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Astrophysical signatures of dark matter: its nature, the structure of haloes, and galaxy formation

暗物质的天体物理特征：它的性质、晕的结构和星系的形成

基本信息

批准号：
48411036
负责人：
Privatdozent Dr. Volker Müller, since 3/2009
金额：
--
依托单位：
Leibniz-Institut für Astrophysik Potsdam (AIP)
依托单位国家：
德国
项目类别：
Research Grants
财政年份：
2007
资助国家：
德国
起止时间：
2006-12-31 至 2012-12-31
项目状态：
已结题

来源：
https://gepris.dfg.de/gepris/projekt/48411036?language=en
关键词：
Astrophysical signatures dark matter its

项目摘要

One of the most remarkable achievements of modern cosmology is the measurement of the fundamental constituents of the Universe. It is now well established that ordinary matter can only account for a mere 4 per cent of the total energy density. The vast majority (about three quarters) is believed to be in the form of a mysterious “dark energy”, while the remaining 21 per cent is composed of so-called “dark matter” particles.Yet, despite the ever increasing amount of astrophysical and cosmological evidence for its existence, dark matter has so far eluded direct detection in particle accelerators and recoil experiments. Thanks to the recent advances in instrumentation, indirect detection through the emission of radiation and relativistic particles has emerged as an interesting alternative, and many theoretical studies have been devoted to investigate the conditions under which dark matter particles would effectively become “visible”.The somewhat surprising conclusion of most of these works is that signatures are indeed expected on astrophysical scales, and in most cases they are within reach of present (INTEGRAL, COMPTEL/EGRET) or planned (GLAST, Planck) observatories. In fact, current data can already impose constraints on both the physical properties of dark matter and on its distribution within galaxies. It is the aim of the present project to make a systematic study of the emission expected for different dark matter models, its detectability by present and forthcoming instruments, and its possible impact on galaxy formation and evolution, in an attempt to address the basic question “What is dark matter?”.

现代宇宙学最显著的成就之一是对宇宙基本成分的测量。现在已经确定，普通物质只能占总能量密度的4%。绝大多数（约四分之三）被认为是一种神秘的“暗能量”，而剩下的21%是由所谓的“暗物质”粒子组成的。然而，尽管有越来越多的天体物理学和宇宙学证据证明暗物质的存在，但迄今为止，暗物质还没有在粒子加速器和反冲实验中被直接探测到。由于最近仪器的进步，通过发射辐射和相对论性粒子的间接探测已经成为一种有趣的选择，许多理论研究已经致力于调查暗物质粒子有效地“可见”的条件。这些工作的一个有点令人惊讶的结论是，在天体物理尺度上的特征确实是预期的，而且在大多数情况下，它们在现有（INTEGRAL, COMPTEL/EGRET）或计划（GLAST, Planck）天文台的范围内。事实上，目前的数据已经可以对暗物质的物理性质及其在星系中的分布施加限制。本项目的目的是对不同暗物质模型的预期发射，现有和即将问世的仪器的可探测性，以及它对星系形成和演化的可能影响进行系统研究，试图解决“什么是暗物质？”这个基本问题。