透过淡淡的外缘螺旋腕可以看见背景星系。
Background galaxies are visible through the faint outer arms.
背景星系大约与我们银河系相当，并大约10倍于前景星系。
The background galaxy is about the size of the Milky Way Galaxy and is about 10 times larger than the foreground galaxy .
在这个范围内还散布着引人入胜的其它背景星系，还包括道钉状的前景恒星。
Intriguing background galaxies are scattered around the field that also includes spiky foreground stars.
在这个天区的精彩长时曝光影像里，还可以看见更遥远的昏暗背景星系。
This impressively deep exposure of the region also reveals faint and even more distant background galaxies.
敏锐的哈勃数据还暴露了更多遥远的背景星系，右边透过NGC 2442的星团和星云可见。
The sharp Hubble data also reveal more distant background galaxies seen right through NGC 2442's star clusters and nebulae.
背景星系的大小大约是NGC7331表面大小的十分之一，而距离上则大约是10倍甚至更远。
The background galaxies are about one tenth the apparent size of NGC 7331 and so lie roughly ten times farther away.
重力能使光线弯折，使巨大的星系团象望远镜一样，扭曲背景星系的图像，使之变得细长。
Gravity can bend light, allowing huge clusters of galaxies to act as telescopes, and distorting images of background galaxies into elongated strands.
暗物质构成了大部分的总质量，并主宰了集群的引力透镜，或从光线弯曲的背景星系因引力。
The dark matter makes up most of the total mass, and dominates the gravitational lensing of the cluster, or the bending of light from background galaxies due to gravity.
引力透镜公式计算所有的变量，比如距离和密度，对光何时离开背景星系以及行走了多远的距离给出更好答案。
The gravitational lens equations account for all the variables such as distance and density, and provide a better idea of when light left the background galaxy and how far it traveled.
在这片美丽的星野中，还有另外一些其它类型的背景星系，右下角的是邻近星系ngc 4562。
An assortment of other background galaxies is included in the pretty field of view, with neighboring galaxy NGC 4562 at the lower right.
结果是这些背景星系的多重影像被扭曲成长而暗的弧——透镜效应的例子，类似于透过酒瓶底的玻璃看远处的街灯。
As a result, multiple images of these background galaxies are distorted into long faint arcs — a simple lensing effect analogous to viewing distant street lamps through a glass of wine.
其中一个背景星系IC 1296在左上角，很清楚可以看到棒状及漩涡状的结构，可以跟漂亮的M57互相辉映。
By chance, one of the background galaxies, IC 1296 at the upper left, is close enough to show its barred, spiral structure making an attractive visual comparison with M57.
但是除了我们略知一二的更遥远背景星系以外，这张深空图像也提示了一个罕见的盒状内晕，在星系多尘的盘面之上和之下伸展到很远。
But along with a smattering of more distant background galaxies, the deep image also reveals a curious box-shaped inner halo extending far above and below this galaxy's dusty plane.
这张高清图片展现了这个星系壮观的的恒星与星尘盘的正面特征，背景上还有这一些星系，有些还能透过M101 看到。
The sharp image shows stunning features in the galaxy's face-on disk of stars and dust along with background galaxies, some visible right through M101 itself.
但仔细观察会发现许多背景上的星系都由于该星群的引力透镜的偏斜而被扩大并扭曲成怪异的长条弧状曲线。
A close inspection, however, shows that many background galaxies are strangely magnified and distorted into long curving arcs by the gravitational lens deflections of the cluster.
在图中还有其他背景性的透镜星系，而天文学家正是通过它们计算出了146-IG的质量。
There are other lensed background galaxies in the image as well, and the astronomers used those to get the mass of 146-ig.
在这片星际画面的背景上甚至还能看到一些在银河系之外的恒星星系。
Even galaxies of stars beyond our Milky Way can be found within the cosmic vista.
