另眼看宇宙之星系和超新星合辑

来源:钱德拉X射线空间望远镜网站

     本帖原名"钱德拉X射线空间望远镜眼中的宇宙".但翻译后发现除钱德拉拍摄的X射线图片外,还有其它空间望远镜拍的图片和几种不同波段的合成图片.故更改名字。己有朋友帮忙翻译了一些将持续更新，第一页是星系的图片，第二页将更新超新星的图片。


M82
Images from three of NASA's Great Observatories were combined to create this spectacular, multiwavelength view of the starburst galaxy M82. Optical light from stars (yellow-green/Hubble Space Telescope) shows the disk of a modest-sized, apparently normal galaxy.

结合来自NASA的3架大天文台的照片，得出了这张壮观的星爆星系M82多波段图象。来自恒星的可见光（图中为黄/绿色，哈勃太空望远镜拍摄）显示出的是一个中等大小、外观正常的星系盘。

Another Hubble observation designed to image 10,000 degree Celsius hydrogen gas (orange) reveals a startlingly different picture of matter blasting out of the galaxy. The Spitzer Space Telescope infrared image (red) shows that cool gas and dust are also being ejected. Chandra's X-ray image (blue) reveals gas that has been heated to millions of degrees by the violent outflow. The eruption can be traced back to the central regions of the galaxy where stars are forming at a furious rate, some 10 times faster than in the Milky Way Galaxy.

哈勃的另一张照片用于拍摄10000摄氏度左右的中性氢气体（图中呈橙色），它揭示出了惊人不同的又一场面，物质正从星系中冲出。斯必泽太空望远镜的红外图象（红色）显示的是外抛的冷气体与尘埃。钱德拉的X射线图象（蓝色）展现的则是被狂暴的外流物加热到数百万度的气体。喷出物可以追溯到星系的中心区域，这里的恒星在以10倍于我们银河系的狂暴速度诞生着。

Many of these newly formed stars are very massive and race through their evolution to explode as supernovas. Vigorous mass loss from these stars before they explode, and the heat generated by the supernovas drive the gas out of the galaxy at millions of miles per hour. It is thought that the expulsion of matter from a galaxy during bursts of star formation is one of the main ways of spreading elements like carbon and oxygen throughout the universe.

许多新近形成的恒星质量都很大，并会快速演化到爆发的超新星。在爆发之前，这些恒星会发生剧烈的物质损失，而超新星产生的热量也可以将气体以每小时几百万英里的速度驱出星系。人们认为，星系在狂暴的产星过程中外抛的物质是将碳、氧等元素洒遍宇宙的一大主要途径。

The burst of star formation in M82 is thought to have been initiated by shock waves generated in a close encounter with a large nearby galaxy, M81, about 100 million years ago. These shock waves triggered the collapse of giant clouds of dust and gas in M82. In another 100 million years or so, most of the gas and dust will have been used to form stars, or blown out of the galaxy, so the starburst will subside.

人们认为，引发M82中恒星形成的原因是1亿年前与邻近星系M81近距离遭遇产生的激波。激波促发了M82中巨型气体尘埃云的坍缩。差不多再过1亿年，大多数气体和尘埃要么用于产星活动，要么被吹出星系，因而星爆会终止。


下图是三个观测站的合成图像

                               
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Chandra X-ray Images of M82, Broadband & 3-Color

钱德拉拍摄的M82 X射线图象，宽波段图与3色图

Chandra's X-ray image reveals gas that has been heated to millions of degrees by the violent outflow of matter blasting out of the galaxy. The eruption can be traced back to the central regions of the galaxy where stars are forming at a furious rate, some 10 times faster than in the Milky Way Galaxy. Many of these newly formed stars are very massive and race through their evolution to explode as supernovas. Vigorous mass loss from these stars before they explode, and the heat generated by the supernovas drive the gas out of the galaxy at millions of miles per hour. It is thought that the expulsion of matter from a galaxy during bursts of star formation is one of the main ways of spreading elements like carbon and oxygen throughout the universe. The Chandra X-ray image on the left is shown in the broadband color scheme used in the X-ray/infrared/optical composite. The image on the right is Chandra's 3-color X-ray view where red, green, and blue represent low, medium, and high-energy X-rays respectively.
Scale: Image is 7.9 arcmin across.

