Theory and Analysis of Cosmic Web Observables

宇宙网可观测理论与分析

• 批准号: RGPIN-2019-07306
• 负责人: Bond, Richard
• 金额: $ 2.99万
• 依托单位: University of Toronto
• 依托单位国家: 加拿大
• 项目类别: Discovery Grants Program - Individual
• 财政年份: 2022
• 资助国家: 加拿大
• 起止时间: 2022-01-01 至 2023-12-31
• 项目状态: 已结题
• 来源: https://www.nserc-crsng.gc.ca/ase-oro/Details-Detailles_eng.asp?id=746480
• 关键词: Theory; Analysis; Cosmic; Web; Observables

This research will develop theoretical frameworks and analysis tools for the tremendous outpouring of Cosmic Microwave Background (CMB) and Large Scale Structure (LSS) and galaxy formation data that will arise over 2019-2024 period, and beyond. The 2012-18 period has been amazing, solidifying a Standard Model of Cosmology (SMc) dominated by dark energy and dark matter at high precision, in large part through our activities on the Planck CMB satellite team and the higher resolution Atacama Cosmology Telescope (ACT) team. The impact was recently recognized by the 2018 Gruber Prize in Cosmology to our Planck group for providing "the definitive description of the universe on the largest and smallest scales." CMB and LSS: This proposal emphasizes planned work on Advanced ACTPol and the Simons Observatory follow-on, the related CCATprime telescope, a second flight of the balloon-borne Spider experiment, cross-correlation work of the CMB with the LSS space experiment Euclid and other ground-based LSS surveys, and various three-dimensional line intensity mapping (LIM) experiments probing galaxy formation and assembly. A primary motivation is to find new physics beyond the standard model of cosmology (BSMc). BSMc projects include how to measure whether dark energy is coupled to matter, whether quantum aspects of dark matter are observable, and to create statistical tests for novel non-Gaussian primordial structures generated in the early Universe.  Gravity Waves and Interstellar Dust Polarization: A major CMB target is to discover early-Universe gravity waves with CMB polarization. The greatest challenge is separating polarized Galactic emissions from what is truly primordial. For this we are developing novel re-mapping measures of anisotropy in the "Milky Way's interstellar web" polarized emissions. Line Intensity Mapping is an emerging technique to map large cosmological volumes to probe the Epoch of Galaxy Assembly and even of the pre-galactic cosmic dawn. The Canadian CHIME radio telescope targeting the 21cm line of hydrogen and COMAP in California, targeting a carbon monoxide line, are now taking data, and CCATprime, targeting ionized carbon, is under construction. Our group at CITA is engaging in all of the analytical and theoretical challenges that will arise from these vast new data sources, including any new BSMc physics that might emerge. Theory and Simulations: We will create ensembles of rapidly-computable yet accurate SMc and BSMc mock simulations we call webskys for cross-analyses, since all of these big-sky experiments are entangled in one fully correlated light-cone, and must ultimately be analyzed together. This is a challenge because of complex gas processes, but the webskys we construct will learn from the highest resolution gasdynamical feedback simulations. HQP: Such work has been and is well suited for engagement of HQP locally at all levels at CITA: Senior RAs and postdocs, graduate and undergraduate research students.

这项研究将开发理论框架和分析工具，用于宇宙微波背景（CMB）和大规模结构（LSS）和银河形成数据的巨大浇注，这些框架将在2019 - 2024年及以后产生。 2012 - 18年度的时期令人惊叹，巩固了以深色和暗物质为主导的标准宇宙学模型（SMC），这在很大程度上是通过我们在Planck CMB CMB卫星团队和更高分辨率Atacama宇宙学望远镜（ACT）团队的活动中进行的。最近，2018年格鲁伯宇宙学奖给我们的普朗克集团（Granck Group）提供了“最大和最小规模的宇宙的确定描述”，这一影响最近得到了认可。 CMB和LSS：该提案强调了对高级ACTPOL和SIMONS观测值跟踪的计划工作编队和组装。主要动机是在宇宙学标准模型（BSMC）之外找到新的物理学。 BSMC项目包括如何衡量是否可以观察到暗物质的量子方面，并为早期宇宙中产生的新型非高斯原始结构进行统计测试。重力波和星际尘埃极化：一个主要的CMB靶标是发现具有CMB极化的早期近亲重力波。最大的挑战是将两极化的银河排放与真正原始的排放分开。为此，我们正在开发“银河系星际网络”两极分化的新型各向异性的重新映射措施。线强度映射是一种新兴技术，用于绘制大型宇宙学量，以探测星系组装的时期，甚至是半乳酸前宇宙黎明的时期。针对加利福尼亚州21厘米的氢和Comap的加拿大钟声射电望远镜，以一氧化碳线为目标，目前正在获取数据，而靶向电离碳的CCATPRIME正在建设中。我们在CITA的小组正在参与这些庞大的新数据源将引起的所有分析和理论挑战，包括任何可能出现的新BSMC物理学。理论和模拟：我们将创建迅速计算但准确的SMC和BSMC模拟模拟的合奏，我们称为跨分析的Webskys，因为所有这些大型的大型实验都纠缠在一个完全相关的轻频率中，并且必须最终一起分析。这是一个挑战，因为复杂的气体过程，但是我们构建的Webskys将从最高的分辨率气体反馈模拟中学习。 HQP：此类工作曾经并且非常适合在CITA的各个级别的HQP参与：高级RAS和Postdocs，研究生和本科研究专业的学生。