BICEP Array 接收机研制：南极下一代 CMB 偏振计
天体物理仪器与方法
2020-12-09 v1 宇宙学与河外天体物理
仪器与探测器
摘要
对原初 CMB 的旋度型（ 模）偏振的探测将是宇宙起源暴胀范式最直接的证据。BICEP/Keck Array（BK）项目以不断提高的灵敏度瞄准角尺度（预期原初 模偏振功率在此达到峰值），并已发表了迄今对暴胀最严格的限制。BICEP Array（BA）是 BK 项目的第三阶段仪器，将由四台 BICEP3 级别的接收机组成，分别在 30/40、95、150 和 220/270 GHz 观测，共含 32,000 多个探测器；如此宽的频率覆盖对于控制银河系前景（其同样会产生角尺度 模信号）是必要的。30/40 GHz 接收机旨在限制同步辐射前景，已于 2020 年初在南极开始观测。在为期 3 年的观测活动结束时，完整的 BICEP Array 仪器预计将达到 介于 0.002 与 0.004 之间，具体取决于前景复杂度以及由引力透镜引起的 模的去除程度（去透镜）。本文概述了首台 BA 接收机的设计、实测天空性能与定标。我们还预览了在 7,776 探测器 150 GHz 接收机时域复用读出中增加的复杂性。
引用
@article{arxiv.2012.04047,
title = {Receiver development for BICEP Array, a next-generation CMB polarimeter at the South Pole},
author = {L. Moncelsi and P. A. R. Ade and Z. Ahmed and M. Amiri and D. Barkats and R. Basu Thakur and C. A. Bischoff and J. J. Bock and V. Buza and J. Cheshire and J. Connors and J. Cornelison and M. Crumrine and A. Cukierman and E. V. Denison and M. Dierickx and L. Duband and M. Eiben and S. Fatigoni and J. P. Filippini and N. Goeckner-Wald and D. C. Goldfinger and J. Grayson and P. Grimes and G. Hall and M. Halpern and S. Harrison and S. Henderson and S. R. Hildebrandt and G. C. Hilton and J. Hubmayr and H. Hui and K. D. Irwin and J. Kang and K. S. Karkare and S. Kefeli and J. M. Kovac and C. L. Kuo and K. Lau and E. M. Leitch and K. G. Megerian and L. Minutolo and Y. Nakato and T. Namikawa and H. T. Nguyen and R. O'Brient and S. Palladino and N. Precup and T. Prouve and C. Pryke and B. Racine and C. D. Reintsema and A. Schillaci and B. L. Schmitt and A. Soliman and T. St. Germaine and B. Steinbach and R. V. Sudiwala and K. L. Thompson and C. Tucker and A. D. Turner and C. Umiltà and A. G. Vieregg and A. Wandui and A. C. Weber and D. V. Wiebe and J. Willmert and W. L. K. Wu and E. Yang and K. W. Yoon and E. Young and C. Yu and L. Zeng and C. Zhang and S. Zhang},
journal= {arXiv preprint arXiv:2012.04047},
year = {2020}
}
备注
Proceedings of SPIE 2020 (AS111). This article supersedes arXiv:1808.00568 and arXiv:2002.05228