钱德拉拍摄的X射线图象展现出了被狂暴的外流物加热到数百万度的气体。喷出物可以追溯到星系的中心区域，这里有恒星在以10倍于我们银河系的狂暴速度诞生着。许多新近形成的恒星质量都很大，并会快速演化到爆发的超新星。在爆发之前，这些恒星会发生剧烈的物质损失，而超新星产生的热量也可以将气体以每小时几百万英里的速度驱出星系。人们认为，星系在狂暴的产星过程中外抛的物质是将碳、氧等元素洒遍宇宙的一大主要途径。左侧这张钱德拉的X射线照片是使用X射线/红外/可见光合成图中的宽波段着色法显示的。右侧是钱德拉的三色X射线图，红、绿、蓝三色分别代表低能、中能与高能X射线。
比例：图象覆盖的视场是7.9角分

                               
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[ 本帖最后由 寻找拉玛 于 2008-2-2 21:56 编辑 ]

LZ可否把图处理一下再传，我打开的好辛苦！慢那！仿佛时光倒流回到未升级前了

继续接2楼的草帽星系


Chandra X-ray Image of the Sombrero Galaxy
钱德拉拍摄的草帽星系X射线图象


The Sombrero galaxy lies at the southern edge of the Virgo cluster of galaxies and is one of the most massive objects in that group, equivalent to about 800 billion suns. This Chandra X-ray image of Sombrero (a.k.a. M104) shows hot gas in the galaxy and point sources that are a mixture of galaxy members and background objects. In this image, Chandra low energy X-rays (0.3-1.5 keV) are color-coded orange and high energy X-rays (1.5-7.0 keV) are in blue. The Chandra image shows hot gas in the Sombrero galaxy and point sources that are a mixture of galaxy members and background objects.

(Credit: NASA/UMass/Q.D.Wang et al.)

草帽星系位于室女座星系团的南缘，也是该星系团中质量最大的天体之一，约合8000亿倍太阳质量。这张由钱德拉拍摄的草帽星系（即M104）X射线图象揭示出了星系中的热气体与点源，后者既包括星系成员，也包括背景天体。在这张照片中，钱德拉拍摄的低能X射线辐射（0.3-1.5 keV）用橙色表示，高能X射线（1.5-7.0 keV）则表示为蓝色。钱德拉的图象揭示出草帽星系中的热气体，以及由星系成员星和背景天体组成的点源。


版权：NASA/UMass/Q.D.Wang et al.

                               
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Spitzer Infrared Image of the Sombero Galaxy

斯必泽拍摄的草帽星系红外图象


The Sombrero galaxy is located some 28 million light-years away. Spitzer detected infrared emission not only from the ring, but from the center of the galaxy too, where there is a huge black hole, believed to be a billion times more massive than our Sun. The Spitzer picture is composed of four images taken at 3.6 (blue), 4.5 (green), 5.8 (orange), and 8.0 (red) microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8 and 8-micron images to enhance the visibility of the dust features.



草帽星系位于2800万光年以外。斯必泽不仅探测到了来自星系环的红外辐射，还有来自星系中心的辐射，这里有一个巨大的黑洞，其质量据信是太阳的10亿倍以上。斯必泽的照片由3.6（蓝）、4.5（绿）、5.8（橙）、8.0（红）微米四个波段上拍摄的照片合成。为增强尘埃结构的对比度，来自星光的辐射（3.6微米波长所表示的）已从5.8和8微米的图象上扣除了。
(Credit: NASA/JPL-Caltech/Univ. AZ/R.Kennicutt/SINGS Team)

版权：NASA/JPL-Caltech/Univ. AZ/R.Kennicutt/SINGS Team

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-25 22:04 编辑 ]

我这里速度可不慢。

The Antennae:
Chandra Locates Mother Lode of Planetary Ore in Colliding Galaxies

触角星系：钱德拉确认出碰撞星系
来源:http://chandra.harvard.edu/photo/2004/antennae/index.html

This montage of Chandra images shows a pair of interacting galaxies known as The Antennae. Rich deposits of neon, magnesium, and silicon were discovered in the interstellar gas of this system.

