Cosmic Information from the Microwave Background & Cosmic Web

来自微波背景的宇宙信息

• 批准号: RGPIN-2017-06954
• 负责人: Bond, Richard
• 金额: $ 2.19万
• 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: 2017
• 资助国家: 加拿大
• 起止时间: 2017-01-01 至 2018-12-31
• 项目状态: 已结题
• 来源: https://www.nserc-crsng.gc.ca/ase-oro/Details-Detailles_eng.asp?id=633179
• 关键词: Cosmic; Information; Microwave; Background; Web

Over the past 35 years (!) my group has shown that primary cosmic background radiation (CMB) anisotropies are the key observables for elucidating the correct structure formation theory, and precision values of cosmological parameters that define it, such as the dark energy, dark matter, baryon and neutrino densities, the amplitude and slope of the spectrum of primordial fluctuations, including gravity waves, the average spatial curvature of the Universe, early and late inflation constraints, including on primordial non-Gaussianities in the spatial curvature. I have been involved in Planck since 1993, as a Planck coI and Canadian Space Agency PI since 2001. Analyzing our Planck results has been my primary focus over the past grant cycle, with major releases of data products and results in 2011, 2013 and 2015, and more work for the next 2017 releases, and beyond): our Canadian group has had a major impact on the cornucopia of influential Planck papers covering all of the cosmological topics listed above. Our Chile-based Atacama CMB Cosmology telescope extended the results to higher resolution. Over the next five years the outpouring of cosmic data will greatly enhance, from CMB and large scale structure (LSS) and other probes, including much more from secondary CMB anisotropies involving nonlinear physics. My group will be in the thick of it, as team members on LSS surveys (the redshifted-21cm BAO experiment CHIME, carbon monoxide and CII intensity mapping experiments, ESA’s EUCLID), as well as CMB experiments (the balloon-borne Spider, since 2005, Advanced ACTpol followed by the Simons Observatory and then the ambitious DOE-based CMB Stage 4).

在过去的35年里，我的团队已经证明，主要宇宙背景辐射（CMB）的各向异性是解释正确结构形成理论的关键观测值，以及定义它的宇宙学参数的精确值，如暗能量、暗物质、重子和中微子密度、包括引力波在内的原始波动光谱的振幅和斜率、宇宙的平均空间曲率、早期和晚期膨胀约束、包括空间曲率中的原始非高斯性。自1993年以来，我一直参与普朗克的工作，从2001年开始担任普朗克的coI和加拿大航天局的PI。在过去的资助周期中，分析我们的普朗克结果一直是我的主要关注点，在2011年、2013年和2015年发布了主要的数据产品和结果，并在2017年及以后发布了更多的工作)：我们的加拿大团队对涵盖上述所有宇宙学主题的有影响力的普朗克论文的聚宝堆产生了重大影响。我们位于智利的阿塔卡马CMB宇宙望远镜将结果扩展到更高的分辨率。在接下来的五年里，来自CMB和大尺度结构（LSS）以及其他探测器的宇宙数据将大大增加，包括更多来自涉及非线性物理的次级CMB各向异性的数据。作为LSS调查（红移21厘米BAO实验CHIME，一氧化碳和CII强度测绘实验，欧空局EUCLID）以及CMB实验（自2005年以来的气球载蜘蛛，高级ACTpol，随后是西蒙斯天文台，然后是雄心勃勃的基于do的CMB阶段4）的团队成员，我的小组将参与其中。