Euclid preparation. Simulations and nonlinearities beyond $Λ$CDM. 1. Numerical methods and validation
Euclid Collaboration, J. Adamek, B. Fiorini, M. Baldi, G. Brando, M. -A. Breton, F. Hassani, K. Koyama, A. M. C. Le Brun, G. Rácz, H. -A. Winther, A. Casalino, … 展开作者
Euclid Collaboration, J. Adamek, B. Fiorini, M. Baldi, G. Brando, M. -A. Breton, F. Hassani, K. Koyama, A. M. C. Le Brun, G. Rácz, H. -A. Winther, A. Casalino, C. Hernández-Aguayo, B. Li, D. Potter, E. Altamura, C. Carbone, C. Giocoli, D. F. Mota, A. Pourtsidou, Z. Sakr, F. Vernizzi, A. Amara, S. Andreon, N. Auricchio, C. Baccigalupi, S. Bardelli, P. Battaglia, D. Bonino, E. Branchini, M. Brescia, J. Brinchmann, A. Caillat, S. Camera, V. Capobianco, V. F. Cardone, J. Carretero, S. Casas, F. J. Castander, M. Castellano, G. Castignani, S. Cavuoti, A. Cimatti, C. Colodro-Conde, G. Congedo, C. J. Conselice, L. Conversi, Y. Copin, F. Courbin, H. M. Courtois, A. Da Silva, H. Degaudenzi, G. De Lucia, M. Douspis, F. Dubath, X. Dupac, S. Dusini, M. Farina, S. Farrens, S. Ferriol, P. Fosalba, M. Frailis, E. Franceschi, M. Fumana, S. Galeotta, B. Gillis, P. Gómez-Alvarez, A. Grazian, F. Grupp, L. Guzzo, S. V. H. Haugan, W. Holmes, F. Hormuth, A. Hornstrup, S. Ilić, K. Jahnke, M. Jhabvala, B. Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, M. Kilbinger, B. Kubik, M. Kümmel, M. Kunz, H. Kurki-Suonio, S. Ligori, P. B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, E. Maiorano, O. Mansutti, O. Marggraf, K. Markovic, M. Martinelli, N. Martinet, F. Marulli, R. Massey, E. Medinaceli, S. Mei, M. Melchior, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, M. Moresco, L. Moscardini, C. Neissner, S. -M. Niemi, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, W. J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. A. Popa, L. Pozzetti, F. Raison, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, R. Saglia, A. G. Sánchez, D. Sapone, B. Sartoris, M. Schirmer, T. Schrabback, A. Secroun, G. Seidel, S. Serrano, C. Sirignano, G. Sirri, L. Stanco, J. Steinwagner, P. Tallada-Crespí, D. Tavagnacco, I. Tereno, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, E. A. Valentijn, L. Valenziano, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Y. Wang, J. Weller, G. Zamorani, E. Zucca, A. Biviano, C. Burigana, M. Calabrese, D. Di Ferdinando, J. A. Escartin Vigo, G. Fabbian, F. Finelli, J. Gracia-Carpio, S. Matthew, N. Mauri, A. Pezzotta, M. Pöntinen, V. Scottez, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, V. Allevato, S. Anselmi, M. Archidiacono, F. Atrio-Barandela, A. Balaguera-Antolinez, M. Ballardini, A. Blanchard, L. Blot, H. Böhringer, S. Borgani, S. Bruton, R. Cabanac, A. Calabro, B. Camacho Quevedo, G. Cañas-Herrera, A. Cappi, F. Caro, C. S. Carvalho, T. Castro, K. C. Chambers, S. Contarini, A. R. Cooray, G. Desprez, A. Díaz-Sánchez, J. J. Diaz, S. Di