这张钱德拉拍摄的拼接图展示的是一对互扰星系，名为触角星系。在系统的星际气体中，人们发现了丰富的氖、镁、硅元素沉积。

The top image, a wide field X-ray view, reveals spectacular loops of hot gas spreading out from the southern part of The Antenna into intergalactic space. Also shown are huge clouds of multimillion degree gas and bright point like sources due to neutron stars and black holes. The image is color coded so that low, medium and high energy X-rays appear as red, green and blue, respectively.

上图是宽视场X射线照片，其中显现的是壮观的热气体环，从触角星系的南侧向外延伸至星系际空间。同样显现在其中的是巨大的气体云团，温度达几百万度，还有明亮的点源，这是由于中子星与黑洞造成的。图中的红、绿、蓝三色分别代表低能、中能与高能X射线。

Direct hits between stars are extremely rare when galaxies collide, but huge gas clouds can crash into each other at high speeds, creating shock waves that heat the clouds and the surrounding gas to millions of degrees. In the closeup view on the lower left, also color coded by X-ray energies, the point sources have been taken out to emphasize the hot gas clouds in the central regions of The Antennae.

当星系相撞时，恒星之间的对撞非常少，但巨大的气体云团会以高速互相冲击，产生激波，并将云团和周围的气体加热到几百万度。在左下的放大图中（仍按X射线波段的着色法表示），点源已被扣除，这样就可以突出触角星系中心区域的热气体云。

Collisions between the gas clouds may trigger a stellar baby boom. The most massive of these young stars race through their evolution in a few million years and explode as supernovas. Heavy elements manufactured inside these stars are blown away by the explosions that further heat the gas clouds and enrich them with heavy elements such as neon, magnesium, silicon and iron.

气体云之间的碰撞可能会触发产星高潮。质量最大的年轻恒星会在几百万年的时间里飞快地演化完毕，并以超新星的形式爆发。恒星内部会产生重元素，爆发将元素吹开，将气体云进一步加热，并使其中的氖、镁、硅、铁等重元素丰度提升。

The image at the lower right is processed and color-coded to show regions rich in iron (red), magnesium (green) and silicon (blue). These are the types of elements that form the ultimate building blocks for habitable planets.

右下图经过处理着色，展现了富含铁（红色）、镁（绿色）和硅（蓝色）的区域。这些元素都是形成可居住行星的根本基石。

Enrichment from supernovas occurs in all galaxies, but usually the new elements are observed in a highly diluted form as they are mixed up with the rest of the interstellar gas. This Chandra image is remarkable in that it shows clouds in which magnesium and silicon are 16 and 24 times as abundant as in the Sun.

所有的星系都历经了超新星导致的重元素富集，但通常情况下，由于与其余星际气体的混合，人们所见的新元素都非常分散。钱德拉的这张照片不寻常的原因是，它显示出的气体云有着16至24倍于太阳的镁与硅丰度。

As the enriched gas cools, a new generation of stars will form, and with them new planets. A number of studies indicate that clouds enriched in heavy elements are more likely to form stars with planetary systems. Several hundred million years from now, an unusually high number of planets may form in The Antennae.

当富含重元素的气体冷却后，新一代恒星将会形成，进而是新的行星。一系列研究表明，富集了重元素的气体云更容易形成拥有行星系统的恒星。几亿年后，触角星系中形成的行星数量将是不寻常地高。

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-24 17:16 编辑 ]

好不容易打开了，看到了，光影好迷幻啊，好图！THX！

车轮星系

5-Panel version of Chandra, GALEX, Spitzer & Hubble Images

钱德拉、GALEX、斯必泽与哈勃拍摄的5联图

This image combines data from four different observatories: the Chandra X-ray Observatory (purple); the Galaxy Evolution Explorer satellite (ultraviolet/blue); the Hubble Space Telescope (visible/green); the Spitzer Space Telescope (infrared/red). The unique shape of the Cartwheel Galaxy with its huge rim - larger than the diameter of the Milky Way galaxy - is likely due to a collision with one of the smaller galaxies on the lower left several hundred million years ago. The insets to the right of the composite show how each telescope individually views the Cartwheel. The colors represented in these insets do not correspond with the colors in the larger composite. Hubble's view of the Cartwheel is colored green in the larger composite and GALEX's UV view is colored blue. (Credit: Composite: NASA/JPL/Caltech/P.Appleton et al.; X-ray: NASA/CXC/A.Wolter & G.Trinchieri et al.)

