Seeing Dark Matter with Weak Gravitational Lensing

用弱引力透镜观察暗物质

• 批准号: RGPIN-2019-04265
• 负责人: Hudson, Michael
• 金额: $ 2.99万
• 依托单位: University of Waterloo
• 依托单位国家: 加拿大
• 项目类别: Discovery Grants Program - Individual
• 财政年份: 2021
• 资助国家: 加拿大
• 起止时间: 2021-01-01 至 2022-12-31
• 项目状态: 已结题
• 来源: https://www.nserc-crsng.gc.ca/ase-oro/Details-Detailles_eng.asp?id=737518
• 关键词: Seeing; Dark; Matter; Weak; Gravitational

Dark matter (DM) is the dominant form of matter in the Universe, yet it remains poorly understood empirically due to the difficulty in directly measuring its properties. An understanding of DM and its link to visible matter is also critical for disentangling the puzzles of galaxy formation, since DM forms the structural framework of halos and filaments within which the visible parts of galaxies form and evolve. Weak gravitational lensing (WL) has emerged as one of the most promising ways to measure the quantity and spatial distribution of dark matter. The Canada-France Imaging Survey (CFIS) has exceptional power (due to its overlap with the Sloan Digital Sky Survey) for science that combines WL with galaxy spectroscopic redshifts. This combination of WL and spectroscopy is unique in the international context and allows studies of dark matter that no other survey can achieve. I am the Lead Scientist of the r-band (WL) component of CFIS, and lead of the international CFIS WL team. This proposal has two primary scientific objectives. The first objective is to map and characterize the fine details of dark matter structure in haloes and filaments. To meet these goals, my group will use CFIS data to study the dark matter structures in previously unexplored regimes of density or environment: (1) in between galaxies, in the form of filaments of the cosmic web; (2) in tidally stripped halos of satellites (3) the shapes of dark matter haloes and their connection to the large-scale environment. The second objective is to test General Relativity (GR) and the cosmological model on large scales. My group will compare the deflection of light with the infall of galaxies into structures: by combining CFIS WL with SDSS redshift data, we will perform the most stringent test to date. We will measure the relationship between matter and galaxies and gravity on the largest scales and in the nearby Universe through comparisons of large-scale structure and peculiar velocities. WL is the driver behind several billion dollar scale projects (the Euclid satellite, the Large Synoptic Survey Telescope), which promise orders of magnitude increases in lensing power when they begin in the early-to-mid 2020s. The experience gained through CFIS will put my group in an exceptional position to exploit these new surveys in this new golden age of weak gravitational lensing.

暗物质（DM）是宇宙中物质的主要形式，但由于难以直接测量其性质，因此在经验上仍然差了解。对DM及其与可见物质的联系的理解对于解开星系形成的难题也至关重要，因为DM构成了光环和细丝的结构框架，其中星系的可见部分形成和进化。 弱重力镜头（WL）已成为测量暗物质数量和空间分布的最有希望的方法之一。加拿大法国成像调查（CFIS）具有与Galaxy Spectroscopic Redshifts相结合的科学科学的特色（由于与Sloan Digital Sky的重叠）。 WL和光谱法的这种结合在国际背景下是独一无二的，允许对其他调查无法实现的暗物质进行研究。我是CFI的R波段（WL）组成部分的首席科学家，也是国际CFIS WL团队的负责人。该提议有两个主要的科学目标。第一个目标是映射和表征光环和细丝中暗物质结构的细节。为了实现这些目标，我的小组将使用CFIS数据研究以前未开发的密度或环境制度中的暗物质结构：（1）在星系之间，以宇宙网络的细丝的形式； （2）在潮汐剥离的卫星光环中（3）暗物质光环的形状及其与大规模环境的联系。第二个目标是在大尺度上测试一般相对论（GR）和宇宙学模型。我的小组将将光的挠度与星系中的偏转与结构进行比较：通过将CFIS WL与SDSS红移数据相结合，我们将执行迄今为止最严格的测试。我们将通过比较大规模结构和特殊的速度来衡量物质与星系之间的关系以及在最大尺度和附近宇宙中的重力之间的关系。 WL是数十亿美元量表项目（Euclid卫星，大型的概要调查望远镜）的背后驾驶员，该项目在2020年代初期开始时承诺，镜头能力的数量级会增加。通过CFI获得的经验将使我的小组处于杰出的位置，以在这个新的重力镜头的黄金时代中利用这些新调查。