made many important contributions to the Big Bang model. With Dicke and others (nearly two decades after George Gamow, Ralph A. Alpher and Robert C. Herman), Peebles predicted the cosmic microwave background radiation.
皮布尔斯对大爆炸模型做出了许多重要贡献。在乔治·伽莫夫, 拉尔夫·阿尔菲和罗伯特·赫尔曼预测微波背景辐射近二十年之后，他与罗伯特·迪克等人解释了宇宙微波背景辐射是大爆炸的印记。
