发表机构
Max Planck Institute for Extraterrestrial Physics; LMU München; Universität Innsbruck; IRAP, Université de Toulouse, CNRS, UPS, CNES; INAF, Osservatorio di Astrofisica e Scienza dello Spazio; Beijing Normal University; Université Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3; National Cheng Kung University; Nagoya University; The University of Tokyo（马克斯·普朗克地外物理研究所; 慕尼黑大学; 因斯布鲁克大学; 图卢兹大学/法国国家科学研究中心/法国航天研究中心天体物理学与行星学研究所; 意大利国家天体物理研究所空间天体物理观测站; 北京师范大学; 格勒诺布尔阿尔卑斯大学; 国立成功大学; 名古屋大学; 东京大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
利用eRASS1星系团计数首次约束早期暗能量，联合外部数据得到f_EDE=0.10和H0=71.4，缓解哈勃常数张力。
AI 中文摘要
大质量星系团质量函数的演化是宇宙学中一个成熟的研究探针。利用光谱伦琴伽马（SRG）任务搭载的eROSITA X射线仪器，eROSITA首次全天巡天（eRASS1）的西银半球提供了一个均匀选择且可靠确认的样本，包含5259个星系团，红移范围为$0.1 < z < 0.8$。当与来自DES第三年、KiDS和HSC的重叠弱引力透镜数据进行质量标定相结合时，该数据集能够对标准$\Lambda$CDM框架及其扩展模型进行精确检验。在本工作中，我们使用eRASS1星系团目录中$0.1 < z < 0.45$的子样本，对类轴子早期暗能量（EDE）情景施加约束。此类模型被提出作为缓解早期宇宙与晚期宇宙哈勃常数测量之间张力的可能机制。在该框架下，一个标量场在重组时期前后暂时增强宇宙膨胀速率，随后在更晚时期迅速稀释，从而在结构增长上留下独特印记。我们利用这些印记，首次给出了由星系团计数推导的EDE约束。仅使用eRASS1计数，我们得到最大EDE分数上限为$f_{\rm EDE} < 0.3$，与初级宇宙微波背景（CMB）分析一致。将我们的星系团分析与初级CMB测量、重子声学振荡和CMB透镜效应相结合，同时明确排除距离阶梯标定数据，得到的结果与非零EDE贡献以及与晚期宇宙测量相容的$H_0$值一致。最显著的探测，显著性约为$3.2\sigma$，来自eRASS1样本与全套外部数据集的联合分析，得到$f_{\rm EDE} = 0.10^{+0.04}_{-0.03}$和$H_0 = 71.4 \pm 1.4$ km/s/Mpc。
英文摘要
The evolution of the mass function of massive galaxy clusters is a well-established probe of cosmology. Using the eROSITA X-ray instrument on board the Spectrum Roentgen Gamma (SRG) mission, the western Galactic hemisphere of eROSITA's first All-Sky Survey (eRASS1) delivers a uniformly selected and securely confirmed sample of 5259 galaxy clusters spanning $0.1 < z < 0.8$. When combined with overlapping weak lensing data from DES Year 3, KiDS, and HSC for mass calibration, this dataset enables precise tests of the standard $Λ$CDM framework and beyond. In this work, we use the $0.1 < z < 0.45$ subsample of the eRASS1 cluster catalog to place constraints on an axion-like Early Dark Energy (EDE) scenario. Such models have been proposed as a possible mechanism to alleviate the tension between early- and late-Universe measurements of the Hubble constant. In this framework, a scalar field temporarily enhances the cosmic expansion rate around the epoch of recombination before rapidly diluting at later times, leaving distinct imprints on structure growth. We leverage these signatures to present the first constraints on EDE derived from galaxy cluster number counts. Using eRASS1 number counts alone, we obtain an upper limit on the maximum EDE fraction of $f_{\rm EDE} < 0.3$, consistent with primary CMB analyses. Combining our cluster analysis with primary CMB measurements, baryon acoustic oscillations, and CMB lensing, while notably excluding distance-ladder calibration data, yields results consistent with a nonzero EDE contribution and $H_0$ values compatible with late-Universe measurements. The most significant detection, at $\sim 3.2σ$, arises from the joint analysis of the eRASS1 sample with the full set of external datasets, yielding $f_{\rm EDE} = 0.10^{+0.04}_{-0.03}$ and $H_0 = 71.4 \pm 1.4$ km/s/Mpc. [ABRIDGED]
Comments26 pages, 18 figures, 4 tables. Accepted for publication by A&A
