Measurements of the E-Mode Polarization and Temperature-E-Mode Correlation of the CMB from SPT-3G 2018 Data
D. Dutcher, L. Balkenhol, P. A. R. Ade, Z. Ahmed, E. Anderes, A. J. Anderson, M. Archipley, J. S. Avva, K. Aylor, P. S. Barry, R. Basu Thakur, K. Benabed, A. N.… 展开作者
D. Dutcher, L. Balkenhol, P. A. R. Ade, Z. Ahmed, E. Anderes, A. J. Anderson, M. Archipley, J. S. Avva, K. Aylor, P. S. Barry, R. Basu Thakur, K. Benabed, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, F. R. Bouchet, L. Bryant, K. Byrum, J. E. Carlstrom, F. W. Carter, T. W. Cecil, C. L. Chang, P. Chaubal, G. Chen, H. -M. Cho, T. -L. Chou, J. -F. Cliche, T. M. Crawford, A. Cukierman, C. Daley, T. de Haan, E. V. Denison, K. Dibert, J. Ding, M. A. Dobbs, W. Everett, C. Feng, K. R. Ferguson, A. Foster, J. Fu, S. Galli, A. E. Gambrel, R. W. Gardner, N. Goeckner-Wald, R. Gualtieri, S. Guns, N. Gupta, R. Guyser, N. W. Halverson, A. H. Harke-Hosemann, N. L. Harrington, J. W. Henning, G. C. Hilton, E. Hivon, G. P. Holder, W. L. Holzapfel, J. C. Hood, D. Howe, N. Huang, K. D. Irwin, O. B. Jeong, M. Jonas, A. Jones, T. S. Khaire, L. Knox, A. M. Kofman, M. Korman, D. L. Kubik, S. Kuhlmann, C. -L. Kuo, A. T. Lee, E. M. Leitch, A. E. Lowitz, C. Lu, S. S. Meyer, D. Michalik, M. Millea, J. Montgomery, A. Nadolski, T. Natoli, H. Nguyen, G. I. Noble, V. Novosad, Y. Omori, S. Padin, Z. Pan, P. Paschos, J. Pearson, C. M. Posada, K. Prabhu, W. Quan, S. Raghunathan, A. Rahlin, C. L. Reichardt, D. Riebel, B. Riedel, M. Rouble, J. E. Ruhl, J. T. Sayre, E. Schiappucci, E. Shirokoff, G. Smecher, J. A. Sobrin, A. A. Stark, J. Stephen, K. T. Story, A. Suzuki, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, L. R. Vale, K. Vanderlinde, J. D. Vieira, G. Wang, N. Whitehorn, W. L. K. Wu, V. Yefremenko, K. W. Yoon, M. R. Young
We present measurements of the $E$-mode ($EE$) polarization power spectrum and temperature-$E$-mode ($TE$) cross-power spectrum of the cosmic microwave background using data collected by SPT-3G, the latest instrument installed on the South Pole Telescope. This analysis uses observations of a 1500 deg$^2$ region at 95, 150, and 220 GHz taken over a four month period in 2018. We report binned values of the $EE$ and $TE$ power spectra over the angular multipole range $300 \le \ell < 3000$, using the multifrequency data to construct six semi-independent estimates of each power spectrum and their minimum-variance combination. These measurements improve upon the previous results of SPTpol across the multipole ranges $300 \le \ell \le 1400$ for $EE$ and $300 \le \ell \le 1700$ for $TE$, resulting in constraints on cosmological parameters comparable to those from other current leading ground-based experiments. We find that the SPT-3G dataset is well-fit by a $Λ$CDM cosmological model with parameter constraints consistent with those from Planck and SPTpol data. From SPT-3G data alone, we find $H_0 = 68.8 \pm 1.5 \mathrm{km\,s^{-1}\,Mpc^{-1}}$ and $σ_8 = 0.789 \pm 0.016$, with a gravitational lensing amplitude consistent with the $Λ$CDM prediction ($A_L = 0.98 \pm 0.12$). We combine the SPT-3G and the Planck datasets and obtain joint constraints on the $Λ$CDM model. The volume of the 68% confidence region in six-dimensional $Λ$CDM parameter space is reduced by a factor of 1.5 compared to Planck-only constraints, with only slight shifts in central values. We note that the results presented here are obtained from data collected during just half of a typical observing season with only part of the focal plane operable, and that the active detector count has since nearly doubled for observations made with SPT-3G after 2018.
SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field
Sorbonne Université（索邦大学）；CNRS（法国国家科学研究中心）；Institut d’Astrophysique de Paris（巴黎天体物理研究所）；Argonne National Laboratory（阿贡国家实验室）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics（卡弗里宇宙学物理研究所）；Kavli Institute for Particle Astrophysics and Cosmology（卡弗里粒子天体物理与宇宙学研究所）；Stanford University（斯坦福大学）；University of California, Berkeley（加州大学伯克利分校）
Improving cosmological constraints from galaxy cluster number counts with CMB-cluster-lensing data: Results from the SPT-SZ survey and forecasts for the future
Using SPTpol, Planck 2015, and non-CMB data to constrain tilted spatially-flat and untilted non-flat $Λ$CDM, XCDM, and $ϕ$CDM dark energy inflation cosmologies
Probing Anisotropic Cosmic Birefringence with Foreground-Marginalised SPT B-mode Likelihoods
University of California, Berkeley（加州大学伯克利分校）；University of Melbourne（墨尔本大学）；University of Chicago（芝加哥大学）；Fermi National Accelerator Laboratory（费米国家加速器实验室）
CMB Lensing Reconstruction Using Two Years of Temperature Data from the SPT-3G Summer Survey
University of Melbourne（墨尔本大学）；National Center for Supercomputing Applications（国家超级计算应用中心）；Sorbonne Université（索邦大学）；Institut d’Astrophysique de Paris（巴黎天体物理学研究所）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Fermi National Accelerator Laboratory（费米国家加速器实验室）；Department of Astronomy and Astrophysics, University of Chicago（芝加哥大学天文与天体物理系）
SPT-3G D1: Quadratic-Estimator CMB Lensing Reconstruction and Cosmology
University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理研究所）；NSF-Simons AI Institute for the Sky (SkAI)（NSF-Simons 天空人工智能研究所 (SkAI)）；California Institute of Technology（加州理工学院）；Kavli Institute for Particle Astrophysics and Cosmology, Stanford University（斯坦福大学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）；Stanford University（斯坦福大学）；Sorbonne Université（索邦大学）；CNRS（法国国家科学研究中心）；Institut d’Astrophysique de Paris（巴黎天体物理学研究所）；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；Department of Astronomy, University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校天文学系）
High $H_0$ Values from CMB E-mode Data: A Clue for Resolving the Hubble Tension?
由普朗克、ACTPol和SPTPol测量的E模式（EE）CMB功率谱将哈勃常数约束为标准$Λ$ CDM模型（后验均值和中心68%区间界限）内的$70.0\pm2.7$、$72.4^{+3.9}_{-4.8}$和$73.1^{+3.3}_{-3.9}$ km s $^{-1}$ Mpc $^{-1}$。这些值高于普朗克温度（TT）功率谱的限制，并与造父变星超新星距离阶梯测量$H_0=73.2\pm1.3$ km s $^{-1}$ Mpc $^{-1}$一致。如果这种对更高值的偏好在联合分析中得到加强，它可能会为哈勃分歧的解决提供一个有趣的暗示。然而，我们发现，结合普朗克，ACTPol，和SPTPol EE的可能性产生$H_0=68.7\pm1.3$ km s $^{-1}$ Mpc $^{-1}$，$2.4σ$低于距离阶梯测量。这是由于不同的简并方向在整个参数空间，特别是涉及重子密度，$Ω_bh^2$，和标量倾斜，$n_s$，所产生的灵敏度不同的多极范围。我们表明，E-模式$Λ$ CDM约束是一致的，在$1.4σ$内的不同实验，并与普朗克TT结果在$0.8σ$。结合普朗克，ACTPol，和SPTPol EE数据约束的现象学透镜振幅，$A_L=0.89\pm0.10$，与预期值一致的单位。
Multichroic TES Bolometers and Galaxy Cluster Mass Scaling Relations with the South Pole Telescope
南极望远镜（英语：South Pole Telescope）是一个高分辨率的微波频率望远镜，用于观测宇宙微波背景（CMB）。到目前为止，已经在SPT上安装了两台摄像机，对CMB进行了两次调查，第一次是强度调查（SPT-SZ），第二次是强度和偏振调查（SPTpol）。目前正在开发第三代偏振敏感相机（SPT-3G）。本论文介绍了工作跨越所有三个仪器上的SPT。我提出我的工作在时间颠倒的顺序，遵循仪器开发，部署和分析的规范叙述。首先，新的3波段多色过渡边缘传感器（TES）的SPT-3G实验测辐射热计的开发和测试进行了详细说明，其次是频率复用低温读出电子的SPTpol实验的开发和部署，并得出结论与SPT-SZ仪器所采取的数据分析。我描述了一个贝叶斯似然为基础的方法，我开发的测量综合康普顿化（YSZ）的星系团的Sunyaev-Zel 'dovich（SZ）效应，并限制星系团YSZ质量标度关系的发展。
SPT-3G D1: Maps of the millimeter-wave sky from 2019 and 2020 observations of the SPT-3G Main field
Argonne National Laboratory（阿贡国家实验室）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Sorbonne Université（索邦大学）；CNRS（法国国家科学研究中心）；Institut d’Astrophysique de Paris（巴黎天体物理研究所）；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；AIM（物质与宇宙研究实验室）；University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；University of California, Berkeley（加州大学伯克利分校）；Fermi National Accelerator Laboratory（费米国家加速器实验室）
