Reanalyzing DESI DR1: 5. Cosmological Constraints with Simulation-Based Priors
Université de Genève（日内瓦大学）；Massachusetts Institute of Technology（麻省理工学院）；The NSF AI Institute for Artificial Intelligence and Fundamental Interactions（美国国家科学基金会人工智能基础相互作用研究所）；Leinweber Institute for Theoretical Physics at Stanford（斯坦福莱因韦伯理论物理研究所）；Kavli Institute for Particle Astrophysics and Cosmology（卡弗里粒子天体物理学与宇宙学研究所）
Anton Chudaykin, Mikhail M. Ivanov, Oliver H. E. Philcox
备注：
24+2 pages, 8+1 figures, 9+1 tables; v2: added Appendix D exploring the sensitivity of the results to quasar priors; added a comparison with previous analyses; matched the version accepted by Phys. Rev. D
我们利用公开的DESI全形状聚类数据进行分析，采用基于模拟的先验（SBPs）。我们的先验是通过将归一化流拟合到从场级模拟中测量到的EFT参数分布中获得的，这些模拟本身是使用为每个追踪器定制的暗物质占位分布（HOD）模型生成的。在功率谱分析中结合SBPs显著增强了ΛCDM宇宙学参数约束；结合DESI DR2的BAO信息和一个关于质子密度的BBN先验，我们发现物质密度参数Ωm=0.2987±0.0066，哈勃常数H0=68.80±0.35 km s⁻¹ Mpc⁻¹，以及质量波动幅度σ8=0.766±0.015（或透镜参数S8=0.764±0.018），这些结果比基线结果分别强1%、40%和50%，尽管σ8有所下降。SBPs在扩展模型中也有显著影响，当与CMB（和超新星）结合时，在w0waCDM分析中暗能量图示优劣提高了70%（20%）。在SBP分析中，我们未发现动态暗能量的统计显著证据：方程状态参数在无（有）超新星分析中与宇宙学常数一致，误差在2.2σ（1.4σ）范围内。中微子质量约束也得到增强，ΛCDM和w0waCDM中95%的限制分别为Mν<0.073 eV和Mν<0.090 eV。后者是迄今为止最强的约束，强化了对正常中微子质量层级的偏好，无论背景动态如何。尽管我们的结果对HOD建模假设敏感，但它们清楚地表明，加入小尺度信息可以显著提高宇宙学参数约束。
英文摘要：
We analyze the public DESI full-shape clustering data using simulation-based priors (SBPs). Our priors are obtained by fitting normalizing flows to the distribution of EFT parameters measured from field-level simulations, themselves generated using tailored halo occupation distribution (HOD) models for each tracer. Incorporating SBPs in a power spectrum analysis significantly enhances $Λ$CDM cosmological parameter constraints; in combination with BAO information from DESI DR2 and a BBN prior on the baryon density, we find the matter density parameter $Ω_m=0.2987\pm0.0066$, the Hubble constant $H_0=68.80\pm0.35\,\rm{km}\,\rm{s}^{-1}\rm{Mpc}^{-1}$, and the mass fluctuation amplitude $σ_8 = 0.766\pm0.015$ (or the lensing parameter $S_8=0.764\pm0.018$), which are $1\%$, $40\%$ and $50\%$ stronger than the baseline results, though with a notable downwards shift in $σ_8$, driven by the quasar HOD assumptions. The SBPs also have a significant impact in extended models, with the dark energy figure-of-merit improving by $70\%$ ($20\%$) in a $w_0w_a$CDM analysis when combining with the CMB (and supernovae). In the SBP analysis, we do not find statistically significant evidence for dynamical dark energy: the equation of state parameters are consistent with a cosmological constant within $2.2σ$ ($1.4σ$) in analyses without (with) supernovae. The neutrino mass constraints are also enhanced, with the $95\%$ limits $M_ν<0.073\,\rm{eV}$ and $M_ν<0.090\,\rm{eV}$ in $Λ$CDM and $w_0w_a$CDM respectively. The latter is the strongest constraint obtained to date and reinforces the preference for the normal neutrino mass hierarchy, regardless of the background dynamics. While our results are sensitive to HOD modeling assumptions, they clearly demonstrate that the inclusion of small-scale information can significantly sharpen cosmological parameter constraints.
