arXiv 2608.25015astro-ph.IM

BICEP阵列的现状及220/270 GHz接收机的集成

Status of BICEP Array and Integration of the 220/270 GHz Receiver

A. Steiger, P. A. R. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Basu Thakur, C. A. Bischoff, D. Beck, J. J. Bock, V. Buza, B. Cantrall, J. R. Cheshire, J. Connors,… 展开作者

A. Steiger, P. A. R. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Basu Thakur, C. A. Bischoff, D. Beck, J. J. Bock, V. Buza, B. Cantrall, J. R. Cheshire, J. Connors, J. Cornelison, M. Crumrine, A. J. Cukierman, E. Denison, L. Duband, M. A. Echter, M. Eiben, B. D. Elwood, S. Fatigoni, J. P. Filippini, A. Fortes, M. Gao, C. Giannakopoulos, N. Goeckner-Wald, D. C. Goldfinger, S. Gratton, J. A. Grayson, A. Greathouse, P. K. Grimes, M. Halpern, S. Henderson, T. D. Hoang, J. Hubmayr, H. Hui, K. D. Irwin, M. Izquierdo Poza, J. H. Kang, K. S. Karkare, S. Kefeli, J. M. Kovac, C. Kuo, K. Lasko, K. Lau, M. Lautzenhiser, G. Liu, S. C. Mackey, N. Maher, K. G. Megerian, L. Minutolo, L. Moncelsi, Y. Nakato, H. T. Nguyen, R. O'Brient, S. N. Paine, A. Patel, M. A. Petroff, A. R. Polish, T. Prouve, C. Pryke, C. D. Reintsema, T. Romand, M. Salatino, A. Schillaci, B. Schmitt, B. Singari, A. Soliman, T. St. Germaine, B. Steinbach, R. Sudiwala, K. L. Thompson, C. Tucker, A. D. Turner, C. Vergès, A. G. Vieregg, A. Wandui, A. C. Weber, J. Willmert, W. L. K. Wu, H. Yang, C. Yu, L. Zeng, C. Zhang, S. Zhang

首次发表 2026-08-31

阅读 PDF

arXiv 页面 ↗HTML 原文 ↗

浏览论文内容

中文总结 AI 辅助

本文介绍了BICEP阵列的现状，该阵列计划2034年将张量-标量比r的不确定度降至约0.001，重点说明了220/270 GHz接收机的集成进展及相关测试情况。

中文摘要 AI 辅助

宇宙微波背景（CMB）的偏振测量对现代宇宙学至关重要，因为它们能约束早期宇宙和宇宙暴胀的物理规律。BICEP阵列（BICEP Array）正在南极使用一系列小口径偏振计测量该信号，计划到2034年将张量-标量比r的测量不确定度控制在约0.001。30/40 GHz接收机和150 GHz接收机已观测CMB多年，其数据将纳入BICEP下一次发布的分析结果，该结果包含截至2024年获取的所有数据。220/270 GHz接收机已部分完成，12个探测器模块中已安装7个，计划在2027年观测季前再安装5个模块。完成该接收机是BICEP阵列的首要任务，因为实验的科学目标需要该接收机实现的尘埃前景清理。2025-26南极夏季的现场表征工作显示，该接收机的光谱学、波束指向性及220 GHz效率均令人满意，而270 GHz效率仍在积极研究中。

英文摘要

Measurements of the polarization of the cosmic microwave background are critical for modern cosmology as they constrain the physics of the early universe and cosmic inflation. BICEP Array is using a series of small-aperture polarimeters located at the South Pole to measure this signal with a projected uncertainty on the tensor-to-scalar ratio r of approximately 0.001 by 2034. The 30/40 GHz receiver and the 150 GHz receiver have been observing the cosmic microwave background for multiple years, and data from these receivers will be included in the next published BICEP analysis result which includes all data taken through 2024. The 220/270 GHz receiver is partially completed with seven out of twelve detector modules installed, and is planned to be filled with five additional modules prior to the 2027 observation season. Finishing this receiver is a top priority for BA as the science goals of the experiment require the dust foreground cleaning this receiver will enable. On-site characterization efforts for this receiver from the 2025-26 austral summer show satisfactory spectroscopy, beam pointing, and 220 GHz efficiency, while the 270 GHz efficiency is an active area of work.

补充信息

备注: 16 pages, 11 figures