The Simons Observatory: Dark Characterization of the Large Aperture Telescope
Saianeesh K. Haridas, Zeeshan Ahmed, Tanay Bhandarkar, Mark Devlin, Simon Dicker, Shannon M. Duff, Daniel Dutcher, Kathleen Harrington, Shawn W. Henderson, Joha… 展开作者
Saianeesh K. Haridas, Zeeshan Ahmed, Tanay Bhandarkar, Mark Devlin, Simon Dicker, Shannon M. Duff, Daniel Dutcher, Kathleen Harrington, Shawn W. Henderson, Johannes Hubmayr, Bradley R. Johnson, Anna Kofman, Alex Manduca, Michael D. Niemack, Michael J. Randall, Thomas P. Satterthwaite, John Orlowski-Scherer, Benjamin L. Schmitt, Carlos Sierra, Max Silva-Feaver, Robert J. Thornton, Yuhan Wang, Kaiwen Zheng
The Simons Observatory (SO) is a cosmic microwave background experiment composed of three 0.42 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT) in the Atacama Desert of Chile. The Large Aperture Telescope Receiver (LATR) was integrated into the LAT in August 2023; however, because mirrors were not yet installed, the LATR optical chain was capped at the 4K stage. In this dark configuration we are able to characterize many elements of the instrument without contributions from atmospheric noise. Here we show this noise is below the required upper limit and its features are well described with a simple noise model. Maps produced using this noise model have properties that are in good agreement with the white noise levels of our dark data. Additionally, we show that our nominal scan strategy has a minimal effect on the noise when compared to the noise when the telescope is stationary
The Simons Observatory: Studies of Detector Yield and Readout Noise From the First Large-Scale Deployment of Microwave Multiplexing at the Large Aperture Telescope
The Simons Observatory: Studies of Phase Drift in RF Transmission Lines from the First Large-Scale Deployment of Microwave Frequency Multiplexing for Cosmology
Stanford University（斯坦福大学）；Kavli Institute for Particle Astrophysics & Cosmology, Stanford（斯坦福粒子天体物理与宇宙学卡弗里研究所）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；Cornell University（康奈尔大学）；Wright Laboratory, Department of Physics, Yale University（耶鲁大学物理莱特实验室）
The Simons Observatory: Detector Polarization Angle Calibration using Sparse Wire Grid with Initial Data Sets of the Small Aperture Telescope
Kyoto University（京都大学）；Okayama University（冈山大学）；Princeton University（普林斯顿大学）；University of California San Diego（加州大学圣迭戈分校）；KEK（高能加速器研究机构）；The University of Tokyo（东京大学）；University of Milano-Bicocca（米兰比可卡大学）
The Simons Observatory: Overview of the Cryogenic Half-wave Plate Polarization Modulators
University of California Riverside（加州大学河滨分校）；Princeton University（普林斯顿大学）；University of California San Diego（加州大学圣地亚哥分校）；The University of Tokyo（东京大学）；The Suwa University of Science（信州大学（原諏訪科學大學））；University of Texas at Austin（德克萨斯大学奥斯汀分校）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）
The Simons Observatory: On-sky performance of radio-transparent multi-layer insulation (RT-MLI) using Styroace-II Styrofoam
Princeton University（普林斯顿大学）；University of Texas at Austin（德克萨斯大学奥斯汀分校）；The University of Tokyo（东京大学）；University of California San Diego（加州大学圣地亚哥分校）；Argonne National Laboratory（阿贡国家实验室）；University of Chicago（芝加哥大学）；High Energy Accelerator Research Organization (KEK)（高能加速器研究机构（KEK））；University of Virginia（弗吉尼亚大学）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）
The Simons Observatory: Overview of data acquisition, control, monitoring, and computer infrastructure
西蒙斯天文台（SO）是一个即将进行的极化宇宙微波背景（CMB）调查实验，将使用三个小口径望远镜和一个大口径望远镜从智利的阿塔卡马沙漠进行观测。总的来说，SO将在27和280 GHz之间的六个光谱波段中放置超过60，000个过渡边缘传感器（TES）测辐射热计，以实现测量或约束众多宇宙学参数所需的灵敏度，包括张量标量比，相对论物质的有效数量以及中微子质量的总和。SO科学目标需要协调和控制分布在现场四台望远镜之间的硬件。为了满足这一需求，我们设计并构建了一个用于分布式系统管理的开源平台，称为Observatory Control System（ocs）。该控制系统与所有子系统接口，包括望远镜控制单元、微波多路复用读出电子设备和低温测温。我们还开发了一个实时监测内务数据和警报的系统，这两者对于远程观察都至关重要。我们利用现有的开源项目，例如用于RPC和PubSub的crossbar，用于异步事件的twisted，用于在线远程监控的grafana以及用于容器化的docker。我们提供了SO软件和计算机基础设施的概述，包括SO开发的代码与开源资源的集成，以及在SO实验室开发硬件系统进行测试时所吸取的经验教训。
The Simons Observatory: Development of a Pipeline to Detect Rapid Transients in Time-Ordered Data
The University of Melbourne（墨尔本大学）；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 National Institute for Astrophysics (INAF)（意大利国家天体物理研究所）；The Institute for Fundamental Physics of the Universe (IFPU)（宇宙基础物理研究所）；University of Pennsylvania（宾夕法尼亚大学）；University of Milano-Bicocca（米兰比可卡大学）；Princeton University（普林斯顿大学）；University of Toronto（多伦多大学）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Specola Vaticana (Vatican Observatory)（梵蒂冈天文台）
The Simons Observatory: Rotation Performance of Cryogenic Half-Wave Plate Polarization Modulators
Princeton University（普林斯顿大学）；University of California, San Diego（加利福尼亚大学圣地亚哥分校）；The University of Tokyo（东京大学）；The Suwa University of Science（诹访科学大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS（宇宙物理与数学研究所（WPI））；University of Texas at Austin（德克萨斯大学奥斯汀分校）；Weinberg Institute for Theoretical Physics（温伯格理论物理研究所）；Texas Center for Cosmology and Astroparticle Physics（德克萨斯宇宙学与高能天体物理中心）
Keck Observatory as an HWO Testbed: validating wavefront sensing and control schemes on a large segmented aperture in parallel with high-contrast science
