The Atacama Cosmology Telescope: Constraints on Pre-Recombination Early Dark Energy
J. Colin Hill, Erminia Calabrese, Simone Aiola, Nicholas Battaglia, Boris Bolliet, Steve K. Choi, Mark J. Devlin, Adriaan J. Duivenvoorden, Jo Dunkley, Simone F… 展开作者
J. Colin Hill, Erminia Calabrese, Simone Aiola, Nicholas Battaglia, Boris Bolliet, Steve K. Choi, Mark J. Devlin, Adriaan J. Duivenvoorden, Jo Dunkley, Simone Ferraro, Patricio A. Gallardo, Vera Gluscevic, Matthew Hasselfield, Matt Hilton, Adam D. Hincks, Renee Hlozek, Brian J. Koopman, Arthur Kosowsky, Adrien La Posta, Thibaut Louis, Mathew S. Madhavacheril, Jeff McMahon, Kavilan Moodley, Sigurd Naess, Umberto Natale, Federico Nati, Laura Newburgh, Michael D. Niemack, Lyman A. Page, Bruce Partridge, Frank J. Qu, Maria Salatino, Alessandro Schillaci, Neelima Sehgal, Blake D. Sherwin, Cristobal Sifon, David N. Spergel, Suzanne T. Staggs, Emilie R. Storer, Alexander van Engelen, Eve M. Vavagiakis, Edward J. Wollack, Zhilei Xu
The early dark energy (EDE) scenario aims to increase the value of the Hubble constant ($H_0$) inferred from cosmic microwave background (CMB) data over that found in $Λ$CDM, via the introduction of a new form of energy density in the early universe. The EDE component briefly accelerates cosmic expansion just prior to recombination, which reduces the physical size of the sound horizon imprinted in the CMB. Previous work has found that non-zero EDE is not preferred by Planck CMB power spectrum data alone, which yield a 95% confidence level (CL) upper limit $f_{\rm EDE} < 0.087$ on the maximal fractional contribution of the EDE field to the cosmic energy budget. In this paper, we fit the EDE model to CMB data from the Atacama Cosmology Telescope (ACT) Data Release 4. We find that a combination of ACT, large-scale Planck TT (similar to WMAP), Planck CMB lensing, and BAO data prefers the existence of EDE at $>99.7$% CL: $f_{\rm EDE} = 0.091^{+0.020}_{-0.036}$, with $H_0 = 70.9^{+1.0}_{-2.0}$ km/s/Mpc (both 68% CL). From a model-selection standpoint, we find that EDE is favored over $Λ$CDM by these data at roughly $3σ$ significance. In contrast, a joint analysis of the full Planck and ACT data yields no evidence for EDE, as previously found for Planck alone. We show that the preference for EDE in ACT alone is driven by its TE and EE power spectrum data. The tight constraint on EDE from Planck alone is driven by its high-$\ell$ TT power spectrum data. Understanding whether these differing constraints are physical in nature, due to systematics, or simply a rare statistical fluctuation is of high priority. The best-fit EDE models to ACT and Planck exhibit coherent differences across a wide range of multipoles in TE and EE, indicating that a powerful test of this scenario is anticipated with near-future data from ACT and other ground-based experiments.
Cosmic Birefringence from the Atacama Cosmology Telescope Data Release 6
Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Ludwig-Maximilians-Universität München（慕尼黑大学）；Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), Todai Institutes for Advanced Study, The University of Tokyo（东京大学前沿研究院 Kavli宇宙物理与数学研究所）
Weak-Lensing Mass Calibration of the Atacama Cosmology Telescope Equatorial Sunyaev-Zeldovich Cluster Sample with the Canada-France-Hawaii Telescope Stripe 82 Survey
The Atacama Cosmology Telescope: A Test of the Gravitational Force Law on Cosmological Scales Using the Kinematic Sunyaev-Zeldovich Effect
