The Simons Observatory: pipeline comparison and validation for large-scale B-modes
K. Wolz, S. Azzoni, C. Hervias-Caimapo, J. Errard, N. Krachmalnicoff, D. Alonso, C. Baccigalupi, A. Baleato Lizancos, M. L. Brown, E. Calabrese, J. Chluba, J. D… 展开作者
K. Wolz, S. Azzoni, C. Hervias-Caimapo, J. Errard, N. Krachmalnicoff, D. Alonso, C. Baccigalupi, A. Baleato Lizancos, M. L. Brown, E. Calabrese, J. Chluba, J. Dunkley, G. Fabbian, N. Galitzki, B. Jost, M. Morshed, F. Nati
The upcoming Simons Observatory Small Aperture Telescopes aim at achieving a constraint on the primordial tensor-to-scalar ratio $r$ at the level of $σ(r=0)\lesssim0.003$, observing the polarized CMB in the presence of partial sky coverage, cosmic variance, inhomogeneous non-white noise, and Galactic foregrounds. We present three different analysis pipelines able to constrain $r$ given the latest available instrument performance, and compare their predictions on a set of sky simulations that allow us to explore a number of Galactic foreground models and elements of instrumental noise, relevant for the Simons Observatory. The three pipelines employ different combinations of parametric and non-parametric component separation at the map and power spectrum levels, and use B-mode purification to estimate the CMB B-mode power spectrum. We applied them to a common set of simulated realistic frequency maps, and compared and validated them with focus on their ability to extract robust constraints on the tensor-to-scalar ratio $r$. We evaluated their performance in terms of bias and statistical uncertainty on this parameter. In most of the scenarios the three methodologies achieve similar performance. Nevertheless, several simulations with complex foreground signals lead to a $>2σ$ bias on $r$ if analyzed with the default versions of these pipelines, highlighting the need for more sophisticated pipeline components that marginalize over foreground residuals. We show two such extensions, using power-spectrum-based and map-based methods, that are able to fully reduce the bias on $r$ below the statistical uncertainties in all foreground models explored, at a moderate cost in terms of $σ(r)$.
The Simons Observatory: Assessing the Impact of Dust Complexity on the Recovery of Primordial $B$-modes
Princeton University（普林斯顿大学）；Stanford University（斯坦福大学）；California Institute of Technology（加州理工学院）；The International School for Advanced Studies (SISSA)（高级研究国际学校）；University of Oxford（牛津大学）；The National Institute for Nuclear Physics (INFN)（意大利国家核物理研究所）；The Institute for Fundamental Physics of the Universe (IFPU)（宇宙基础物理研究所）；The University of Manchester（曼彻斯特大学）；University of Virginia（弗吉尼亚大学）；The National Institute for Nuclear Physics (INFN) - Sezione di Catania（意大利国家核物理研究所卡塔尼亚分部）
The Simons Observatory: Quantifying the impact of beam chromaticity on large-scale B-mode science
University of Milano-Bicocca（米兰比可卡大学）；University of Oxford（牛津大学）；Princeton University（普林斯顿大学）；Max-Planck-Institut fur Astrophysik（马克斯·普朗克天体物理学研究所）；University of California, Berkeley（加州大学伯克利分校）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；University of Iceland（冰岛大学）；Stockholm University（斯德哥尔摩大学）；The International School for Advanced Studies (SISSA)（国际高等研究院）；The National Institute for Nuclear Physics (INFN)（意大利国家核物理研究所）
The Simons Observatory: Design and Initial Performance of the Detector Readout System for the Large-Aperture Telescope
Stanford University（斯坦福大学）；Kavli Institute for Particle Astrophysics and Cosmology（卡弗里粒子天体物理与宇宙学研究所）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；University of California San Diego（加州大学圣地亚哥分校）；University of Pennsylvania（宾夕法尼亚大学）；Princeton University（普林斯顿大学）
Forecasting Constraints on Non-Thermal Light Massive Relics from Future CMB Experiments (CMB-S4/Simons Observatory)
Indian Institute of Science Education and Research（印度科学教育研究所）；Harish-Chandra Research Institute, A CI of Homi Bhabha National Institute（哈里什-昌德拉研究所，霍米·巴巴国立学院成员机构）；Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University（亚琛工业大学理论粒子物理与宇宙学研究所（TTK））；Indian Institute of Astrophysics（印度天体物理研究所）
The Simons Observatory: Commissioning of the Mid-Frequency Small Aperture Telescopes
High Energy Physics Division, Argonne National Laboratory（阿贡国家实验室高能物理部）；Department of Astronomy and Astrophysics, University of Chicago（芝加哥大学天体物理学系）；Department of Physics and Astronomy, University of Southern California（南加州大学物理与天文学系）；Department of Physics, University of Texas at Austin（德克萨斯大学奥斯汀分校物理系）；Weinberg Institute for Theoretical Physics, Texas Center for Cosmology and Astroparticle Physics（韦恩伯格理论物理研究所、德州宇宙学与粒子物理中心）；Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University（普林斯顿大学杰弗里·亨利物理实验室）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学 Kavli宇宙起源研究所（WPI）、UTIAS）；Department of Physics, University of Chicago（芝加哥大学物理系）
Kavli IPMU (WPI), UTIAS, The University of Tokyo（Kavli IPMU（WPI），UTIAS，东京大学）；Department of Applied Mathematics and Theoretical Physics, University of Cambridge（剑桥大学应用数学与理论物理系）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）
