高红移Lyα发射线星系观测研究

高红移Lyα发射线星系的研究是理解宇宙恒星形成历史和早期星系形成的关键.作为高红移宇宙的重要组成部分,Lyα发射线星系是研究星系形成、宇宙恒星形成和结构形成历史以及宇宙再电离时期的重要探针.近20年随着8–10 m级地面望远镜和红外设备的发展,利用窄带测光技术和光谱观测,人们对Lyα发射线星系的研究取得了巨大进展.本文主要介绍由窄带测光技术选取的红移2以上的Lyα发射线星系的成团性质、恒星星族和发射线星云性质、恒星形成性质、紫外连续谱和Lyα发射线形态,与莱曼断裂星系的关系,对宇宙恒星形成率密度的贡献,以及极高红移Lyα发射线星系对宇宙再电离时期的限制等方面的研究进展.     

低红移河外星系中性氢原子气体观测

我们回顾了近年来近邻宇宙星系中HI的研究进展,包括星系怎样吸积HI气体、HI在星系中的含量和分布、HI跟恒星形成率的关系以及环境对星系中HI的影响.近邻宇宙中仍然没有发现直接的证据支持HI吸积,说明这个过程很缓和.星系团、组尺度的环境以及局部星系密度环境对星系中HI含量有很明显的影响,然而我们仍不清楚实现这一过程的具体细节.不同星系内HI的分布具有很多共性,例如HI质量-直径关系,HI盘在光学盘外沿弯曲的普遍性,然而从宇宙学下的星系形成模型上理解这些共性仍然是个难题.在没有可探测的分子气体的低气体面密度区,HI与恒星形成活动有密切联系,表现在恒星形成覆盖面积比例和恒星形成面密度都与HI面密度相关.然而HI和恒星形成之间的联系怎样被激发以及被哪些物理条件约束仍然未明.相信接下来几年到几十年里,射电数据量的大爆炸会让一些未解之谜逐渐明朗.     

星系紫外深场巡天观测进展

紫外波段是星系能谱分布中的重要部分.其包含大量原子、离子和分子的共振线以及研究重要物理过程的连续辐射,提供了理论研究重要的观测限制.在星系研究中,紫外辐射追踪大质量恒星,是测量和理解宇宙中恒星形成历史的重要工具.紫外辐射也可追踪大质量黑洞吸积盘,是理解吸积物理过程的重要手段.其涉及的关键科学问题包括宇宙正午时期的恒星形成历史与星系演化、宇宙重子物质缺失、宇宙再电离能量来源以及星系吸积和外流反馈等.本文重点阐述了紫外深场巡天观测的发展现状及其在星系科学研究中发挥的作用.主要介绍了深场仪器的基本参数、深场观测的目的和任务,以及数据及科学产出,并对国内外正在计划中的未来紫外观测进行了总结和展望.     

国内期刊亮点

<正>专刊推介LAMOST巡天及早期成果星系是宇宙结构的基本单元,恒星形成和演化的场所。研究和阐释星系的形成和演化是21世纪天体物理学的重大问题。银河系是唯一可以将其星族组成解析为单体并进行细致研究的旋涡星系。位于河北省兴隆县、由中国科学院国家天文台运行的大天区面积多目标光纤光谱天文望远镜(LAMOST)是当今世界上光谱获取率最高的大口径、宽视场光谱巡天望远镜。2012     

星系(含银河系)中的恒星形成

正宇宙中各尺度的恒星形成,不论是位于宇宙边缘的第1代恒星还是在我们银河系"家园"里的恒星,都是贯穿于宇宙起源和天体演化的核心科学问题。可以说,恒星是宇宙中的"原子",有关恒星是怎样形成的这一问题则是当代天体物理学研究的枢纽:恒星形成不但决定星系的结构和演化,而且人类赖以生存的行星系统的起源也与之紧密相关。另外,宇宙中的大部分元素(包     

科学家谈天文学重要方向 星系的演化

正星系的形成和演化是天体物理的前沿领域。该领域以现代宇宙学提供的大尺度结构形成和演化的成熟理论作为基本框架,通过观测和统计研究宇宙各时期星系的形态结构、星族构成、气体吸积、恒星演化、黑洞成长、化学元素、恒星和气体动力学等物理性质及其演变过程,试图阐明宇宙中各类星系的物理起源、演化关系以及它们与宇宙大尺度结构的物理联系,从而总结出支配星系演化的普适物理规律。目前被普遍接受的星系形成理论认为,星系在暗物质晕中形成和演化,其基本图     

星系团的性质与其最亮成员星系中的恒星形成活动的相关性

基于哈勃空间望远镜的CLASH巡天观测数据,对其中23个大质量的、红移范围在0.18z0.89的星系团的物理性质(质量、中心区域的熵等)与其最亮成员星系(最亮团星系)中的恒星形成活动间的关系进行了研究。研究表明最亮团星系的恒星形成率与其宿主星系团的质量、中心区域的熵值存在明显的相关:质量越小、中心区域熵值越低的星系团中其最亮团星系的恒星形成率越高,而与最亮团星系本身的物理性质(如恒星质量)几乎不存在相关。研究结果意味着:造成中等红移最亮团星系中的恒星形成活动的冷气体来源于其宿主星系团内的热气体冷却,而不是星系本身。     

