Collaborative Research: Imaging the Beginning of Time from the South Pole: Completing the BICEP Array Survey

合作研究：从南极想象时间的开始：完成 BICEP 阵列调查

• 批准号: 2220445
• 负责人: James Bock
• 金额: $ 232.89万
• 依托单位: California Institute of Technology
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2022
• 资助国家: 美国
• 起止时间: 2022-09-01 至 2027-08-31
• 项目状态: 未结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=2220445&HistoricalAwards=false
• 关键词: Collaborative; Research; Imaging; Beginning; Time

The theory of the "Big Bang" provides an established cosmological model for the origin of our Universe from its earliest known periods through its subsequent large-scale evolution. However, this theory leaves open the question of explaining the initial conditions. Current thoughts are consistent with the entire observable Universe being spawned in a dramatic, exponential "Inflation" of a sub-nuclear volume that lasted about one trillionth of a trillionth of a trillionth of a second. Following this short inflationary period, the Universe continues to expand, but at a less rapid rate. While this basic "Inflationary paradigm" is accepted by most cosmologists, the detailed physics mechanism responsible for inflation is still not known, but there is a testable prediction that this violent space-time expansion would have produced primordial gravitational waves now propagating through the expanding Universe and forming a cosmic gravitational-wave background (CGB). The CGB amplitude defines the energy scale of Inflation that imprints a faint signature in the polarization of the Cosmic Microwave Background (CMB) radiation. Therefore, detecting this polarization signature is arguably the most important goal in cosmology today. This award will continue addressing the oldest question ever posed by mankind "How did the Universe begin?", and it does so via observations made at one of the harshest places on Earth – the Amundsen-Scott South Pole Station in Antarctica. The most recent, community driven Decadal Survey Astro2020 report “Pathways to Discovery in Astronomy and Astrophysics for the 2020s” reaffirmed the importance of search for B-modes polarization signatures of primordial gravitational waves and Inflation, and specifically endorsed the CMB Stage-4 science to be pursued by systematically supported CMB experiments in Antarctica and Chile. The recently released BICEP results place stringent limits on Inflationary models which, for the first time, go well beyond what can be done with temperature data alone, and which rule out two entire classes of previously popular single-field models—natural Inflation and simple monomial potentials. This award aims to complete deployment of all four BICEP Array receivers and then operate them as the Stage-3+ generation observing system. BICEP Array will measure the polarized sky in six frequency bands to reach an ultimate sensitivity to the amplitude of PGW of σ(r) ≲ 0.003, extrapolating from achieved performance, and after conservatively accounting for the Galactic dust, Galactic synchrotron and CMB lensing foregrounds. These measurements will be a definitive test of slow-roll models of Inflation, which generally predict a gravitational-wave signal above approximately r=0.01. BICEP Array will therefore realize the goal set by the NASA/DOE/NSF Task Force for CMB Research in 2005 to achieve sensitivity at this level, and confirmed as “the most exciting quest of all” by the Astro2010, and advance the B-mode search strongly endorsed by the Astro2020 Decadal Survey. The project will continue to provide excellent training for undergraduate and graduate students and postdoctoral fellows including those from underrepresented groups in laboratories that have exceptional track records in this regard. Cosmology and research in Antarctica both capture the public imagination, making this combination a remarkably effective vehicle for stimulating interest in science. This project advances the goals of the NSF Windows on the Universe Big Idea.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.