   这张照片是使用4架轨道天文台的数据合成的：钱德拉X射线天文台（紫）、星系演化探测器（紫外波段，蓝色）、哈勃太空望远镜（可见光波段，绿色）以及斯必泽太空望远镜（红外波段，红色）。车轮星系独特的外观及庞大的外缘（比银河系的直径还要大）可能起源于几亿年前与左下某个小星系的碰撞。右侧插入的小图是每架望远镜各自眼中的车轮星系。插图中的颜色与大型合成图中的不同。在合成图中，哈勃所见的车轮星系以绿色表示，GALEX所见的UV图以蓝表示。
版权：合成图：NASA/JPL/Caltech/P.Appleton et al.；X射线：NASA/CXC/A.Wolter & G.Trinchieri et al.

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-25 21:54 编辑 ]

Chandra X-ray Image of Cartwheel Galaxy

钱德拉拍摄的车轮星系X射线照片


The brightest X-ray sources in the Chandra X-ray image of the Cartwheel Galaxy are likely black holes, and appear as the white dots that lie along the rim of the X-ray image. The Cartwheel contains an unusually large number of these black hole X-ray sources, because many massive stars formed in the rim. (Credit: NASA/CXC/A.Wolter & G.Trinchieri et al.)
在钱德拉拍摄的车轮星系X射线照片中，最明亮的X射线源可能是黑洞，它们是沿X射线图象边缘排布的白点。车轮星系中，这样的黑洞X射线源出乎寻常地多，这是由于有大量的大质量恒星在外缘形成。
版权：Credit: NASA/CXC/A.Wolter & G.Trinchieri et al.

                               
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星系演化探测器拍摄的车轮星系紫外图象

                               
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斯必泽太空望远镜拍摄的车轮星系红外图象

                               
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哈勃太空望远镜拍摄的车轮星系光学图象

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-25 22:01 编辑 ]

NGC 4258 (M106):

Mysterious Arms Revealed
揭示神秘的旋臂

A combination of space and ground-based observations, including X-ray data from Chandra, has helped reveal the nature of the so-called anomalous arms in the spiral galaxy NGC 4258 (also known as M106). These arms have been known for decades, but their origin remained mysterious to astronomers.

结合地面和空间的观测（包括钱德拉的X射线数据），人们揭示出了旋涡星系NGC 4258（即M106）中所谓反常旋臂的本质。数十年前这些旋臂就已为人所知，但对于天文学家来说，它们的起源仍旧是个谜。

In visible (shown in gold) and infrared (red) light, two prominent arms emanate from the bright nucleus and spiral outward. These arms are dominated by young, bright stars, which light up the gas within the arms. But in radio (purple) and Chandra's X-ray (blue) images, two additional spiral arms are seen.

在可见光（以金黄色表示）和红外（以红色表示）波段，两条突出的旋臂从星系核区伸出，并螺旋向外延展。旋臂上主要是年轻明亮的恒星，是它们将旋臂内的气体照亮。但在射电（以紫色表示）及钱德拉所见的X射线（以蓝色表示）图象上，还可以看到另外两条旋臂。

By analyzing data from XMM-Newton, Spitzer, and Chandra, scientists have confirmed earlier suspicions that the ghostly arms represent regions of gas that are being violently heated by shock waves. Previously, some astronomers had suggested that the anomalous arms are jets of particles being ejected by a supermassive black hole in nucleus of NGC 4258. But radio observations at the Very Large Array later identified another pair of jets originating in the core.

通过分析来自XMM-牛顿、斯必泽与钱德拉的数据，科学家证实了早期的猜想，即在朦胧的旋臂区域中，气体正被激波剧烈加热。先前一些天文学家认为，反常旋臂是被NGC 4258中心的特大质量黑洞抛出的粒子喷流。但随后甚大天线阵进行的射电观测辨认出了另外一对源自星系核的喷流。

However, the jets do heat the gas in their line of travel, forming an expanding cocoon. Because the jets lie close to M106's disk, the cocoon generates shock waves and heat the gas in the disk to millions of degrees, causing it to radiate brightly in X-rays and other wavelengths.