空中有多个太阳吗

美国加州理工学院的天文学家在新近出版 的《自然》杂志上报告说,他们发现天鹅星座中 的HD188753星系中有3颗恒星。处于该星系中 心的一颗恒星与太阳系中的太阳类似,它旁边 的行星体积至少比木星大14％。该行星与中心恒 星的距离大约为800万千米,是太阳和地球之间 距离的二十分之一。而星系的另外两颗恒星处 于外围,它们彼此相距不远,也围绕中心恒星公 转。 银河系中的星系多为单星系或双星系,具 有三颗以上恒星的星系被称为聚星系,不太多 见。 恒星并不是平均分布在宇宙之中,多数的 恒星会受彼此的引力影响,形成聚星系统,如双     

恒星诞生使宇宙发出第一缕光

由于幼年时期宇宙温度太高,光在那时根本无法闪亮。那么宇宙中的第一缕光线是从哪儿来的呢?通过研究距地球2.81亿光年的一个小星系发出的辐射,天文学家认为,星系内部恒星的诞生可能促使宇宙发出了第一缕光。宇宙被认为产生于距今约137亿年前的“大爆炸”。紧接着“大爆炸”后的宇宙温度极高,物质粒子全部以离子化形式存在。这种情况下,恒星星系这种致密的物质结构无法轻易形成。随着宇宙的膨胀、冷却和去离子化,很多原子核和电子结合在一起,形成了氢和氦这种中性的、原子量小的原子。虽然恒星随后开始形成,但由于宇宙处于去离子化状态,光很…     

如何测量宇宙中所有的星光?

<正>第一颗恒星诞生于宇宙大爆炸后的几亿年。自此之后,宇宙变成了效率极高的"造星工厂"。迄今为止,宇宙已产生了约2万亿个星系,包含了数不尽的恒星。这些星星一共发出了多少光?近日,来自美国克莱姆森大学的天体物理学家居然给出了答案:宇宙中的恒星已经产生了4×1084个光子。实际上,宇宙中所有曾经存在过的星系发出的光芒都积累在河外背景光(EBL)中,只是因为散布     

A close nuclear black-hole pair in the spiral galaxy NGC 3393

The current picture of galaxy evolution advocates co-evolution of galaxies and their nuclear massive black holes, through accretion and galactic merging. Pairs of quasars, each with a massive black hole at the centre of its galaxy, have separations of 6,000 to 300,000 light years (refs 2 and 3; 1 parsec = 3.26 light years) and exemplify the first stages of this gravitational interaction. The final stages of the black-hole merging process, through binary black holes and final collapse into a single black hole with gravitational wave emission, are consistent with the sub-light-year separation inferred from the optical spectra and light-variability of two such quasars. The double active nuclei of a few nearby galaxies with disrupted morphology and intense star formation (such as NGC 6240 with a separation of about 2,600 light years and Mrk 463 with a separation of about 13,000 light years between the nuclei) demonstrate the importance of major mergers of equal-mass spiral galaxies in this evolution; such mergers lead to an elliptical galaxy, as in the case of the double-radio-nucleus elliptical galaxy 0402+379 (with a separation of about 24 light years between the nuclei). Minor mergers of a spiral galaxy with a smaller companion should be a more common occurrence, evolving into spiral galaxies with active massive black-hole pairs, but have hitherto not been seen. Here we report the presence of two active massive black holes, separated by about 490 light years, in the Seyfert galaxy NGC 3393 (50 Mpc, about 160 million light years). The regular spiral morphology and predominantly old circum-nuclear stellar population of this galaxy, and the closeness of the black holes embedded in the bulge, provide a hitherto missing observational point to the study of galaxy/black hole evolution. Comparison of our observations with current theoretical models of mergers suggests that they are the result of minor merger evolution.     

Energy input from quasars regulates the growth and activity of black holes and their host galaxies

In the early Universe, while galaxies were still forming, black holes as massive as a billion solar masses powered quasars. Supermassive black holes are found at the centres of most galaxies today, where their masses are related to the velocity dispersions of stars in their host galaxies and hence to the mass of the central bulge of the galaxy. This suggests a link between the growth of the black holes and their host galaxies, which has indeed been assumed for a number of years. But the origin of the observed relation between black hole mass and stellar velocity dispersion, and its connection with the evolution of galaxies, have remained unclear. Here we report simulations that simultaneously follow star formation and the growth of black holes during galaxy-galaxy collisions. We find that, in addition to generating a burst of star formation, a merger leads to strong inflows that feed gas to the supermassive black hole and thereby power the quasar. The energy released by the quasar expels enough gas to quench both star formation and further black hole growth. This determines the lifetime of the quasar phase (approaching 100 million years) and explains the relationship between the black hole mass and the stellar velocity dispersion.     