Reanalyzing DESI DR1: 1. $Λ$CDM Constraints from the Power Spectrum and Bispectrum
Département de Physique Théorique and Center for Astroparticle Physics, Université de Genève（日内瓦大学理论物理系与天体粒子物理中心）；Center for Theoretical Physics – a Leinweber Institute, Massachusetts Institute of Technology（麻省理工学院莱因韦伯研究所理论物理中心）；Simons Society of Fellows, Simons Foundation（西蒙斯基金会西蒙斯学者协会）；Center for Theoretical Physics, Columbia University（哥伦比亚大学理论物理中心）；Leinweber Institute for Theoretical Physics at Stanford（斯坦福大学莱因韦伯理论物理研究所）
Reanalyzing DESI DR1: 4. Percent-Level Cosmological Constraints from Combined Probes and Robust Evidence for the Normal Neutrino Mass Hierarchy
Center for Theoretical Physics – a Leinweber Institute, Massachusetts Institute of Technology（麻省理工学院莱因韦伯理论物理中心）；The NSF AI Institute for Artificial Intelligence and Fundamental Interactions（美国国家科学基金会人工智能基础相互作用研究所）；Department of Physics, Columbia University（哥伦比亚大学物理系）；NASA Hubble Fellowship Program（NASA哈勃奖学金项目）；Département de Physique Théorique and Center for Astroparticle Physics, Université de Genève（日内瓦大学理论物理系与天体粒子物理中心）；Department of Physics, University of California, Berkeley（加州大学伯克利分校物理系）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）
Cosmological preference for a positive neutrino mass at 2.7$σ$: A joint analysis of DESI DR2, DESY5, and DESY1 data
Liaoning Key Laboratory of Cosmology and Astrophysics, College of Sciences, Northeastern University（东北大学理学院宇宙学与天体物理辽宁省重点实验室）；School of Physics, Ningxia University（宁夏大学物理学院）；MOE Key Laboratory of Data Analytics and Optimization for Smart Industry, Northeastern University（东北大学工业智能与系统优化数据解析与优化教育部重点实验室）；National Frontiers Science Center for Industrial Intelligence and Systems Optimization, Northeastern University（东北大学工业智能与系统优化国家前沿科学中心）
Cosmological Evidence for Dark Axion-Dark Baryon Interactions from Apparent Phantom Crossing
University of Pennsylvania（宾夕法尼亚大学）；Simon Fraser University（西蒙菲莎大学）；Canadian Institute for Theoretical Astrophysics (CITA), University of Toronto（多伦多大学加拿大理论天体物理研究所）
Impact of a negative cosmological constant on the reconstruction of dark energy in light of DESI BAO data
School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, UCAS（杭州高等研究院基础物理与数学学院，UCAS）；School of Physical Sciences, University of Chinese Academy of Sciences（中国科学院大学物理科学学院）；International Center for Theoretical Physics Asia-Pacific（亚太理论物理中心）；Institute of Theoretical Physics, Chinese Academy of Sciences（中国科学院理论物理研究所）
Nonlocal Gravity, Restricted CPL Dynamics and DESI Constraints
Ruprecht-Karls-Universität Heidelberg（海德堡大学）；New York University Abu Dhabi（纽约大学阿布扎比分校）；University of the Basque Country UPV/EHU（巴斯克大学）；Indian Institute of Astrophysics（印度天体物理研究所）；Universidad Complutense de Madrid（马德里康普顿斯大学）
Study of the cosmological tensions and DESI-DR2 in the framework of the Little Rip model
University of Mohammed first（穆罕默德一世大学）；Mohammed I University（穆罕默德一世大学）；Laboratory of Physics of Matter and Radiation（物质与辐射物理实验室）；Astrophysical and Cosmological Center（天体物理与宇宙学中心）；Faculty of Sciences（理学院）；Higher School of Education and Training（教育与培训高等学院）
Cosmological constraints on nonphantom dynamical dark energy with DESI Data Release 2 Baryon Acoustic Oscillations: A 3$σ$+ lensing anomaly
Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS, The University of Tokyo（宇宙物理数学卡弗里研究所（WPI），UTIAS，东京大学）
