标题： CHEX-MATE：三维聚类多探针（CLUMP-3D）II。来自X射线、SZE和WL的组合气体和暗物质分析 显示英文标题

标题： CHEX-MATE: Cluster Multi-Probes in Three Dimensions (CLUMP-3D) II. Combined Gas and Dark Matter Analysis from X-ray, SZE, and WL

摘要： 在分层结构形成的标准模型下，星系团的整体几何形状比球体更适用于三轴椭圆来描述。 因此，应用球对称模型可能导致显著的偏差。 这些偏差可以通过拟合三轴模型来减轻，这需要深度多探针数据和一组物理上有根据的模型来描述它们。 在这里，我们提出了一种基于集群遗产项目中星系团数据的多探针三轴分析方法，该数据包括XMM-Newton - 结构形成终点的质晕和热力学（CHEX-MATE），其中包括来自XMM-Newton的X射线数据，来自Planck和ACT的SZ数据，以及来自Subaru的WL数据。 这项工作建立在我们之前在论文I中开发的仅气体X射线和SZ三轴拟合形式基础上。 我们将我们的方法应用于CHEX-MATE星系团PSZ2 G313.33+61.13（Abell 1689），发现其沿视线方向相对于天球平面延长了一个因子$\mathcal{R}_{LP} = 1.27 \pm 0.02$。 因此，从我们的三轴拟合得到的WL质量，$\text{M}_{200c}=(13.69_{-1.41}^{+1.56})\times10^{14} \text{M}_{\odot}$，明显低于从采用相同方法的球对称拟合得到的值$(17.77_{-1.75}^{+2.00})\times10^{14} \text{M}_{\odot}$。 我们的三轴拟合发现浓度为$c_{200c}=8.55_{-1.61}^{+2.20}$，与球对称值$9.99_{-1.78}^{+2.26}$一致，这表明Abell 1689中意外高的浓度不是由于三轴性和取向造成的。 我们还测量了半径在0.18-1.37 Mpc之间的非热压力分数，发现中间半径处的最小值约为20%，在最小和最大半径处增加到接近30%，典型的测量精度为$\pm$5%。 显示英文摘要

摘要： Under the standard model of hierarchical structure formation, the overall geometry of galaxy clusters is better described by a triaxial ellipse than a sphere. As a result, applying spherically-symmetric models can result in significant biases. These biases can be mitigated by fitting a triaxial model, requiring deep multiprobe data and a set of physically motivated models to describe them. Here we present a multiprobe triaxial analysis methodology based on the data available for galaxy clusters in the Cluster Heritage project with XMM-Newton - Mass Assembly and Thermodynamics at Endpoint of structure formation (CHEX-MATE), which includes X-ray data from XMM-Newton, SZ data from Planck and ACT, and WL data from Subaru. This work builds on our previous development of a gas-only X-ray and SZ triaxial fitting formalism in Paper I. We apply our approach to the CHEX-MATE cluster PSZ2 G313.33+61.13 (Abell 1689) and find that it is elongated along the line of sight relative to the plane of sky by a factor of $\mathcal{R}_{LP} = 1.27 \pm 0.02$. As a result, the WL mass obtained from our triaxial fit, $\text{M}_{200c}=(13.69_{-1.41}^{+1.56})\times10^{14} \text{M}_{\odot}$, is significantly lower than the value of $(17.77_{-1.75}^{+2.00})\times10^{14} \text{M}_{\odot}$ obtained from a spherically-symmetric fit that otherwise employs the same methodology. Our triaxial fit finds a concentration of $c_{200c}=8.55_{-1.61}^{+2.20}$, consistent with the spherically-symmetric value of $9.99_{-1.78}^{+2.26}$, which suggests that the unexpectedly high concentration in Abell 1689 is not due to triaxiality and orientation. We also measure the non-thermal pressure fraction at radii between 0.18-1.37 Mpc, finding a minimum of approximately 20 per cent at intermediate radii increasing to near 30 per cent at both the smallest and largest radii, and with a typical measurement precision of $\pm$5 per cent.