南极天文台三大观测宇宙的天文台之一，旨在检测由宇宙大爆炸而产生的大量存在于微光辐射中的扭曲现象，利用天文望远镜对宇宙射线背景进行筛选，再利用星系群的特点确定一个点，即当宇宙射线穿过极热气体时会产生轻微混乱，混乱的那一刻就是所要找的那个点。
The telescopes sift through the background cosmic radiation to find spots where it has been slightly perturbed as it passes through extremely hot gas, a hallmark characteristic of galaxy clusters.
卡什林斯基和同事们是在研究星系团气体与宇宙微波背景辐射之间相互作用时首次注意到黑暗流的。
Kashlinsky and colleagues first noticed the dark flow when studying the way gas in galaxy clusters interacts with the cosmic microwave background radiation.
在画面最右侧的部分略微有所压缩，好让你能看到背景上引人注目的相互作用的一对星系。
The frame at the far right has been compressed slightly to bring into view an intriguing interacting pair of background galaxies.
据期，含有更多热气的更明亮的星系团对于宇宙微波背景将有更大影响，而这正是新研究要证实的。
Brighter clusters-those with more hot gases-would be expected to have greater affects on the cosmic microwave background, and that's what the new study confirmed.
宇宙微波背景几乎但并不都是均匀的，而已知的不均匀的射线被认为是用来标记来自哪个星系(包括恒星系和行星系)。
The CMB is almost, but not quite, uniform, and the known irregularities in it are thought to mark the seeds from which galaxies-and therefore stars and planets-grew.
当宇宙微波背景辐射通过星系团时，气体将其中光线散射开来，其方式类似于地球大气层散射星光而使一些星星貌似闪烁。
These gases scatter light from the cosmic microwave background radiation as it passes through the clusters, similar to the way Earth's atmosphere can scatter starlight, making some stars twinkle.
这些类星体的河外星系是由当黑洞所发射的电子与大爆炸所遗留下来的宇宙背景辐射碰撞后所形成的，它为天文学家提供了关于早期宇宙的线索。
These quasar jets are formed when electrons emitted from a black hole impact with cosmic background radiation left by the big bang, giving astronomers clues about the conditions in the early universe.
从威尔金森微波各向异性探测器(WMAP)得来的数据显示出，细微温度变化是在宇宙微波背景辐射移动通过银河星系团气体时产生的。
Data from the Wilkinson microwave Anisotropy Probe (WMAP) can show the minute temperature changes created as the cosmic microwave background radiation moves through gases in galaxy clusters.
这反映了附近恒星的光热，2170星系是由其他蓝色反射星云，紧凑的红色发光区域，以及在模糊的背景下对恒星尘埃的飘带组成。
Reflecting the light of nearby hot stars, NGC 2170 is joined by other bluish reflection nebulae, a compact red emission region, and streamers of obscuring dust against a backdrop of stars.
但WMAP却没能够发现这些高能量的光子，所以在宇宙微波背景辐射上那些星系的周围有些光子的亏损。
WMAP cannot detect these higher energy photons, so there should be a deficit of CMB photons around clusters.
通常来说，宇宙微波背景辐射粒子先发生了蓝移（它们的峰向光谱的蓝端移动），但当它进入超星系团之后又发生了红移。这两个效果相互抵消。
Normally a CMB photon is first blueshifted (its peak shifts towards the blue end of the spectrum) when it enters the supercluster and then redshifted as it leaves, so that the two effects cancel.
ATA能够观察广泛的波长，因此可以检查在氢原子云层的星系团背景下的前景ETI信号。
The ATA can observe a wide range of wavelengths, so it can check stars in the foreground for ETI signals while it watches background galaxies for clouds of atomic hydrogen.
ATA能够观察广泛的波长，因此可以检查在氢原子云层的星系团背景下的前景ETI信号。
The ATA can observe a wide range of wavelengths, so it can check stars in the foreground for ETI signals while it watches background galaxies for clouds of atomic hydrogen.
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