MSIP: Innovation to Achieve the Full Science Reach of the BICEP Array Stage 3 CMB Polarization Experiment

MSIP：实现 BICEP 阵列第 3 阶段 CMB 极化实验全面科学成果的创新

• 批准号: 1836010
• 负责人: Chao-Lin Kuo
• 金额: $ 767.31万
• 依托单位: Stanford University
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2018
• 资助国家: 美国
• 起止时间: 2018-10-01 至 2024-09-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1836010&HistoricalAwards=false
• 关键词: MSIP; Innovation; Achieve; Full; Science

Scientists funded by this program develop advanced millimeter-wave instruments to conduct observations from the U.S. South Pole Station to study properties of the early Universe. The main goal of the project is to test the inflationary theory, a remarkable idea that the entire observable Universe began in a violently accelerated expansion of a microscopic volume. Along the way, superconducting detector technology and our knowledge on astronomical emission will be significantly advanced. The specific feature being pursued is a tiny swirly polarization pattern in the cosmic microwave background (CMB) radiation, the 2.7-Kelvin afterglow of the Big Bang. Scientists involved in this program will design and build a telescope populated with more than 20 thousand state-of-the-art superconducting sensors, and field it to the South Pole station -- the driest place on Earth. The research activities will provide excellent opportunities for training of graduate students and postdocs. In addition, there is a set of outreach goals aiming at the public audience: (1) Providing middle and high school teachers with the training and tools they need to inspire students to pursue STEM via the Research Experiences for Teachers program at Stanford; (2) Inspiring the faculty, postdocs, and graduate students engaged in the proposed work to be effective science communicators with well-organized workshops, and (3) Enabling broad access to some of the most fascinating, but difficult, concepts that underlie modern cosmology by creating a set of animations. The team will use the BICEP Array and SPT-3G data to produce cutting-edge measurements of CMB polarization. Data from this new system will be used to discriminate the dust emission from our own Galaxy and the primordial CMB signal. The program consists of three parts: (1) Development of a 22,000-detector 220/270GHz receiver to complete the BICEP Array. The required high detector count is enabled by a new technology?microwave SQUID multiplexers; (2) Implementation of delensing analysis in conjunction with SPT-3G; (3) Improvements to the control of instrumental systematics. In addition to the main science goal of constraining inflation, the high-frequency receiver will dramatically improve understanding of polarized Galactic dust emission. Also, BICEP Array combined with SPT-3G is a pathfinder towards the CMB-S4 initiative to build an "ultimate" Stage 4 CMB polarization experiment.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.

由该计划资助的科学家开发先进的毫米波仪器，从美国南极站进行观测，研究早期宇宙的性质。 该项目的主要目标是测试暴胀理论，这是一个了不起的想法，即整个可观测的宇宙开始于微观体积的剧烈加速膨胀。 沿着这条路，超导探测器技术和我们对天文辐射的认识将得到显著的进步。 正在研究的具体特征是宇宙微波背景辐射（CMB）中的一个微小的漩涡偏振模式，即大爆炸的2.7开尔文余辉。 参与该计划的科学家将设计和建造一个装有2万多个最先进的超导传感器的望远镜，并将其放置在南极站-地球上最干燥的地方。 研究活动将为培养研究生和博士后提供极好的机会。 此外，还有一套针对公众的推广目标：（1）通过斯坦福大学的教师研究经验计划，为初中和高中教师提供他们所需的培训和工具，以激励学生追求STEM;（2）通过精心组织的研讨会，使从事拟议工作的教师、博士后和研究生成为有效的科学传播者，以及（3）通过创建一组动画，使人们能够广泛接触到现代宇宙学中一些最迷人但最困难的概念。 该团队将使用BICEP阵列和SPT-3G数据来进行CMB偏振的尖端测量。 来自这个新系统的数据将被用来区分来自我们银河系的尘埃排放和原始CMB信号。 该计划包括三个部分：（1）开发一个22，000探测器的220/270 GHz接收机，以完成BICEP阵列。 所需的高探测器数量是由一种新技术实现的？微波SQUID多路复用器（2）结合SPT-3G进行去透镜分析;（3）改进仪器分类学的控制。 除了限制膨胀的主要科学目标外，高频接收器还将大大提高对极化银河尘埃发射的理解。 此外，BICEP阵列与SPT-3G相结合，是CMB-S4计划的开拓者，该计划旨在建立一个“终极”第4阶段CMB极化实验。该奖项反映了NSF的法定使命，并通过使用基金会的知识价值和更广泛的影响审查标准进行评估，被认为值得支持。

