arXiv 2402.040062024-02astro-ph.CO

来自Chandra-Planck星系团样本的宇宙学约束

Cosmological constraints from the Chandra-Planck galaxy cluster sample

G. Aymerich, M. Douspis, G. W. Pratt, L. Salvati, E. Soubrié, F. Andrade-Santos, W. Forman, C. Jones, N. Aghanim, R. Kraft, R. J. van Weeren

备注：: 21 pages, 20 figures, accepted by A&A
发表信息：: A&A 690, A238 (2024)
DOI：: 10.1051/0004-6361/202449513

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AI总结：

基于Chandra和Planck星系团样本，提出新标度关系与选择效应校正方法，校准质量偏差并推导宇宙学约束，发现放宽红移演化假设可消除与CMB结果的S8张力。

摘要：

我们利用由Chandra在X射线波段观测的Planck早期Sunyaev-Zeldovich（ESZ）星表中的星系团样本，给出了$Y_{\text{SZ}}$（积分Sunyaev-Zeldovich信号）与$M_{500}^{Y_{\text{X}}}$（由X射线观测导出的星系团质量）之间新的标度关系，并将其与Planck合作团队基于ESZ子样本的XMM-Newton观测结果进行了比较。利用来自CCCP和MENeaCS已发表的弱引力透镜数据，我们针对新的标度关系以及Planck合作团队给出的标度关系，在Planck宇宙学星系团样本的一个子集上校准了质量偏差。我们提出了一种解释选择效应的新方法，发现对于Chandra校准的标度关系，质量偏差为$(1-b)=0.89\pm0.04$，而对于XMM-Newton校准的标度关系，质量偏差为$(1-b)=0.76\pm0.04$。我们将推导出的标度关系应用于完整的Planck宇宙学星系团样本，获得了不受所用X射线样本影响的相同宇宙学约束，结果为$σ_8 =0.77\pm0.02$，$Ω_m=0.31\pm0.02$，以及$S_8= σ_8 \sqrt{Ω_m / 0.3}=0.78\pm0.02$。我们还提供了将标度关系的红移演化从数据中拟合得到的约束结果，而不是将其固定为自相似值。我们发现红移演化显著偏离自相似值，导致更高的$S_8=0.81\pm0.02$。我们将我们的结果与各种宇宙学探针的结果进行了比较，发现我们的$S_8$约束与文献中最紧的约束相当。当假设自相似红移演化时，我们的约束与大多数晚期探针一致，但与CMB原初各向异性的约束存在张力。当放宽红移演化假设并将其拟合到数据时，我们发现与晚期探针或CMB的结果均不存在显著张力。

英文摘要：

We provide a new scaling relation between $Y_{\text{SZ}}$, the integrated Sunyaev-Zeldovich signal and $M_{500}^{Y_{\text{X}}}$, the cluster mass derived from X-ray observations, using a sample of clusters from the Planck Early Sunyaev-Zeldovich (ESZ) catalogue observed in X-rays by Chandra, and compare it to the results of the Planck collaboration obtained from XMM-Newton observations of a subsample of the ESZ. We calibrated a mass bias on a subset of the Planck cosmological cluster sample using published weak-lensing data from CCCP and MENeaCS, for the new scaling relation as well as that from the Planck collaboration. We propose a novel method to account for selection effects and find a mass bias of $(1-b)=0.89\pm0.04$ for the Chandra-calibrated scaling relation, and $(1-b)=0.76\pm0.04$ for the XMM-Newton-calibrated scaling relation. We apply the scaling relations we derived to the full Planck cosmological cluster sample and obtain identical cosmological constraints regardless of the X-ray sample used, with $σ_8 =0.77\pm0.02$, $Ω_m=0.31\pm0.02$, and $S_8= σ_8 \sqrt{Ω_m / 0.3}=0.78\pm0.02$. We also provide constraints with a redshift evolution of the scaling relation fitted from the data instead of fixing it to the self-similar value. We find a redshift evolution significantly deviating from the self-similar value, leading to a higher value of $S_8=0.81\pm0.02$. We compare our results to those from various cosmological probes, and find that our $S_8$ constraints are competitive with the tightest constraints from the literature. When assuming a self-similar redshift evolution, our constraints are in agreement with most late-time probes and in tension with constraints from the CMB primary anisotropies. When relaxing the assumption of redshift evolution and fitting it to the data, we find no significant tension with results from either late-time probes or the CMB.

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