表征40 GHz TES强仪对二头肌阵列的灵敏度

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表征40 GHz TES强仪对二头肌阵列的灵敏度

Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array

论文作者

Zhang, C., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Bischoff, C. A., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Dierickx, M., Duband, L., Fatigoni, S., Filippini, J. P., Hall, G., Halpern, M., Harrison, S., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Megerian, K. G., Moncelsi, L., Namikawa, T., Nguyen, H. T., O'Brient, R., Palladino, S., Precup, N., Prouvé, T., Pryke, C., Racine, B., Reintsema, C. D., Richter, S., Schillaci, A., Schmitt, B., Schwarz, R., Sheehy, C. D., 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.

论文摘要

二头肌/凯克（BK）实验旨在检测宇宙微波背景极化中原始引力波的烙印，这将是通胀理论的直接证据。虽然张量与量表的比率已限制为在95％C.L.时为R_0.05 <0.06，但由于偏振银乳流前景排放和去除引力透镜极化，因此对该上限的进一步改善受到阻碍。二头肌阵列（BA）的30/40 GHz接收器将在2019年底部署，并将在BK Sky贴片中以前所未有的准确性来限制同步加速器前景。我们将展示30/40 GHz检测器的设计，并测试结果总结了其性能。在这些频率下的低光学和大气负荷要求我们的TES检测器具有低饱和功率，以使光子噪声占主导地位。为了实现250 MK碱温度所需的低导热率，我们开发了新的钢计腿设计。我们将介绍相关测量的检测器参数：G，TC，RN，PSAT和光谱带和噪声光谱。我们达到了每座NEP，包括2.07e-17 w/sqrt（Hz）的所有噪声组件，包括预期的光子噪声水平1.54e-17 w/sqrt（Hz）。

The BICEP/Keck (BK) experiment aims to detect the imprint of primordial gravitational waves in the Cosmic Microwave Background polarization, which would be direct evidence of the inflation theory. While the tensor-to-scalar ratio has been constrained to be r_0.05 < 0.06 at 95% c.l., further improvements on this upper limit are hindered by polarized Galactic foreground emissions and removal of gravitational lensing polarization. The 30/40 GHz receiver of the BICEP Array (BA) will deploy at the end of 2019 and will constrain the synchrotron foreground with unprecedented accuracy within the BK sky patch. We will show the design of the 30/40 GHz detectors and test results summarizing its performance. The low optical and atmospheric loading at these frequencies requires our TES detectors to have low saturation power in order to be photon-noise dominated. To realize the low thermal conductivity required from a 250 mK base temperature, we developed new bolometer leg designs. We will present the relevant measured detector parameters: G, Tc, Rn, Psat , and spectral bands, and noise spectra. We achieved a per bolometer NEP including all noise components of 2.07E-17 W/sqrt(Hz), including an anticipated photon noise level 1.54E-17 W/sqrt(Hz).

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