项目成果

Thermal testing for cryogenic CMB instrument optical design

低温 CMB 仪器光学设计的热测试

• DOI: 10.1117/12.2629490
• 发表时间: 2022
• 期刊: Proceedings of the SPIE
• 作者: Goldfinger, David C.;Ade, Peter A.;Ahmed, Zeeshan;Amiri, Mandana;Barkats, Denis;Basu Thakur, Ritoban;Beck, Dominic;Bischoff, Colin A.;Bock, James J.;Buza, Victor
• 通讯作者: Buza, Victor

A demonstration of improved constraints on primordial gravitational waves with delensing

通过去透镜改进对原初引力波的约束的演示

• DOI: 10.1103/physrevd.103.022004
• 发表时间: 2021
• 期刊: Physical Review D
• 影响因子: 5
• 作者: Ade, P. A. R.;Ahmed, Z.;Amiri, M.;Anderson, A. J.;Austermann, J. E.;Avva, J. S.;Barkats, D.;Thakur, R. Basu;Beall, J. A.;Bender, A. N.
• 通讯作者: Bender, A. N.

BICEP/Keck. XVII. Line-of-sight Distortion Analysis: Estimates of Gravitational Lensing, Anisotropic Cosmic Birefringence, Patchy Reionization, and Systematic Errors

二头肌/凯克。

• DOI: 10.3847/1538-4357/acc85c
• 发表时间: 2023
• 期刊: The Astrophysical Journal
• 作者: Ade, P. A. R.;Ahmed, Z.;Amiri, M.;Barkats, D.;Thakur, R. Basu;Bischoff, C. A.;Beck, D.;Bock, J. J.;Boenish, H.;Bullock, E.
• 通讯作者: Bullock, E.

2022 upgrade and improved low frequency camera sensitivity for CMB observation at the South Pole

2022年升级并提高了南极CMB观测的低频相机灵敏度

• DOI: 10.1117/12.2628058
• 发表时间: 2022
• 期刊: Proceedings of the SPIE
• 作者: Soliman, Ahmed;Ade, P.A.R.;Ahmed, Z.;Amiri, M.;Barkats, D.;Basu Thakur, R.;Bischoff, C.A.;Beck, D.;Bock, J.J.;Buza, V.
• 通讯作者: Buza, V.

BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen

• DOI: 10.3847/1538-4357/acb64c
• 发表时间: 2022-10
• 期刊: The Astrophysical Journal
• 作者: B. C. P. Ade;Z. Ahmed;M. Amiri;D. Barkats;R. Thakur;D. Beck;C. Bischoff;J. Bock;H. Boenish;E. Bullock;V. Buza;IV J.R.Cheshire;S. Clark;J. Connors;J. Cornelison;M. Crumrine;A. Cukierman;E. Denison;M. Dierickx;L. Duband;M. Eiben;S. Fatigoni;J. Filippini;S. Fliescher;C. Giannakopoulos;N. Goeckner-wald;D. Goldfinger;J. Grayson;P. Grimes;G. Halal;G. Hall;M. Halpern;E. Hand;S. Harrison;S. Henderson;S. Hildebrandt;J. Hubmayr;H. Hui;K. Irwin;J. Kang;K. Karkare;E. Karpel;S. Kefeli;S. A. Kernasovskiy;J. Kovac;C. Kuo;K. Lau;E. Leitch;A. Lennox;K. Megerian;L. Minutolo;L. Moncelsi;Y. Nakato;T. Namikawa;H. T. Nguyen;R. O’Brient;IV R.W.Ogburn;S. Palladino;M. Petroff;T. Prouvé;C. Pryke;B. Racine;C. Reintsema;S. Richter;A. Schillaci;B. Schmitt;R. Schwarz;C. Sheehy;B. Singari;A. Soliman;T. S. Germaine;B. Steinbach;R. Sudiwala;G. Teply;K. Thompson;J. Tolan;C. Tucker;A. Turner;C. Umilta;C. Vergés;A. Vieregg;A. Wandui;A. Weber;D. Wiebe;J. Willmert;C. Wong;W.L.K. Wu;H. Yang;K. Yoon;E. Young;C. Yu;L. Zeng;C. Zhang;S. University;Kipacslac;U. Columbia;HarvardCfA;Caltech;U. Cincinnati;S. University;Nasa Jpl;M. I. O. Astrophysics;U. Chicago;U. Minnesota;Nist;Sbt Grenoble;U. I. Urbana-Champaign;H. University;T. U. O. Tokyo;Aix-Marseille Université;Brookhaven National Laboratory