Domizio, H. Dole, S. Escoffier, A. G. Ferrari, P. G. Ferreira, I. Ferrero, A. Finoguenov, F. Fornari, L. Gabarra, K. Ganga, J. García-Bellido, T. Gasparetto, V. Gautard, E. Gaztanaga, F. Giacomini, F. Gianotti, G. Gozaliasl, C. M. Gutierrez, A. Hall, H. Hildebrandt, J. Hjorth, A. Jimenez Muñoz, S. Joudaki, J. J. E. Kajava, V. Kansal, D. Karagiannis, C. C. Kirkpatrick, S. Kruk, J. Le Graet, L. Legrand, J. Lesgourgues, T. I. Liaudat, A. Loureiro, G. Maggio, M. Magliocchetti, F. Mannucci, R. Maoli, C. J. A. P. Martins, L. Maurin, R. B. Metcalf, M. Migliaccio, M. Miluzio, P. Monaco, A. Montoro, A. Mora, C. Moretti, G. Morgante, S. Nadathur, L. Patrizii, V. Popa, P. Reimberg, I. Risso, P. -F. Rocci, M. Sahlén, E. Sarpa, A. Schneider, M. Sereno, A. Silvestri, A. Spurio Mancini, K. Tanidis, C. Tao, N. Tessore, G. Testera, R. Teyssier, S. Toft, S. Tosi, A. Troja, M. Tucci, C. Valieri, J. Valiviita, D. Vergani, G. Verza, P. Vielzeuf, N. A. Walton
备注：
20 pages, 7 figures, 1 appendix; submitted on behalf of the Euclid Collaboration
To constrain models beyond $Λ$CDM, the development of the Euclid analysis pipeline requires simulations that capture the nonlinear phenomenology of such models. We present an overview of numerical methods and $N$-body simulation codes developed to study the nonlinear regime of structure formation in alternative dark energy and modified gravity theories. We review a variety of numerical techniques and approximations employed in cosmological $N$-body simulations to model the complex phenomenology of scenarios beyond $Λ$CDM. This includes discussions on solving nonlinear field equations, accounting for fifth forces, and implementing screening mechanisms. Furthermore, we conduct a code comparison exercise to assess the reliability and convergence of different simulation codes across a range of models. Our analysis demonstrates a high degree of agreement among the outputs of different simulation codes, providing confidence in current numerical methods for modelling cosmic structure formation beyond $Λ$CDM. We highlight recent advances made in simulating the nonlinear scales of structure formation, which are essential for leveraging the full scientific potential of the forthcoming observational data from the Euclid mission.
A more inclusive effective dark fluid equation of state parameter: constraints from SKA and Euclid like surveys
Instituto de Física Teórica UAM-CSIC（UAM-CSIC理论物理研究所）；IRAP, Université de Toulouse, CNRS, CNES, UPS（图卢兹大学）；Faculty of Sciences, Université St Joseph（圣约瑟夫大学理学院）
syren-halofit: A fast, interpretable, high-precision formula for the $Λ$CDM nonlinear matter power spectrum
CNRS（法国国家科学研究中心）；Sorbonne Université（索邦大学）；Center for Computational Astrophysics, Flatiron Institute（弗拉蒂伦研究所计算天体物理中心）；University of Oxford（牛津大学）；Institute of Cosmology & Gravitation, University of Portsmouth（朴茨茅斯大学宇宙学与引力研究所）
