二头肌阵列的接收器开发，这是南极的下一代CMB极化计

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二头肌阵列的接收器开发，这是南极的下一代CMB极化计

Receiver development for BICEP Array, a next-generation CMB polarimeter at the South Pole

论文作者

Moncelsi, L., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Bischoff, C. A., Bock, J. J., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Denison, E. V., Dierickx, M., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P., Hall, G., Halpern, M., Harrison, S., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Megerian, K. G., Minutolo, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Palladino, S., Precup, N., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Schillaci, A., Schmitt, B. L., Soliman, A., Germaine, T. St., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tucker, C., Turner, A. D., Umiltà, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, E., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., Zhang, S.

论文摘要

检测主要CMB的卷曲型（$ b $ mode）极化将是宇宙起源通货膨胀范式的直接证据。二头肌/凯克阵列（BK）程序针对度角度尺度，其中原始$ b $ mmode极化的功率预计将达到峰值，并具有越来越多的灵敏度，并且已经发布了迄今为止对通货膨胀的最严格限制。二头肌阵列（BA）是BK程序的第三阶段仪器，将组成四个bicep3级接收器，观察到30/40、95、150和220/270 GHz，共有32,000多个检测器；如此广泛的频率覆盖范围对于控制银河前景，这也产生了学位尺度$ b $ mmode信号。 30/40 GHz接收器旨在限制同步加速器的前景，并于2020年初开始观察南极。到了为期3年的观测活动结束时，根据$ - $ - $ - $ dress的销售，预计完整的二头肌阵列仪器将达到0.002至0.004之间的$σ_r$ $σ_r$ $σ_R$。本文概述了设计的概述，测量了第一个BA接收器的天空性能和校准。我们还提供了7,776-detector 150 GHz接收器的时域多路复用读数中附加复杂性的预览。

A detection of curl-type ($B$-mode) polarization of the primary CMB would be direct evidence for the inflationary paradigm of the origin of the Universe. The BICEP/Keck Array (BK) program targets the degree angular scales, where the power from primordial $B$-mode polarization is expected to peak, with ever-increasing sensitivity and has published the most stringent constraints on inflation to date. BICEP Array (BA) is the Stage-3 instrument of the BK program and will comprise four BICEP3-class receivers observing at 30/40, 95, 150 and 220/270 GHz with a combined 32,000+ detectors; such wide frequency coverage is necessary for control of the Galactic foregrounds, which also produce degree-scale $B$-mode signal. The 30/40 GHz receiver is designed to constrain the synchrotron foreground and has begun observing at the South Pole in early 2020. By the end of a 3-year observing campaign, the full BICEP Array instrument is projected to reach $σ_r$ between 0.002 and 0.004, depending on foreground complexity and degree of removal of $B$-modes due to gravitational lensing (delensing). This paper presents an overview of the design, measured on-sky performance and calibration of the first BA receiver. We also give a preview of the added complexity in the time-domain multiplexed readout of the 7,776-detector 150 GHz receiver.

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