KiDS-DR3中的AMICO星系团：来自大尺度叠加弱透镜轮廓的宇宙学约束
AMICO galaxy clusters in KiDS-DR3: cosmological constraints from large-scale stacked weak lensing profiles
摘要：
上下文围绕着星系团的暗物质晕的大尺度质量分布提供了敏感的宇宙学信息。目的。在这项工作中，我们利用一个大的光度星系团样本，从公开的第三次数据发布的千度巡天，和相应的剪切信号，评估集群质量和测试的一致性$Λ$ -冷暗物质（$Λ$ CDM）模型。特别是，我们研究了弱引力透镜效应的规模超过集群维里半径，其中的信号是由相关和不相关的物质密度分布沿视线。分析的目录包括6962个星系团，在红移范围$0.1 \leq z \leq 0.6$和信噪比大于3.5。方法.我们执行一个完整的贝叶斯分析，这些集群的堆叠剪切剖面模型。所采用的似然函数既考虑了小规模的1-晕项，主要用于约束集群的结构特性，和2-晕项，可用于约束宇宙学参数。结果我们发现，所采用的建模是成功的，以评估集群质量和总物质密度参数，$Ω_M$，拟合剪切剖面时，最大的可用尺度为35 Mpc/h。此外，我们的结果为星系团的叠加引力透镜中的2晕信号提供了强有力的观测证据，进一步证明了该探测器在宇宙学研究中的可靠性。这项工作的主要结果是一个强大的约束$Ω_M$，假设平坦的$Λ$ CDM宇宙学。我们得到$Ω_M = 0.29 \pm 0.02$，估计从全后验概率分布，符合估计从宇宙微波背景实验。
英文摘要：
Context. The large-scale mass distribution around dark matter haloes hosting galaxy clusters provides sensitive cosmological information. Aims. In this work, we make use of a large photometric galaxy cluster sample, constructed from the public Third Data Release of the Kilo-Degree Survey, and the corresponding shear signal, to assess cluster masses and test the concordance $Λ$-cold dark matter ($Λ$CDM) model. In particular, we study the weak gravitational lensing effects on scales beyond the cluster virial radius, where the signal is dominated by correlated and uncorrelated matter density distributions along the line-of-sight. The analysed catalogue consists of 6962 galaxy clusters, in the redshift range $0.1 \leq z \leq 0.6$ and with signal-to-noise ratio larger than 3.5. Methods. We perform a full Bayesian analysis to model the stacked shear profiles of these clusters. The adopted likelihood function considers both the small-scale 1-halo term, used primarily to constrain the cluster structural properties, and the 2-halo term, that can be used to constrain cosmological parameters. Results. We find that the adopted modelling is successful to assess both the cluster masses and the total matter density parameter, $Ω_M$, when fitting shear profiles up to the largest available scales of 35 Mpc/h. Moreover, our results provide a strong observational evidence of the 2-halo signal in the stacked gravitational lensing of galaxy clusters, further demonstrating the reliability of this probe for cosmological studies. The main result of this work is a robust constraint on $Ω_M$, assuming a flat $Λ$CDM cosmology. We get $Ω_M = 0.29 \pm 0.02$, estimated from the full posterior probability distribution, consistent with the estimates from cosmic microwave background experiments.
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