The relationship between the formation of galaxies and large-scale structures

星系的形成与大尺度结构的关系

• 批准号: PP/E005306/1
• 负责人: Duncan Farrah
• 金额: $ 50.26万
• 依托单位: University of Sussex
• 依托单位国家: 英国
• 项目类别: Fellowship
• 财政年份: 2007
• 资助国家: 英国
• 起止时间: 2007 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=PP%2FE005306%2F1
• 关键词: relationship; between; formation; galaxies; large

When we look up at the night sky, we see that galaxies seem to be arranged in a particular way. One might expect that galaxies would be distributed randomly, much as grains of sand would if you threw a handful across the floor, but instead, they seem to trace elegant structures; galaxy clusters are connected to each other by long filaments, interspersed with large voids, where few or no galaxies are seen. The reason why galaxies are arranged this way is deeply mysterious; we know that, when the Universe was very young, it was a very smooth, even place, so how did the Universe go from being homogeneous and smooth just after the Big Bang to the clumpy, clustered, irregularly structured Universe we see today? A second problem, concerns how bright and active we see galaxies to be. Nearby galaxies are quiet, placid things where not an awful lot happens; at most a few stars are born and a few die each year. For galaxies a long long way away, things are completely different; they are much more violent - forming hundreds, if not thousands of new stars each year - and are many hundreds of times brighter than local galaxies. Furthermore, these distant galaxies seem to be colliding with each other much more frequently than galaxies nearby us, and it is suspected that these galaxy collisions are in some way responsible for their huge star formation rates. The central puzzle remains though; why is the Universe nearby to us such a quiet, unassuming place, while the distant Universe is so violent and active? In recent years, astronomers have started to suspect that the answer to both these questions may lie in the same place, namely the mysterious and poorly understood `dark' matter. Dark matter is so called because it has the singularly disobliging tendency not to emit any light at all, at any wavelength, which makes it impossible to see with conventional telescopes. If however we look at the way stars move in galaxies, we can see that there must be an awful lot of dark matter in these galaxies (something like ten times the mass of visible matter), as we can see the dark matter pulling the stars around. We might suspect that this dark matter may have something to do with how galaxies are distributed on the sky, simply because there's so much of it. We might also expect that galaxies should trace the dark matter, with more galaxies occurring in regions of more dark matter and vice versa, because dark matter is comprised, in part, of the gas and dust from which stars are formed. So, if we want to work out why galaxies trace the structures they do, or how galaxies are formed, we must work out how galaxies trace the underlying dark matter, and how this dark matter affects galaxy formation. This is one of the most important problems in astronomy today, as it literally underpins everything we see. A series of new telescopes hold the promise of a revolution in our understanding of how galaxies, and clusters and filaments, form. The goal of the fellowship will be to combine data from these new facilities with the latest computer models and simulations, to make great strides in our understanding of galaxy and structure formation. Work using optical data will focus on how the stars in very distant galaxies are assembled. Does it happen gradually or all at once? When during the history of the Universe do most stars in galaxies form? What parts of the Universe will eventually become the densest galaxy clusters we see nearby us, and which will become large, empty voids? Work in the infrared on the other hand will focus on galaxies with huge bursts of star formation - these are thought to be the formation events of some of the biggest galaxies in the Universe. By studying how these distant infrared bright galaxies are grouped on the sky, and exactly how the star formation within them is occurring, I will relate how and when they form to the dark matter that surrounds them.

当我们仰望夜空时，我们看到星系似乎是以一种特殊的方式排列的。人们可能会认为星系会随机分布，就像你在地板上扔一把沙子一样，但相反，它们似乎描绘了优雅的结构;星系团通过长长的细丝相互连接，散布着大空洞，很少或根本看不到星系。星系以这种方式排列的原因是非常神秘的;我们知道，当宇宙非常年轻时，它是一个非常平滑的地方，那么宇宙是如何从大爆炸后的均匀和平滑变成我们今天看到的混乱，集群，不规则结构的宇宙的呢？第二个问题是，我们看到的星系有多明亮和活跃。附近的星系是安静的，平静的东西，没有太多的事情发生;每年最多有几颗恒星诞生，也有几颗恒星死亡。对于遥远的星系来说，情况完全不同;它们更加猛烈-每年形成数百颗，如果不是数千颗的话-并且比本地星系亮数百倍。此外，这些遥远的星系似乎比我们附近的星系更频繁地相互碰撞，人们怀疑这些星系碰撞在某种程度上是它们巨大的星星形成率的原因。然而，核心的谜团仍然存在;为什么我们附近的宇宙是如此安静，谦逊的地方，而遥远的宇宙是如此暴力和活跃？近年来，天文学家开始怀疑这两个问题的答案可能都在同一个地方，即神秘而又知之甚少的“暗”物质。暗物质之所以被称为暗物质，是因为它有一种奇怪的不情愿的倾向，在任何波长下都不发射任何光，这使得它不可能用传统的望远镜看到。然而，如果我们观察恒星在星系中运动的方式，我们可以看到这些星系中一定有大量的暗物质（大约是可见物质质量的十倍），因为我们可以看到暗物质拉着恒星。我们可能会怀疑这些暗物质可能与星系在天空中的分布有关，仅仅是因为它们太多了。我们也可能会认为星系应该跟踪暗物质，更多的星系出现在暗物质更多的区域，反之亦然，因为暗物质部分由气体和尘埃组成，恒星就是从这些气体和尘埃形成的。所以，如果我们想弄清楚为什么星系会追踪它们的结构，或者星系是如何形成的，我们必须弄清楚星系是如何追踪潜在的暗物质的，以及暗物质如何影响星系的形成。这是当今天文学中最重要的问题之一，因为它确实支撑着我们所看到的一切。一系列新的望远镜有望为我们理解星系、星系团和星系丝的形成带来一场革命。该奖学金的目标将是将这些新设施的联合收割机数据与最新的计算机模型和模拟相结合，在我们对星系和结构形成的理解方面取得重大进展。使用光学数据的工作将集中在非常遥远的星系中的恒星是如何聚集的。它是逐渐发生的还是突然发生的？在宇宙的历史中，星系中的大多数恒星是什么时候形成的？宇宙的哪些部分最终会变成我们在附近看到的密集的星系团，哪些会变成巨大的空洞？另一方面，红外线的工作将集中在具有巨大的星星形成爆发的星系上--这些被认为是宇宙中一些最大星系的形成事件。通过研究这些遥远的红外明亮星系是如何在天空中分组的，以及它们内部的星星是如何形成的，我将把它们如何以及何时形成与它们周围的暗物质联系起来。

