Exploring Cosmic Origins with CORE: B-mode Component Separation
M. Remazeilles, A. J. Banday, C. Baccigalupi, S. Basak, A. Bonaldi, G. De Zotti, J. Delabrouille, C. Dickinson, H. K. Eriksen, J. Errard, R. Fernandez-Cobos, U.… 展开作者
M. Remazeilles, A. J. Banday, C. Baccigalupi, S. Basak, A. Bonaldi, G. De Zotti, J. Delabrouille, C. Dickinson, H. K. Eriksen, J. Errard, R. Fernandez-Cobos, U. Fuskeland, C. Hervías-Caimapo, M. López-Caniego, E. Martinez-González, M. Roman, P. Vielva, I. Wehus, A. Achucarro, P. Ade, R. Allison, M. Ashdown, M. Ballardini, R. Banerji, N. Bartolo, J. Bartlett, D. Baumann, M. Bersanelli, M. Bonato, J. Borrill, F. Bouchet, F. Boulanger, T. Brinckmann, M. Bucher, C. Burigana, A. Buzzelli, Z. -Y. Cai, M. Calvo, C. -S. Carvalho, G. Castellano, A. Challinor, J. Chluba, S. Clesse, I. Colantoni, A. Coppolecchia, M. Crook, G. D'Alessandro, P. de Bernardis, G. de Gasperis, J. -M. Diego, E. Di Valentino, S. Feeney, S. Ferraro, F. Finelli, F. Forastieri, S. Galli, R. Genova-Santos, M. Gerbino, J. González-Nuevo, S. Grandis, J. Greenslade, S. Hagstotz, S. Hanany, W. Handley, C. Hernandez-Monteagudo, M. Hills, E. Hivon, K. Kiiveri, T. Kisner, T. Kitching, M. Kunz, H. Kurki-Suonio, L. Lamagna, A. Lasenby, M. Lattanzi, J. Lesgourgues, A. Lewis, M. Liguori, V. Lindholm, G. Luzzi, B. Maffei, C. J. A. P. Martins, S. Masi, D. McCarthy, J. -B. Melin, A. Melchiorri, D. Molinari, A. Monfardini, P. Natoli, M. Negrello, A. Notari, A. Paiella, D. Paoletti, G. Patanchon, M. Piat, G. Pisano, L. Polastri, G. Polenta, A. Pollo, V. Poulin, M. Quartin, J. -A. Rubino-Martin, L. Salvati, A. Tartari, M. Tomasi, D. Tramonte, N. Trappe, T. Trombetti, C. Tucker, J. Valiviita, R. Van de Weijgaert, B. van Tent, V. Vennin, N. Vittorio, K. Young, M. Zannoni
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87 pages, 32 figures, 4 tables, expanded abstract. Updated to match version accepted by JCAP
We demonstrate that, for the baseline design of the CORE satellite mission, the polarized foregrounds can be controlled at the level required to allow the detection of the primordial cosmic microwave background (CMB) $B$-mode polarization with the desired accuracy at both reionization and recombination scales, for tensor-to-scalar ratio values of ${r\gtrsim 5\times 10^{-3}}$. We consider detailed sky simulations based on state-of-the-art CMB observations that consist of CMB polarization with $τ=0.055$ and tensor-to-scalar values ranging from $r=10^{-2}$ to $10^{-3}$, Galactic synchrotron, and thermal dust polarization with variable spectral indices over the sky, polarized anomalous microwave emission, polarized infrared and radio sources, and gravitational lensing effects. Using both parametric and blind approaches, we perform full component separation and likelihood analysis of the simulations, allowing us to quantify both uncertainties and biases on the reconstructed primordial $B$-modes. Under the assumption of perfect control of lensing effects, CORE would measure an unbiased estimate of $r=\left(5 \pm 0.4\right)\times 10^{-3}$ after foreground cleaning. In the presence of both gravitational lensing effects and astrophysical foregrounds, the significance of the detection is lowered, with CORE achieving a $4σ$-measurement of $r=5\times 10^{-3}$ after foreground cleaning and $60$% delensing. For lower tensor-to-scalar ratios ($r=10^{-3}$) the overall uncertainty on $r$ is dominated by foreground residuals, not by the 40% residual of lensing cosmic variance. Moreover, the residual contribution of unprocessed polarized point-sources can be the dominant foreground contamination to primordial B-modes at this $r$ level, even on relatively large angular scales, $\ell \sim 50$. Finally, we report two sources of potential bias for the detection of the primordial $B$-modes.[abridged]
Crawling the Cosmic Network: Exploring the Morphology of Structure in the Galaxy Distribution
虽然相干的大尺度结构，如细丝和墙壁是显而易见的星系红移调查，他们迄今为止被证明难以用计算机算法来表征。本文提出了一种利用星系密度场Hessian矩阵的特征值和特征向量来表征大尺度结构形态的方法。通过分析平滑的密度场及其海森矩阵，我们可以确定结构的类型-壁，细丝或团块-作为尺度的函数主导星系的大尺度分布。我们已经运行的模拟星系分布的LCDM宇宙学N体模拟和斯隆数字巡天观测到的星系分布的算法。两个星表的结构形态相似，在10 - 20 h ^{-1} Mpc平滑尺度上均以顺磁为主，在5 h ^{-1} Mpc尺度上均以团块为主。在这两种分布中都有壁存在的证据，但在小于~25 h ^{-1} Mpc的尺度上，壁并不是主要的结构。模拟的分析表明，在一个给定的共动平滑尺度，结构随着时间的推移，从墙壁到细丝到团块，在较小的平滑尺度上发现的那些在给定的时间进一步在这个过程中。
Objects Appear Smaller as They Recede: How Proper Motions Can Directly Reveal the Cosmic Expansion, Provide Geometric Distances, and Measure the Hubble Constant
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Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心、天体物理学和信息学实验室）；Institute for Astronomy, University of Hawaii（夏威夷大学天文学研究所）
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Exploring Joint Observation of the CSST Shear and clustering of astrophysical gravitational wave source measurements
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Sciences, University of Chinese Academy of Sciences(UCAS)（中国科学院大学天文与空间科学学院）
Exploring a Cosmic-Ray Inverse-Compton Origin to the SZ-to-X-Ray Pressure Deficit in the Cool Core Cluster ZwCl 3146
California Institute of Technology（加州理工学院）；University of Pennsylvania（宾夕法尼亚大学）；National Radio Astronomy Observatory（美国国家射电天文台）；University of Virginia（弗吉尼亚大学）
Conditional Diffusion-Flow models for generating 3D cosmic density fields: applications to f(R) cosmologies
Grupo Signos, Departamento de Matemáticas, Universidad El Bosque（埃尔博斯克大学数学系信号组）；Data Science Research Centre, Liverpool John Moores University（利物浦约翰·莫尔斯大学数据科学研究中心）；Departamento de Física, Universidad de Córdoba（科尔多瓦大学物理系）
