SPT-3G+：南极望远镜的宇宙微波背景实验

SPT-3G+: A Cosmic Microwave Background Experiment for the South Pole Telescope

T. Natoli, Z. Ahmed, H. Athreya, J. E. Austermann, K. Bae, A. Bapat, D. R. Barron, P. S. Barry, A. N. Bender, B. A. Benson, L. E. Bleem, J. E. Carlstrom, T. W. Cecil, C. L. Chang, S. Cisneros, A. Coerver, J. Cornelison, T. M. Crawford, R. Datta, K. R. Dibert, W. Dominguez, S. M. Duff, K. Fichman, J. P. Filippini, L. Gades, P. A. Gallardo, S. Galli, N. W. Halverson, Q. Hao, S. Henderson, R. Herbst, W. L. Holzapfel, A. Hryciuk, J. Hubmayr, D. Jones, V. Kabra, K. S. Karkare, C. King, M. A. Koc, A. M. Kofman, R. A. Lew, M. J. Link, T. J. Lucas, A. Mangu, E. S. Martsen, J. J. McMahon, J. Montgomery, J. M. Nagy, H. Nguyen, V. Novosad, S. Padin, T. Pinsonneault-Marotte, S. Raghunathan, A. S. Rahlin, C. L. Reichardt, L. Ruckman, J. E. Ruhl, M. S. Sarwar, S. Simon, R. Singh, J. A. Sobrin, A. A. Stark, Q. Taylor, C. Tucker, J. Ullom, J. Van Lanen, J. D. Vieira, A. G. Vieregg, M. R. Vissers, G. Wang, W. L. K. Wu, V. Yefremenko, E. Yilmaz, C. Yu, J. Zivick

arXiv 2608.20236首次发表：2026-08-21更新：2026-08-21

AI 中文总结

该研究介绍计划2029年安装于南极望远镜的SPT-3G+接收机，其采用6020个双色极化像素等技术，测绘速度较SPT-3G提升近10倍，将观测6年以获取深CMB图，用于约束暴胀相关的张量-标量比r。

AI 中文摘要

SPT-3G+是计划于2029年初安装在10米南极望远镜（South Pole Telescope, SPT）上的下一代巡天接收机。这款新接收机将配备6020个极化敏感双色像素，采用过渡边缘传感器，在中心频率为90 GHz和150 GHz的波段进行观测。SPT-3G+接收机中的24080个探测器将通过稀释制冷机冷却至100 mK，并使用微波SQUID多路复用技术进行读出。该接收机的光学设计可实现直径为4度的视场，该视场被划分为14个独立的光学管，每个光学管包含低温氧化铝、硅和尼龙透镜。这些技术选择将使SPT-3G+接收机的测绘速度比当前运行的SPT-3G接收机提高近一个数量级。部署后，SPT-3G+接收机将对与BICEP巡天重叠的天区进行6年观测，以获得结合90 GHz和150 GHz的宇宙微波背景（CMB）图深度为0.5 μK·arcmin。这些观测数据将用于创建前所未有的深CMB引力透镜图、发现新的星系团以及探测天体物理瞬变源。SPT-3G+产生的引力透镜图将用于去除或“透镜校正”前景B模式，其中大尺度结构通过引力透镜作用于CMB，将E模式转化为B模式极化，目标是揭示暴胀产生的B模式。作为南极天文台的一部分，结合BICEp阵列的数据，SPT-3G+的数据将用于约束张量-标量比r，目标是实现σ(r)=0.001的测量精度。

英文摘要

SPT-3G+ is the next survey receiver planned to be installed in early 2029 on the 10-meter South Pole Telescope (SPT). This new receiver will feature 6,020 polarization-sensitive dichroic pixels with transition-edge sensors observing in frequency bands centered at 90 GHz and 150 GHz. The 24,080 detectors in the SPT-3G+ receiver will be cooled to 100 mK by a dilution refrigerator and read out using microwave SQUID multiplexing. The optical design of the receiver enables a 4 degree diameter field of view, which is broken up into 14 individual optics tubes each containing cryogenic alumina, silicon, and nylon lenses. These technology choices will allow the SPT-3G+ receiver to improve on the mapping speed of the currently operating SPT-3G receiver by nearly an order of magnitude. Once deployed, the SPT-3G+ receiver will observe for 6-years an area overlapping with the BICEP survey to achieve a combined (90 GHz and 150 GHz) CMB map depth of 0.5 uK-arcmin. Data from these observations will be used to create unprecedentedly deep CMB lensing maps, discover new galaxy clusters, and detect astrophysical transients. The lensing map produced by SPT-3G+ will be used to remove or "delens" foreground B modes, where large-scale structure gravitationally lenses the CMB and converts E modes into B-mode polarization, with the goal of revealing inflationary B modes. Together with data from the BICEP Array as part of the South Pole Observatory, SPT-3G+ data will be used to constrain the tensor-to-scalar ratio $r$ with a goal of achieving a measurement of $σ(r) = 0.001$

Comments22 pages, 7 figures, Proceedings for SPIE Astronomincal Telescopes + Instrumentation 2026 Paper 14156-14

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