The Simons Observatory: science goals and forecasts
The Simons Observatory: science goals and forecasts
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DOI：
10.1088/1475-7516/2019/02/056
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发表时间：
2019-02-01
影响因子：
6.4
通讯作者：
Zhu, Ningfeng
中科院分区：
文献类型：
--
作者：
Ade, Peter;Aguirre, James;Zhu, Ningfeng
Simons天文台（SO）是一个新的宇宙微波背景实验，该实验是在智利的Cerro Toco上建造的，这是由于2020年代初期开始观察。我们描述了实验的科学目标，激励设计并预测其性能。因此，将在六个频带中测量宇宙微波背景的温度和极化各向异性，该频带为：27、39、93、145、225和280 GHz。 SO的初始构造将具有三个小孔径0.5-m望远镜和一个6 m望远镜的大量伸缩，总计60,000个低温验证仪。我们的关键科学目标是表征原始扰动，测量相对论物种的数量和中微子的质量，测试与宇宙常数的偏差，改善我们对星系进化的理解，并限制了复位的持续时间。小孔望远镜将瞄准可观察到的最大的角度尺度，在93和145 GHz频段中，将大约至10％的天空映射到白噪声水平为2 Mu K-Arcmin，以测量原始张量张量 - 量表比率，以在Sigma的目标水平上，以SIGMA的目标水平（R）（R）= 0.003。大型孔径望远镜将在高度的93和145 GHz带中绘制到高度为6 mu k-arcmin的预期白噪声水平的天空的40％，与大多数大型Synoptict Sumpecope Sky区域重叠，并部分与深色能源光谱仪器重叠。与普朗克卫星的地图相比，高分辨率的天空地图将限制宇宙参数，宇宙学参数，微波背景的重力镜头，原始双光谱的重力镜头，以及热和kinyaev-zel'dovich的巨大效果，并将效应效果张量比比率。该调查还将提供16,000个星系簇和20,000多个婚后源的旧目录。（1）
The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial con figuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping approximate to 10% of the sky to a white noise level of 2 mu K-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of sigma(r) = 0.003. The large aperture telescope will map approximate to 40% of the sky at arcminute angular resolution to an expected white noise level of 6 mu K-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources.(1)