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（！）我的小组已经证明，初级宇宙背景辐射（CMB）各向异性是阐明正确的结构形成理论以及定义它的宇宙学参数的精确值（例如暗能量）的关键可观测值、暗物质、重子和中微子密度、原始波动频谱的幅度和斜率，包括重力波、宇宙的平均空间曲率、早期和晚期膨胀我自 1993 年以来一直参与普朗克研究，自 2001 年起担任普朗克学院和加拿大航天局 PI。分析我们的普朗克结果一直是我在过去的资助周期中的主要关注点。 2011年、2013年和2015年数据产品和结果的主要版本，以及2017年下一个版本的更多工作，以及超越）：我们的加拿大小组对涵盖上述所有宇宙学主题的有影响力的普朗克论文产生了重大影响，我们位于智利的阿塔卡马宇宙微波背景宇宙学望远镜在接下来的五年中将结果扩展到了更高的分辨率。来自 CMB 和大尺度结构 (LSS) 和其他探测器的宇宙数据将大大增强，包括更多来自涉及非线性物理的次级 CMB 各向异性。 LSS 巡天的成员（红移 21 厘米 BAO 实验 CHIME、一氧化碳和 CII 强度绘图实验、ESA 的 EUCLID）以及 CMB 实验（气球载蜘蛛，自 2005 年以来，高级 ACTpol，随后是西蒙斯天文台，然后是雄心勃勃的基于能源部的 CMB 第 4 阶段）。