Title: Hydrostatic mass profiles in X-COP galaxy clusters Show Chinese title

Title: X-COP星系团的静压质量分布

Abstract: We present the reconstruction of the hydrostatic mass profiles in 13 X-ray luminous galaxy clusters that have been mapped in their X-ray and SZ signal out to $R_{200}$ for the XMM Cluster Outskirt Project (X-COP). Using profiles of the gas temperature, density and pressure that have been spatially resolved out to $0.9 R_{500}$, $1.8 R_{500}$, and $2.3 R_{500}$, respectively, we are able to recover the hydrostatic gravitating mass profile with several methods and using different mass models. The hydrostatic masses are recovered with a relative (statistical) error of 3% at $R_{500}$ and 6% at $R_{200}$. We evaluate some of the systematic uncertainties to be in the order of 5% at both $R_{500}$ and $R_{200}$. A Navarro-Frenk-White profile provides the best-fit in 9 cases, with the remaining four cases that do not show a statistically significant tension with it. The distribution of the mass concentration follows the correlations with the total mass predicted from numerical simulations with a scatter of 0.18 dex. We compare them with the estimates of the total gravitational mass obtained through X-ray scaling relations, and from weak lensing and galaxy dynamics techniques, and measure a substantial agreement with the results from scaling laws, from WL at both $R_{500}$ and $R_{200}$, from cluster velocity dispersions, but a significant tension with the caustic masses that tend to underestimate the hydrostatic masses by 40% at $R_{200}$. We also compare these measurements with predictions from alternative models to CDM, like the Emergent Gravity and MOND scenarios, confirming that the latter underestimates the hydrostatic masses by 40% at $R_{1000}$, with a decreasing tension as the radius increases, and reaches $\sim$15% at $R_{200}$, whereas the former reproduces $M_{500}$ within 10%, but overestimates $M_{200}$ by about 20%. Show Chinese abstract

Abstract: 我们展示了对13个X射线明亮星系团的静压质量轮廓的重建，这些星系团已经在X射线和SZ信号方面被绘制出来，直至$R_{200}$，这是XMM星系团外围项目（X-COP）的一部分。 利用在空间上解析至$0.9 R_{500}$、$1.8 R_{500}$和$2.3 R_{500}$的气体温度、密度和压力轮廓，我们能够使用多种方法和不同的质量模型恢复静压引力质量轮廓。 在$R_{500}$处，静压质量的相对（统计）误差为3%，在$R_{200}$处为6%。 我们评估了一些系统不确定性，在$R_{500}$和$R_{200}$处约为5%。 Navarro-Frenk-White模型在9种情况下提供了最佳拟合，其余四种情况与该模型没有统计显著的矛盾。 质量浓度的分布遵循数值模拟预测的总质量相关性，离散度为0.18 dex。 我们将它们与通过X射线标度关系、弱引力透镜和星系动力学技术获得的总引力质量估计进行比较，发现与标度定律的结果、在$R_{500}$和$R_{200}$处的弱引力透镜结果以及团簇速度弥散的结果有显著的一致性，但与倾向于在$R_{200}$处低估静力质量40%的尖点质量存在显著矛盾。 我们还将这些测量结果与替代模型的预测进行了比较，如引 emergent gravity 和 MOND 场景，确认后者在$R_{1000}$处低估了流体静力质量 40%，随着半径增加，矛盾逐渐减小，并在$R_{200}$处达到$\sim$的 15%，而前者在$M_{500}$范围内重现了数据，但大约高估了$M_{200}$的 20%。