We examine whether a comparison between wCDM and R_h=ct using merged Type Ia SN catalogs produces results consistent with those based on a single homogeneous sample. Using the Betoule et al. (2014) joint lightcurve analysis (JLA) of a combined sample of 613 events from SNLS and SDSS-II, we estimate the parameters of the two models and compare them. We find that the improved statistics can alter the model selection in some cases, but not others. In addition, based on the model fits, we find that there appears to be a lingering systematic offset of ~0.04-0.08 mag between the SNLS and SDSS-II sources, in spite of the cross-calibration in the JLA. Treating wCDM, LCDM and R_h=ct as separate models, we find in an unbiased pairwise statistical comparison that the Bayes Information Criterion (BIC) favors the R_h=ct universe with a likelihood of 82.8% versus 17.2% for wCDM, but the ratio of likelihoods is reversed (16.2% versus 83.8%) when w_de=-1 (i.e., LCDM) and strongly reversed (1.0% versus 99.0%) if in addition k=0 (i.e., flat LCDM). We point out, however, that the value of k is a measure of the net energy (kinetic plus gravitational) in the Universe and is not constrained theoretically, though some models of inflation would drive k to 0 due to an expansion-enforced dilution. Since we here consider only the basic LCDM model, the value of k needs to be measured and, therefore, the pre-assumption of flatness introduces a significant bias into the BIC.
BAQARO: Tracing Stochastic Black Hole Growth Histories and Quasar Lightcurves in a Cosmological Context
Center for Astrophysics | Harvard & Smithsonian（天体物理中心 | 哈佛与史密森尼学会）；Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；Department of Physics, University of California, Santa Barbara（加州大学圣塔芭芭拉分校物理系）
Cosmological Parameter Estimation with a Joint-Likelihood Analysis of the Cosmic Microwave Background and Big Bang Nucleosynthesis
New York University（纽约大学）；Princeton University（普林斯顿大学）；Flatiron Institute（平顿研究所）；Boston University（波士顿大学）；University of Chicago（芝加哥大学）；Fermi National Accelerator Laboratory（费米国家加速器实验室）；Massachusetts Institute of Technology（麻省理工学院）；Harvard University（哈佛大学）
First Cosmological Constraints from the Joint Analysis of Galaxy Clustering and the Kinetic Sunyaev-Zel'dovich Effect
School of Physics and Astronomy, Sun Yat-sen University（中山大学物理学院）；CSST Science Center for the Guangdong–Hong Kong–Macau Greater Bay Area, SYSU（中山大学深空巡天科学中心）
The Role of Big Bang Nucleosynthesis in Joint Cosmological Analyses
Boston University（波士顿大学）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；University of California, Berkeley（加州大学伯克利分校）
First full-shape joint analysis of the two- and three-point correlation functions on real data: $Λ$CDM cosmological constraints from BOSS DR12
Università di Bologna（博洛尼亚大学）；INAF–Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文物理与空间科学观测站）；INAF-Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；INFN-Sezione di Genova（意大利国家核物理学院热那亚分部）；Università di Genova（热那亚大学）
KiDS-Legacy: Consistency of cosmic shear measurements and joint cosmological constraints with external probes
Ruhr University Bochum（波鸿鲁尔大学）；Newcastle University（纽卡斯尔大学）；University of Edinburgh（爱丁堡大学）；Leiden University（莱顿大学）；University College London（伦敦大学学院）；Universität Bonn（波恩大学）；University of Waterloo（滑铁卢大学）；Utrecht University（乌得勒支大学）；Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT)（能源、环境和技术研究中心）；University of Portsmouth（朴茨茅斯大学）；Universität Innsbruck（因斯布鲁克大学）；Alma Mater Studiorum Università di Bologna（博洛尼亚大学）；Istituto Nazionale di Astrofisica (INAF)（意大利国家天体物理研究所）；Istituto Nazionale di Fisica Nucleare (INFN)（意大利国家核物理研究所）；Durham University（杜伦大学）；Polish Academy of Sciences（波兰科学院）；ETH Zürich（苏黎世联邦理工学院）；The Barcelona Institute of Science and Technology（巴塞罗那科学技术研究院）；University of Oxford（牛津大学）；Stockholm University（斯德哥尔摩大学）；Imperial College London（帝国理工学院）；University of Naples Federico II（那不勒斯费德里科二世大学）；University of Groningen（格罗宁根大学）
Cosmological Prediction from the joint observation of MeerKAT and CSST at $z$ = 0.4 $\sim$ 1.2
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences(UCAS)（中国科学院大学天文与空间科学学院）；Department of Physics, Stellenbosch University（斯泰伦博斯大学物理系）；Science Center for Chinese Space Station Survey Telescope, National Astronomical Observatories, Chinese Academy of Science（中国科学院国家天文台中国空间站巡天望远镜科学中心）
Evidence for a correlation between the Si II 4000 width and Type Ia supernova color
本文研究了Ia型超新星Si Ⅱ 4000特征在红移0.0024 < z < 0.634范围内的赝等效宽度。我们发现，这个光谱指标与光变曲线颜色过剩（SALT 2 c）以及先前定义的光谱子类（分支类型）和Si II 6150速度的演变相关，即，即所谓的速度梯度。基于我们对来自不同调查的55个物体的研究，我们发现Si II 4000光谱指示器可以提供重要信息，以改善Ia型超新星的宇宙学距离测量。
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）
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）
