论文标题
西蒙斯天文台的小孔望远镜
Small Aperture Telescopes for the Simons Observatory
论文作者
论文摘要
Simons天文台（SO）是位于智利Cerro Toco上的即将到来的宇宙微波背景（CMB）实验，它将在六个跨越27至285 GHz的六个频带中以温度和极化为单位绘制微波炉的天空。因此，将由一个6米大的孔径望远镜（LAT）外观$ \ sim $ 30,000探测器和一个三个0.42米小孔径望远镜（SAT）组成的阵列，将另外30,000个探测器放置。这种协同作用将使CMB在角度尺度上具有极其敏感的表征，从弧线到数十度，从而实现了广泛的科学输出。在这里，我们专注于靶向程度角度尺度的SAT，并使用连续的二色体仪器（MF：93/145 GHz）观察到超高频率（UHF：225/285 GHz）和低频（LF：LF：27/39 GHz）。组合93和145 GHz时，这三个SAT将能够将$ \ sim $ 10％的天空映射到2 $μ$ k-arcmin的噪声水平。多频带将使CMB与银河前景（主要是同步子和尘埃）分开，其主要科学目标是表征原始张张量比$ r $，目标水平为$σ\ left（r \ right）\约0.003 $。
The Simons Observatory (SO) is an upcoming cosmic microwave background (CMB) experiment located on Cerro Toco, Chile, that will map the microwave sky in temperature and polarization in six frequency bands spanning 27 to 285 GHz. SO will consist of one 6-meter Large Aperture Telescope (LAT) fielding $\sim$30,000 detectors and an array of three 0.42-meter Small Aperture Telescopes (SATs) fielding an additional 30,000 detectors. This synergy will allow for the extremely sensitive characterization of the CMB over angular scales ranging from an arcmin to tens of degrees, enabling a wide range of scientific output. Here we focus on the SATs targeting degree angular scales with successive dichroic instruments observing at Mid-Frequency (MF: 93/145 GHz), Ultra-High-Frequency (UHF: 225/285 GHz), and Low-Frequency (LF: 27/39 GHz). The three SATs will be able to map $\sim$10% of the sky to a noise level of 2 $μ$K-arcmin when combining 93 and 145 GHz. The multiple frequency bands will allow the CMB to be separated from galactic foregrounds (primarily synchrotron and dust), with the primary science goal of characterizing the primordial tensor-to-scalar ratio, $r$, at a target level of $σ\left(r\right) \approx 0.003$.
