The Simons Observatory: Galactic Science Goals and Forecasts
The Simons Observatory: Galactic Science Goals and Forecasts
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DOI：
10.3847/1538-4357/ac5e36
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发表时间：
2021-11
期刊：
影响因子：
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通讯作者：
B. Hensley;S. Clark;Valentina Fanfani;N. Krachmalnicoff;G. Fabbian;D. Poletti;G. Puglisi;G. Coppi;Jacob Nibauer;R. Gerasimov;N. Galitzki;Steve K. Choi;P. Ashton;C. Baccigalupi;E. Baxter;B. Burkhart;E. Calabrese;J. Chluba;J. Errard;A. Frolov;C. Herv'ias-Caimapo;K. Huffenberger;Bradley R. Johnson;B. Jost;B. Keating;H. McCarrick;F. Nati;Mayuri Sathyanarayana Rao;A. van Engelen;S. Walker;K. Wolz;Zhilei Xu;N. Zhu;A. Zonca
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文献类型：
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作者：
B. Hensley;S. Clark;Valentina Fanfani;N. Krachmalnicoff;G. Fabbian;D. Poletti;G. Puglisi;G. Coppi;Jacob Nibauer;R. Gerasimov;N. Galitzki;Steve K. Choi;P. Ashton;C. Baccigalupi;E. Baxter;B. Burkhart;E. Calabrese;J. Chluba;J. Errard;A. Frolov;C. Herv'ias-Caimapo;K. Huffenberger;Bradley R. Johnson;B. Jost;B. Keating;H. McCarrick;F. Nati;Mayuri Sathyanarayana Rao;A. van Engelen;S. Walker;K. Wolz;Zhilei Xu;N. Zhu;A. Zonca
西蒙斯天文台（SO）在27至280 GHz的六个频段进行观测，除了其主要的宇宙学目标外，还准备解决银河系天体物理学中的许多问题。在这项工作中，我们提供了一系列银河系科学案例的天体物理参数的定量预测。我们发现，SO可以：将偏振尘埃辐射的频谱限制在Δβ d ≤ 0.01的水平，从而测试尘埃成分模型，预测偏振β d与总强度测量值不同;测量偏振尘埃和同步辐射之间的相关系数，其精度比当前限制高两倍;如果真实分数与巨行星的探测率相似，则排除在大约2.9σ处不存在外奥尔特云;绘制850多个分子云，其中至少有50个独立的偏振测量值，分辨率为1 pc;在选定区域探测或设定0.1%水平的CO（2-1）发射和异常微波发射的偏振分数上限;并在1°斑块中测量光学星光偏振和微波偏振尘埃发射之间的相关系数，所有视线为NH 2 × 1020 cm−2。这里概述的目标和预测为其他微波偏振实验提供了路线图，以通过银河系天体物理学扩展其科学范围。37 37介绍作者对本文所作贡献的补充资料可在https://simonsobservatory.org/wp-content/uploads/2022/02/SO_GS_Contributions.pdf上查阅。描述作者对本文贡献的补充说明可以在https://simonsobservatory.org/wp-content/uploads/2022/02/SO_GS_Contributions.pdf上找到。
Observing in six frequency bands from 27 to 280 GHz over a large sky area, the Simons Observatory (SO) is poised to address many questions in Galactic astrophysics in addition to its principal cosmological goals. In this work, we provide quantitative forecasts on astrophysical parameters of interest for a range of Galactic science cases. We find that SO can: constrain the frequency spectrum of polarized dust emission at a level of Δβ d ≲ 0.01 and thus test models of dust composition that predict that β d in polarization differs from that measured in total intensity; measure the correlation coefficient between polarized dust and synchrotron emission with a factor of two greater precision than current constraints; exclude the nonexistence of exo-Oort clouds at roughly 2.9σ if the true fraction is similar to the detection rate of giant planets; map more than 850 molecular clouds with at least 50 independent polarization measurements at 1 pc resolution; detect or place upper limits on the polarization fractions of CO(2–1) emission and anomalous microwave emission at the 0.1% level in select regions; and measure the correlation coefficient between optical starlight polarization and microwave polarized dust emission in 1° patches for all lines of sight with N H ≳ 2 × 1020 cm−2. The goals and forecasts outlined here provide a roadmap for other microwave polarization experiments to expand their scientific scope via Milky Way astrophysics. 37 37 A supplement describing author contributions to this paper can be found at https://simonsobservatory.org/wp-content/uploads/2022/02/SO_GS_Contributions.pdf. A supplement describing author contributions to this paper can be found at https://simonsobservatory.org/wp-content/uploads/2022/02/SO_GS_Contributions.pdf.