Cosmological and lunar laser ranging constraints on evolving dark energy in a nonminimally coupled curvature-matter gravity model
Istituto per le Applicazioni del Calcolo, CNR（意大利国家研究委员会计算应用研究所）；INFN - Laboratori Nazionali di Frascati (LNF)（意大利国家核物理研究所弗拉斯卡蒂国家实验室）；Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto（波尔图大学理学院物理与天文系）；Centro de Física das Universidades do Minho e do Porto（米尼奥大学和波尔图大学物理中心）；Universitá di Camerino（卡梅里诺大学）；Al-Farabi Kazakh National University（阿里-法拉比哈萨克国立大学）；ICRANet（国际相对论天体物理中心网络）
Measurements of the Angular Homogeneity Scale from DESI DR1
Observatório Nacional（国家天文台）；Universidade Federal Rural do Rio de Janeiro（里约热内卢联邦农村大学）；Zhejiang University（浙江大学）；Universidade do Estado do Rio de Janeiro（里约热内卢州立大学）
Updated cosmological constraints on axion dark energy with DESI
Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Boston University（波士顿大学）；University College London（伦敦大学学院）；NSF NOIRLab（美国国家科学基金会NOIR天文台实验室）；University of California, Berkeley（加州大学伯克利分校）；Institute of Cosmology and Gravitation, University of Portsmouth（朴茨茅斯宇宙学与引力研究所）；Institute of Space Sciences, ICE-CSIC（空间科学研究所，西班牙高等科学研究委员会）；Fermi National Accelerator Laboratory（费米国家加速器实验室）；Center for Cosmology and AstroParticle Physics, The Ohio State University（俄亥俄州立大学宇宙学与天体粒子物理中心）；Department of Physics, The Ohio State University（俄亥俄州立大学物理系）；The Ohio State University（俄亥俄州立大学）；School of Mathematics and Physics, University of Queensland（昆士兰大学数学与物理学院）；Department of Physics, The University of Texas at Dallas（德克萨斯大学达拉斯分校物理系）；Department of Physics, Southern Methodist University（南方卫理公会大学物理系）；Department of Physics and Astronomy, University of California, Irvine（加州大学尔湾分校物理与天文系）；Department of Physics and Astronomy, Siena College（西纳学院物理与天文系）；Department of Physics and Astronomy, Sejong University（世宗大学物理与天文系）；Department of Physics, University of Michigan（密歇根大学物理系）；University of Michigan（密歇根大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
Cosmological inference from a joint DESI DR1 full-shape power spectrum and bispectrum analysis
University of Edinburgh（爱丁堡大学）；University of Michigan（密歇根大学）；University of Hertfordshire（赫特福德大学）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）；University of Sussex（萨塞克斯大学）；Ohio University（俄亥俄大学）；University of Waterloo（滑铁卢大学）；CEA, Université Paris-Saclay（法国原子能和替代能源委员会，巴黎萨克雷大学）
Design and optimization of neural networks for multifidelity cosmological emulation
University of California, Riverside（加州大学河滨分校）；Department of Physics & Astronomy, University of California, Riverside（加州大学河滨分校物理与天文系）；Department of Physics, University of Michigan（密歇根大学物理系）；Leinweber Center for Theoretical Physics（莱因韦伯理论物理中心）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）
Cosmological constraints from the small scale clustering of Emission Line Galaxies
Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；University of the Basque Country UPV/EHU（巴斯克大学）；IKERBASQUE, Basque Foundation for Science（伊卡萨巴斯克科学基金会）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（ICE，CSIC））；Institute for Computational Cosmology, Department of Physics, Durham University（达勒姆大学物理学院计算宇宙学研究所）；Institute of Astronomy, Madingley Road, Cambridge（剑桥大学天文学研究所）；Kavli Institute for Cosmology Cambridge（卡弗里宇宙学剑桥研究所）；LadHyX UMR CNRS 7646, École Polytechnique, Institut Polytechnique de Paris（巴黎理工学院高等工业学校拉迪液压实验室）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森尼天体物理中心）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理研究所）