等导程回转刀具虚拟实境的通用模型及其应用

根据轴向速度与回转速度之比为螺旋参数 ,给出了等导程回转刀具上刃口设计的通用模型和虚拟制造中磨用砂轮与回转刀具相对进给速度的通用公式 ,进而结合实例给出了等导程回转刀具虚拟实境研究中相关问题的处理方法和对应结果 .     

An almost head-on collision as the origin of two off-centre rings in the Andromeda galaxy

The unusual morphology of the Andromeda galaxy (Messier 31, the closest spiral galaxy to the Milky Way) has long been an enigma. Although regarded for decades as showing little evidence of a violent history, M31 has a well-known outer ring of star formation at a radius of ten kiloparsecs whose centre is offset from the galaxy nucleus. In addition, the outer galaxy disk is warped, as seen at both optical and radio wavelengths. The halo contains numerous loops and ripples. Here we report the presence of a second, inner dust ring with projected dimensions of 1.5 x 1 kiloparsecs and offset by about half a kiloparsec from the centre of the galaxy (based upon an analysis of previously-obtained data). The two rings appear to be density waves propagating in the disk. Numerical simulations indicate that both rings result from a companion galaxy plunging through the centre of the disk of M31. The most likely interloper is M32. Head-on collisions between galaxies are rare, but it appears nonetheless that one took place 210 million years ago in our Local Group of galaxies.     

Study on the Relation between the Drape of Fabrics and Its Revolving Speed

Based on the tests of eight kinds of typical fabrics, the relation between the drape coefficient of different fabrics and its revolving speed was analyzed and discussed. The result of regression curve fitting of experimental data showed that the relation between drape coefficient of fabric and its revolving speed could be expressed by negative exponential equation. Meanwhile, the difference of drape coefficients between static and dynamic at 100 - ISOr.p.m was suggested to be one of the expressing parameters of the lively degree of fabric dynamic drape.     

The discovery of a galaxy-wide superwind from a young massive galaxy at redshift z approximately 3

High-velocity galactic outflows, driven by intense bursts of star formation and black hole accretion, are processes invoked by current theories of galaxy formation to terminate star formation in the most massive galaxies and to deposit heavy elements in the intergalactic medium. From existing observational evidence (for high-redshift galaxies) it is unclear whether such outflows are localized to regions of intense star formation just a few kiloparsecs in extent, or whether they instead have a significant impact on the entire galaxy and its surroundings. Here we present two-dimensional spectroscopy of a star-forming galaxy at redshift z = 3.09 (seen 11.5 gigayears ago, when the Universe was 20 per cent of its current age): its spatially extended Lyalpha line emission appears to be absorbed by H i in a foreground screen covering the entire galaxy, with a lateral extent of at least 100 kpc and remarkable velocity coherence. This screen was ejected from the galaxy during a starburst several 10(8) years earlier and has subsequently swept up gas from the surrounding intergalactic medium and cooled. This demonstrates the galaxy-wide impact of high-redshift superwinds.     

The suppression of star formation by powerful active galactic nuclei

The old, red stars that constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly as a result of accretion onto black holes. It is widely suspected, but unproved, that the tight correlation between the mass of the black hole and the mass of the stellar bulge results from the AGN quenching the surrounding star formation as it approaches its peak luminosity. X-rays trace emission from AGN unambiguously, whereas powerful star-forming galaxies are usually dust-obscured and are brightest at infrared and submillimetre wavelengths. Here we report submillimetre and X-ray observations that show that rapid star formation was common in the host galaxies of AGN when the Universe was 2-6 billion years old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 10(44) ergs per second. This suppression of star formation in the host galaxy of a powerful AGN is a key prediction of models in which the AGN drives an outflow, expelling the interstellar medium of its host and transforming the galaxy's properties in a brief period of cosmic time.     

暗物质之迷

由星系团的运行速度观测而推测出来的宇宙中含有大量暗物质的理论似乎获得了大部分物理学界和天文学界的人的认同。而我却不认同此理论,因为事实上并不存大大量的暗物质,只要将整个星系的各个恒星对星系边沿的恒星的万有引力重新逐个计算并统计引力效应就能得到边沿恒星绕行所需要的引力值。使得万有引力的增大的原因在于临边陡增效应和力桥效应,并由此提出了万有引力新的表述。     

The massive binary companion star to the progenitor of supernova 1993J

The massive star that underwent a collapse of its core to produce supernova (SN)1993J was subsequently identified as a non-variable red supergiant star in images of the galaxy M81 taken before explosion. It showed an excess in ultraviolet and B-band colours, suggesting either the presence of a hot, massive companion star or that it was embedded in an unresolved young stellar association. The spectra of SN1993J underwent a remarkable transformation from the signature of a hydrogen-rich type II supernova to one of a helium-rich (hydrogen-deficient) type Ib. The spectral and photometric peculiarities were best explained by models in which the 13-20 solar mass supergiant had lost almost its entire hydrogen envelope to a close binary companion, producing a 'type IIb' supernova, but the hypothetical massive companion stars for this class of supernovae have so far eluded discovery. Here we report photometric and spectroscopic observations of SN1993J ten years after the explosion. At the position of the fading supernova we detect the unambiguous signature of a massive star: the binary companion to the progenitor.