但在喷流行进的过程中，它们确实会将气体加热，产生膨胀的茧状结构。由于喷流靠近M106的星系盘，茧状结构会产生激波，将盘中的气体加热的几百万度，使其在X射线及其他波段上发出明亮的辐射。

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-24 17:08 编辑 ]

M31
来源:http://chandra.harvard.edu/photo/2006/m31/index.html

Andromeda Galaxy (M31): The Heat Is On in Andromeda's Center

仙女座大星云（M31）：仙女中心的热量沸腾

This color-coded Chandra image (red/low energy, green/medium energy, and blue/high energy X-rays) shows the central region of the Andromeda Galaxy, a.k.a. M31 where a diffuse, X-ray emitting cloud of hot gas was discovered in the midst of a collection of point-like sources.

钱德拉的伪彩色图象（红色表示低能，绿色表示中能段，蓝色表示高能X射线）展示了仙女座大星系机M31的中心，在一群点源中间发现的是弥漫的高温气体云，发出X射线辐射。

Analysis of the X-ray data shows that the point sources are associated with binary star systems that contain a neutron star or black hole that is pulling matter away from a normal star. As the matter falls toward the neutron star or black hole, it is heated by frictional forces to tens of millions of degrees, and produces X-rays.

对X射线数据的分析表明，点源与包含有中子星或黑洞（它们正从正常恒星吸走物质）的双星系统成协。当物质落向中子星或黑洞时，会被摩擦力加热到几百万度，并产生X射线。

The diffuse X-ray cloud is due to gas that has accumulated in the central region and been heated to millions of degrees, probably by shock waves from supernova explosions. The energy input from the supernovas could also be driving gas out of the central region. This process may affect both the shape and evolution of the galaxy by depleting the raw material for the formation of new stars and preventing more gas from accumulating there.

弥漫的X射线云的成因是中心区域所积累并被加热到数百万度的气体，加热的可能原因是超新星爆发产生的激波。来自超新星的能量注入还可以将气体从中心驱出。这样的过程对星系的外形与演化都会有影响，原因是它会让产生新生恒星的原始物质耗尽，也会阻碍更多气体在这里的积累。

Andromeda, a large spiral galaxy much like our Milky Way Galaxy, is relatively nearby and can be easily seen with binoculars in the autumn sky. The galaxy's central region is called the galactic bulge because the stars form a ball a few thousand light years in diameter that extends above and below the disk of the galaxy.

仙女座大星云是类似银河系的大型旋涡星系，距离我们相对较近，在秋季的星空下，用双筒望远镜就可以很容易地看到它。星系的中心区域叫做核球，原因是恒星组成了直径几千光年的球体，膨胀到星系盘上下两侧。

                               
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Chandra X-ray & Spitzer Infrared Image of Andromeda Galaxy (M31)

钱德拉的X射线图象与斯必泽的红外图象


Andromeda, a large spiral galaxy much like our Milky Way Galaxy, is relatively nearby and can be easily seen with binoculars in the autumn sky. The galaxy's central region is called the galactic bulge because the stars form a ball a few thousand light years in diameter that extends above and below the disk of the galaxy. In this Chandra/Spitzer composite, red represents Spitzer's 24 micron mid-infrared data, green represents low-energy X-rays from Chandra (0.5-2.0 keV), and blue represents high-energy X-rays from Chandra (2.0-4.0 keV).
仙女座大星云是类似银河系的大型旋涡星系，距离我们相对较近，在秋季的星空下，用双筒望远镜就可以很容易地看到它。星系的中心区域叫做核球，原因是恒星组成了直径几千光年的球体，膨胀到星系盘上下两侧。在这张钱德拉与斯必泽的合成图中，红色代表斯必泽的24微米中红外数据，绿色代表钱德拉的低能X射线数据（0.5-2.0 keV），蓝色代表钱德拉的高能X射线数据（2.0-4.0 keV）

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-25 21:46 编辑 ]

第二页将更新超新星的图片

[ 本帖最后由 寻找拉玛 于 2007-12-25 22:02 编辑 ]

好看,想看,继续上.