Non-linear evolution of the cosmic neutrino background
我们研究了非线性演化的遗迹宇宙中微子背景运行大盒子大小，高分辨率的N体模拟。我们的一组模拟探索中微子的性质在参考$Λ$ CDM模型与总中微子质量在0.05-0.60 eV之间的冷暗物质晕的质量$10^{11}-10^{15}$ $h^{-1}$ M $_{\odot}$，在红移范围$z=0-2$。我们计算的晕质量函数，并表明，它是合理的Sheth-Tormen公式拟合。更重要的是，我们专注于CDM和中微子性质的密度和奇特的速度场的宇宙体积，内部和外围的维里化晕。中微子粒子的动力学状态强烈地依赖于它们的动量：而在低速尾的中微子行为类似于CDM粒子，在高速尾的中微子不受底层CDM组件的聚集。我们发现，中微子（线性）未扰动的动量分布被修改和质量和红移依赖的偏差从预期的费米-狄拉克分布都在宇宙体积和内晕。我们仔细研究了维里化晕周围的中微子密度分布，并给出了一个简单的拟合公式。中微子的配置文件，不像冷的暗物质之一，被发现是核心的核心大小和中心密度取决于中微子的质量，红移和质量的晕，质量大于$\sim 10^{13.5}h^{-1}$ M $_{\odot}$的晕。对于较低的质量中微子档案是最好的拟合一个简单的幂律关系的范围内探测的模拟。我们的研究结果是特别重要的，鉴于即将到来的大尺度结构调查，如欧几里得，预计将探讨在百分比水平的非线性政权与透镜和聚类观察。
Going beyond $S_8$: fast inference of the matter power spectrum from weak-lensing surveys
Université Grenoble Alpes, CNRS, LPSC-IN2P3（格勒诺布尔阿尔卑斯大学，法国国家科学研究中心，LPSC-IN2P3）；Kavli Institute for Cosmological Physics, Enrico Fermi Institute, and Department of Astronomy & Astrophysics, University of Chicago（芝加哥大学卡弗里宇宙学物理研究所、恩里科·费米研究所及天文学与天体物理学系）
Modeling nonlinear scales for dynamical dark energy cosmologies with COLA
CBPF - Brazilian Center for Research in Physics（巴西物理研究中心）；Instituto de Física Teórica da Universidade Estadual Paulista（圣保罗州立大学理论物理研究所）；Department of Physics & Astronomy, Stony Brook University（石溪大学物理与天文学系）；C. N. Yang Institute for Theoretical Physics, Stony Brook University（石溪大学陈省身理论物理研究所）
Euclid preparation. The shape of halo profiles in $Λ$CDM and non-standard cosmologies
Università degli Studi di Milano Bicocca（米兰比可卡大学）；INAF-Osservatorio Astronomico di Trieste（的里雅斯特天文台）；Laboratoire d’etude de l’Univers et des phenomenes eXtremes, Observatoire de Paris, Université PSL, Sorbonne Université, CNRS（极端宇宙现象研究实验室，巴黎天文台，巴黎文理研究大学，索邦大学，法国国家科学研究中心）；Institut d’Astrophysique de Paris, UMR 7095, CNRS, and Sorbonne Université（巴黎天体物理研究所，法国国家科学研究中心，索邦大学）；Université Paris-Cité（巴黎西岱大学）；University of Helsinki（赫尔辛基大学）；Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester（曼彻斯特大学天体物理学乔德雷尔银行中心）；Yusuf Hamied Department of Chemistry, University of Cambridge（剑桥大学尤素福·哈米德化学系）；Instituto de Física Teórica UAM-CSIC（马德里自治大学-西班牙国家科学研究委员会理论物理研究所）
Euclid preparation: Testing multi-field inflation with galaxy power spectrum and bispectrum
INFN Gruppo Collegato di Parma（意大利核物理研究所帕尔马协作组）；Laboratoire d’Annecy-le-Vieux de Physique Theorique, CNRS & Universite Savoie Mont Blanc（阿讷西勒沃伊理论物理实验室，法国国家科学研究中心与萨瓦蒙布朗大学）；Institute of Space Sciences (ICE, CSIC), Campus UAB（空间科学研究所（CSIC下属），巴塞罗那自治大学校区）；Dipartimento di Fisica, Università degli studi di Genova, and INFN-Sezione di Genova（热那亚大学物理系及意大利核物理研究所热那亚分部）；SISSA, International School for Advanced Studies（国际高等研究院）；INAF-Osservatorio Astronomico di Trieste（的里雅斯特天文台）；IFPU, Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Technion Israel Institute of Technology（以色列理工学院）
