Receiver development for BICEP Array, a next-generation CMB polarimeter at the South Pole
Receiver development for BICEP Array, a next-generation CMB polarimeter at the South Pole
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DOI：
10.1117/12.2561995
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发表时间：
2020-12
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通讯作者：
L. Moncelsi;P. Ade;Z. Ahmed;M. Amiri;D. Barkats;R. Thakur;C. Bischoff;J. Bock;J. Bock;V. Buza;V. Buza;J. Cheshire;J. Connors;J. Connors;J. Cornelison;M. Crumrine;A. Cukierman;E. Denison;M. Dierickx;L. Duband;M. Eiben;S. Fatigoni;J. Filippini;N. Goeckner-wald;D. Goldfinger;J. Grayson;P. Grimes;G. Hall;G. Hall;M. Halpern;S. Harrison;S. Henderson;S. Hildebrandt;S. Hildebrandt;G. Hilton;J. Hubmayr;H. Hui;K. Irwin;J. Kang;J. Kang;K. Karkare;K. Karkare;S. Kefeli;J. Kovac;C. Kuo;K. Lau;E. Leitch;K. Megerian;L. Minutolo;Y. Nakato;Y. Nakato;T. Namikawa;T. Namikawa;Hien T. Nguyen;R. O’Brient;R. O’Brient;S. Palladino;N. Precup;T. Prouvé;C. Pryke;B. Racine;C. Reintsema;A. Schillaci;B. Schmitt;A. Soliman;T. S. Germaine;T. S. Germaine;B. Steinbach;R. Sudiwala;K. Thompson;C. Tucker;A. Turner;C. Umilta;C. Umilta;A. Vieregg;A. Wandui;A. Weber;D. Wiebe;J. Willmert;W. L. K. Wu;E. Yang;K. Yoon;E. Young;C. Yu;L. Zeng;C. Zhang;S. Zhang
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作者：
L. Moncelsi;P. Ade;Z. Ahmed;M. Amiri;D. Barkats;R. Thakur;C. Bischoff;J. Bock;J. Bock;V. Buza;V. Buza;J. Cheshire;J. Connors;J. Connors;J. Cornelison;M. Crumrine;A. Cukierman;E. Denison;M. Dierickx;L. Duband;M. Eiben;S. Fatigoni;J. Filippini;N. Goeckner-wald;D. Goldfinger;J. Grayson;P. Grimes;G. Hall;G. Hall;M. Halpern;S. Harrison;S. Henderson;S. Hildebrandt;S. Hildebrandt;G. Hilton;J. Hubmayr;H. Hui;K. Irwin;J. Kang;J. Kang;K. Karkare;K. Karkare;S. Kefeli;J. Kovac;C. Kuo;K. Lau;E. Leitch;K. Megerian;L. Minutolo;Y. Nakato;Y. Nakato;T. Namikawa;T. Namikawa;Hien T. Nguyen;R. O’Brient;R. O’Brient;S. Palladino;N. Precup;T. Prouvé;C. Pryke;B. Racine;C. Reintsema;A. Schillaci;B. Schmitt;A. Soliman;T. S. Germaine;T. S. Germaine;B. Steinbach;R. Sudiwala;K. Thompson;C. Tucker;A. Turner;C. Umilta;C. Umilta;A. Vieregg;A. Wandui;A. Weber;D. Wiebe;J. Willmert;W. L. K. Wu;E. Yang;K. Yoon;E. Young;C. Yu;L. Zeng;C. Zhang;S. Zhang
探测到初级CMB的卷曲型($B$模)偏振将是宇宙起源暴涨范式的直接证据。BICEP/Keck阵列(BK)计划的目标是度角标度，原始$B$模式偏振的功率预计将在度角标度处达到峰值，灵敏度不断提高，并发布了迄今最严格的通胀限制。二头肌阵列(BA)是BK计划的第三阶段仪器，将包括四个在30/40、95、150和220/270 GHz观测的BICEP3级接收器，组合起来有32,000+个探测器；这样的宽频率覆盖对于控制银河系前景是必要的，这也会产生度尺度$B模式信号。30/40 GHz的接收器旨在限制同步加速器的前景，并于2020年初开始在南极进行观测。到为期三年的观测活动结束时，整个BICEP阵列仪器预计将在0.002至0.004年间达到$\sigma_r$，这取决于前景的复杂性和引力透镜(去偏振)导致的$B$-模式的消除程度。本文概述了第一个BA接收机的设计、星上测量性能和定标。我们还给出了在7,776个检测器150 GHz接收器的时域多路复用器读出中增加的复杂性的预览。
A detection of curl-type ($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 $\sigma_r$ 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.