“大爆炸”的理论为我们宇宙的起源提供了一个既定的宇宙学模型，从已知的早期时期到其随后的大规模演变。但是，该理论打开了解释初始条件的问题。当前的思想与整个可观察到的宇宙相一致，以戏剧性的，指数的“通货膨胀”为核，核糖量的“通货膨胀”持续了大约一万分之一的一秒钟。在这个短期的通货膨胀期之后，宇宙继续扩大，但速度较差。虽然大多数宇宙学家都接受了这种基本的“通货膨胀范式”，但导致通货膨胀的详细物理机制仍然尚不清楚，但是可以检验的预测，这种暴力的时空扩张将产生原始的引力波，如今正在通过扩展的宇宙传播，并形成宇宙膜片背景（CGB）。 CGB放大器定义了通货膨胀的能量尺度，该量表在宇宙微波背景（CMB）辐射的极化中刻有微弱的特征。因此，检测这种极化签名可以说是当今宇宙学中最重要的目标。该奖项将继续解决人类有史以来最古老的问题“宇宙是如何开始的？”，并且通过在地球上最危险的地方之一 - 南极洲的Amundsen-Scott South Pole车站进行的观察。最新的，社区驱动的衰落调查Astro2020报告了“ 2020年代的天文学和天体物理学发现的途径”，重申了寻找B-Modes搜索B-Modes极化签名的重要性，而原始引力波和通货膨胀的极化签名，并特别认可CMB 4阶段科学，以系统地支持CMB Science和CMB的CMB实验。最近发布的二头肌结果对通货膨胀模型进行了严格的限制，这首先​​远远超出了仅使用温度数据所能完成的事情，并且排除了两种以前流行的单场模型的整个类别 - 自然通货膨胀和简单的单一潜力。该奖项旨在完成所有四个二头肌阵列接收器的部署，然后将其作为3阶段+生成观测系统运行。二头肌阵列将在六个频带中测量两极分化的天空，以达到对σ（r）≲0.003的PGW放大器的最终敏感性，从实现的性能中推断出来，并在保守地考虑了银河灰尘，银河系同步子和CMB镜头前景。这些测量值将是对慢速通货膨胀模型的明确检验，该模型通常可以预测高于r = 0.01的重力波信号。因此，二头肌阵列将实现2005年NASA/DOE/NSF工作组为CMB研究设定的目标，以在此级别上实现敏感性，并确认为Astro2010的“最令人兴奋的全部追求”，并通过Astro2020 Decadal decadal decadal decadal decadal decadal decadal decadal necation强烈认可B模式搜索。该项目将继续为本科生和研究生和博士后研究员提供出色的培训，其中包括来自实验室中代表性不足的团体的培训，这些团体在这方面具有出色的记录。南极洲的宇宙学和研究都捕捉到了公众的想象，使这种组合成为激发科学兴趣的非常有效的工具。该项目推动了NSF窗口在宇宙大想法上的目标。该奖项反映了NSF的法定任务，并通过使用基金会的知识分子优点和更广泛的影响审查标准来评估，被认为是珍贵的支持。

项目成果

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

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.

Plastic Laminate Antireflective Coatings for Millimeter-Wave Optics in BICEP Array

BICEP 阵列中毫米波光学器件的塑料层压抗反射涂层

• DOI: 10.1007/s10909-023-02967-1
• 发表时间: 2023
• 期刊: Journal of Low Temperature Physics
• 影响因子: 2
• 作者: Dierickx, M.;Ade, P. A.;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.

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

Bicep/Keck XV: The Bicep3 Cosmic Microwave Background Polarimeter and the First Three-year Data Set

• DOI: 10.3847/1538-4357/ac4886
• 发表时间: 2021-10
• 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;J. Connors;J. Cornelison;M. Crumrine;A. Cukierman;E. Denison;M. Dierickx;L. Duband;M. Eiben;S. Fatigoni;J. Filippini;S. Fliescher;N. Goeckner-wald;D. Goldfinger;J. Grayson;P. Grimes;G. Halal;G. Hall;M. Halpern;E. Hand;S. Harrison;S. Henderson;S. Hildebrandt;G. Hilton;J. Hubmayr;H. Hui;K. Irwin;J. Kang;K. Karkare;E. Karpel;S. Kefeli;S. Kernasovskiy;J. Kovac;C. Kuo;K. Lau;E. Leitch;A. Lennox;K. Megerian;L. Minutolo;L. Moncelsi;Y. Nakato;T. Namikawa;H. Nguyen;R. O’Brient;IV R.W.Ogburn;S. Palladino;T. Prouvé;C. Pryke;B. Racine;C. Reintsema;S. Richter;A. Schillaci;B. Schmitt;R. Schwarz;C. Sheehy;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. L. 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