填补了本版空白的好图！
精华！

赞  就这是X波段  强

真好,真美.

虽然，看不懂但是很漂亮。
顶啦

G292.0+1.8:
Stellar Forensics with Striking Image from Chandra

G292.0+1.8：钱德拉新图中的恒星纷争
来源:http://chandra.harvard.edu/photo/2007/g292/index.html

The aftermath of the death of a massive star is shown in beautiful detail in this new composite image of G292.0+1.8. In color is the Chandra X-ray Observatory image - easily the deepest X-ray image ever obtained of this supernova remnant - and in white is optical data from the Digitized Sky Survey. Although considered a "textbook" case of a supernova remnant, the intricate structure shown here reveals a few surprises.

这张新的G292.0+1.8合成照片以漂亮的细节揭示出了大质量恒星来世的复杂性。彩色部分是钱德拉X射线天文台拍摄的图象，它轻易地成为了有有史以来曝光最深的超新星遗迹X射线照片；而白色表示来自数字化巡天的光学数据。虽然该遗迹被认为是超新星遗迹的“教科书”式样板，复杂的结构还是揭示出了几个惊人之处。

Near the center of G292.0+1.8 is the so-called pulsar wind nebula, most easily seen in high energy X-rays. This is the magnetized bubble of high-energy particles that surrounds the "pulsar", a rapidly rotating neutron star that remained behind after the original, massive star exploded. The narrow, jet-like feature running from north to south in the image is likely parallel to the spin axis of the pulsar.


G292.0+1.8中心附近是所谓的脉冲星风星云，在高能X射线下轻易可见。它是磁化的高能粒子泡，围绕着“脉冲星”，也就是初始的大质量恒星爆发后残留的快速自转中子星。自北向南贯穿图象的狭窄喷流结构可能与脉冲星的自转轴重合。

The pulsar is located slightly below and to the left of the center of G292.0+1.8. Assuming that the pulsar was born at the center of the remnant, it is thought that recoil from the lopsided explosion may have kicked the pulsar in this direction. However, the kick direction and the pulsar spin direction do not appear to be aligned, in contrast to apparent spin-kick alignments seen in some other supernova remnants.


脉冲星位于G292.0+1.8中部略略偏左的地方。假设脉冲星诞生于遗迹中心，人们认为，偏心爆发产生的反作用力可能把脉冲星踢到了这个方向上。不过自转方向与外力方向看起来并不重合，而某些超新星遗迹的情况与之相反，自转与外力吻合。


Another key feature of this remnant is the long white line running from left to right across the center called the equatorial belt. This structure is thought to be created when the star - before it died - expelled material from around its equator via winds. The orientation of the equatorial belt suggests the parent star maintained the same spin axis both before and after it exploded.

该遗迹的另一关键特征是，赤道方向有一道明亮的白色环带，自左向右穿过穿过遗迹的中心，名为环赤道带。该结构据信产生于恒星死亡之前，是它以星风的形式沿赤道外抛的物质。环赤道带的方向说白，前身星在爆发前后的自转轴取向保持不变。


One puzzling aspect of the image is the lack of evidence for thin filaments of high energy X-ray emission, thought to be an important site for cosmic ray acceleration in supernova remnants. These filaments are seen in other supernova remnants such as Cassiopeia A, Tycho and Kepler. One explanation may be that efficient acceleration occurs primarily in very early stages of supernova remnant evolution, and G292.0+1.8, with an estimated age of several thousand years, is too old to show these effects. Casseiopeia A, Tycho and Kepler, with ages of several hundred years, are much younger.


这张图片令人困惑的一点是，其中缺乏高能X射线辐射的精细纤维结构迹象，人们认为这样的结构是超新星遗迹中宇宙线加速的重要场所。纤维结构见于仙后座A、第谷、开普勒等超新星遗迹中。一种可能的解释是，有效的加速发生在超新星演化极早期，而G292.0+1.8测出的年龄是几千岁，对于这些过程来说已经是太老了。而仙后座A、第谷、开普勒只有几百年的历史，要年轻得多。

                               
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[ 本帖最后由 寻找拉玛 于 2007-12-24 17:26 编辑 ]