项目成果

MID-INFRARED SPECTROSCOPY OF CANDIDATE ACTIVE GALACTIC NUCLEI-DOMINATED SUBMILLIMETER GALAXIES

候选活动星系核主导的亚毫米星系的中红外光谱

• DOI: 10.1088/0004-637x/713/1/503
• 发表时间: 2010
• 期刊: The Astrophysical Journal
• 作者: Coppin K

A SPITZER HIGH-RESOLUTION MID-INFRARED SPECTRAL ATLAS OF STARBURST GALAXIES

斯皮策星暴星系高分辨率中红外光谱图集

• DOI: 10.1088/0067-0049/184/2/230
• 发表时间: 2009
• 期刊: The Astrophysical Journal Supplement Series
• 作者: Bernard-Salas J

Herschel unveils a puzzling uniformity of distant dusty galaxies

• DOI: 10.1051/0004-6361/201014687
• 发表时间: 2010-05
• 期刊: Astronomy and Astrophysics
• 影响因子: 6.5
• 作者: D. Elbaz;H. Hwang;B. Magnelli;E. Daddi;H. Aussel;B. Altieri;A. Amblard;P. Andreani;V. Arumugam;R. Auld;T. Babbedge;S. Berta;A. Blain;J. Bock;J. Bock;Á. Bongiovanni;A. Boselli;V. Buat;D. Burgarella;N. Castro-RodrÍguez;A. Cava;J. Cepa;P. Chanial;R. Chary;A. Cimatti;D. Clements;A. Conley;L. Conversi;A. Cooray;A. Cooray;M. Dickinson;H. Dominguez;C. Dowell;C. Dowell;J. Dunlop;E. Dwek;S. Eales;D. Farrah;N. F. Schreiber;M. Fox;A. Franceschini;W. Gear;R. Genzel;J. Glenn;M. Griffin;C. Gruppioni;M. Halpern;E. Hatziminaoglou;E. Ibar;K. Isaak;R. Ivison;R. Ivison;G. Lagache;D. L. Borgne;E. Floc’h;L. Levenson;L. Levenson;N. Lu;D. Lutz;S. Madden;B. Maffei;G. Magdis;G. Mainetti;R. Maiolino;L. Marchetti;A. Mortier;Hien Nguyen;Hien Nguyen;R. Nordon;B. O’Halloran;K. Okumura;S. Oliver;A. Omont;M. Page;P. Panuzzo;A. Papageorgiou;C. Pearson;C. Pearson;I. Fournón;A. P. Garćıa;A. Poglitsch;M. Pohlen;P. Popesso;F. Pozzi;J. Rawlings;D. Rigopoulou;D. Rigopoulou;L. Riguccini;D. Rizzo;G. Rodighiero;I. Roseboom;M. Rowan‐Robinson;A. Saintonge;M. S. Portal;P. Santini;M. Sauvage;B. Schulz;D. Scott;N. Seymour;Lijing Shao;D. Shupe;Anthony J. Smith;J. Stevens;E. Sturm;M. Symeonidis;L. Tacconi;M. Trichas;K. Tugwell;Mattia Vaccari;I. Valtchanov;J. Vieira;L. Vigroux;L. Wang;R. Ward;G. Wright;C. Xu;M. Zemcov;M. Zemcov

AzTEC half square degree survey of the SHADES fields â?? I. Maps, catalogues and source counts

AzTEC SHADES 场的半平方度调查 – ??

• DOI: 10.1111/j.1365-2966.2009.15620.x
• 发表时间: 2010
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Austermann J

HerMES: Halo occupation number and bias properties of dusty galaxies from angular clustering measurements

HerMES：来自角聚类测量的尘埃星系的晕占据数和偏差特性

• DOI: 10.1051/0004-6361/201014597
• 发表时间: 2010
• 期刊: Astronomy and Astrophysics
• 影响因子: 6.5
• 作者: Cooray A