University of Pennsylvania（宾夕法尼亚大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理研究所）；University of Southern California（南加州大学）；Columbia University（哥伦比亚大学）；Stanford University（斯坦福大学）；Simons Society of Fellows, Simons Foundation（西蒙斯基金会西蒙斯学者协会）；Cornell University（康奈尔大学）；Sapienza University of Rome（罗马第一大学）；Cardiff University（卡迪夫大学）；University of California, Riverside（加州大学河滨分校）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学物理学院天体物理研究所）；Centro de Astro-Ingeniería, Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学天文工程中心）
The Atacama Cosmology Telescope: A demonstration of CMB lensing measurement from daytime data
University of Cambridge（剑桥大学）；Kavli Institute for Cosmology Cambridge（卡弗里宇宙学剑桥研究所）；Kavli Institute for Particle Astrophysics and Cosmology（卡弗里粒子天体物理与宇宙学研究所）；SLAC National Accelerator Laboratory（斯坦福直线加速器中心）；University of Pennsylvania（宾夕法尼亚大学）；Princeton University（普林斯顿大学）；Cardiff University（卡迪夫大学）
精确测量宇宙复合光谱可以为观察早期宇宙提供一个全新的窗口。我们的目标是量化隐藏在宇宙复合谱中的信息，为此，我们开发了一种新的代码，遵循Ali-Haimoud和Hirata（2010），Ali-Haimoud（2013）提出的算法。我们的代码紧密基于COSMOSPEC代码[Chluba and Ali-Haimoud（2016）]。我们发现，使用Fisher信息矩阵，并假设前景可以通过使用更高或更低的频率通道和空间信息减去，超出检测将需要一个实验的灵敏度$25$倍更好的建议的实验PIXIE相比。这样的实验将能够测量宇宙学参数，其精度与CMB各向异性实验具有竞争力。最好的约束参数是重子能量密度，$Ω_{\rm b}$，原则上可以以令人难以置信的精度确定。我们还表明，氢线的形状连接到氢复合的速度，与复合线的峰值重合的复合率的峰值。一般来说，谱线的形状编码了关于作为红移函数的重组率的信息。
The Atacama Cosmology Telescope: Probing new signatures of ultralight axions with gravitational lensing
University of Pennsylvania（宾夕法尼亚大学）；King’s College London（伦敦国王学院）；Imperial College London（帝国理工学院）；Dunlap Institute for Astronomy and Astrophysics, University of Toronto（多伦多大学邓普天文学与天体物理研究所）；Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学加拿大理论天体物理研究所）；Cardiff University（卡迪夫大学）；Princeton University（普林斯顿大学）；University of Southern California（南加州大学）；Institute for Advanced Study（高等研究院）
Constraints on Dark Matter Self-Interactions from weak lensing of galaxies from the Dark Energy Survey around clusters from the Atacama Cosmology Telescope Survey
The Atacama Cosmology Telescope: Constraints on Local Non-Gaussianity from the ACT Cluster Catalog
ICCUB, University of Barcelona（巴塞罗那大学）；Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学理论天体物理研究所）；Wits Centre for Astrophysics, School of Physics, University of the Witwatersrand（威特沃特斯兰德大学物理学院天体物理中心）；Astrophysics Research Centre, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal（夸祖鲁-纳塔尔大学数学、统计与计算机科学学院天体物理研究中心）；ICREA（加泰罗尼亚高级研究院）；Department of Physics and Astronomy, University of Pittsburgh（匹兹堡大学物理与天文系）；Department of Physics, Stanford University（斯坦福大学物理系）；Kavli Institute for Particle Astrophysics and Cosmology（卡弗里粒子天体物理与宇宙学研究所）
Detection of the pairwise kinematic Sunyaev-Zel'dovich effect with BOSS DR11 and the Atacama Cosmology Telescope
我们提出了一个新的测量的运动学Sunyaev-Zeldovich效应使用的数据从阿塔卡玛宇宙望远镜（ACT）和重子振荡光谱巡天（BOSS）。使用600平方度的重叠天空区域，我们评估了与BOSS DR 11大尺度结构目录中50，000个明亮星系的位置相关的平均成对重子动量。一个非零信号来自包含样本星系的晕的大尺度运动。数据拟合的分析信号模型以及，与微波光子散射的光学深度作为一个自由参数确定的整体信号幅度。我们估计的协方差矩阵的平均成对动量作为星系分离的函数，使用微波天空模拟，折刀评估，和自助估计。最保守的基于模拟的误差给出了不同星系光度削减的信噪比估计在3.6和4.1之间。我们讨论了如何其他错误的决定，可以导致更高的信噪比值，并考虑几种可能的系统误差的影响。从样本星系位置的平均热Sunyaev-Zeldovich信号的光学深度的估计与从平均成对动量信号获得的光学深度的估计大致一致。
The Atacama Cosmology Telescope: Detection of the Pairwise Kinematic Sunyaev-Zel'dovich Effect with SDSS DR15 Galaxies
我们提出了一个5.4 $σ$检测成对运动学Sunyaev-Zel'dovich（kSZ）的影响，使用阿塔卡玛宇宙望远镜（ACT）和$\it{Planck}$ CMB的观测结合从斯隆数字巡天（SDSS）DR 15目录的亮红星系样本。结果是使用三个ACT CMB地图获得的：共同添加的150 GHz和98 GHz地图，结合2008-2018年（ACT DR 5）的观测结果，与SDSS DR 15重叠超过3，700平方米。度，和一个使用2014-2015年（ACT DR 4）夜间观测的分量分离图，与SDSS DR 15重叠超过2，089平方米。°的这三个地图的结果的比较提供了关于潜在的频率相关的前景污染的一致性检查。总共有343，647个星系被用作示踪剂，以识别和定位星系群和星系团，并使用孔径测光从中提取kSZ信号。我们考虑了各种孔径测光假设和协方差估计方法对信号提取的影响。成对速度的理论预测用于获得最佳拟合，质量平均，光学深度估计为五个亮度选择示踪剂样品。kSZ派生的光学深度测量在这里获得的那些来自热SZ效应相同的样品的比较是在配套文件。
