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

Title: X-COP星系团中的流体静力质量分布profiles

Abstract: We present the reconstruction of 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-Newton Cluster Outskirts Project (X-COP). Using profiles of the gas temperature, density and pressure that have been spatially resolved out to (median value) 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) median error of 3% at $R_{500}$ and 6% at $R_{200}$. By using several different methods to solve the equation of the hydrostatic equilibrium, we evaluate some of the systematic uncertainties to be of the order of 5% at both $R_{500}$ and $R_{200}$. A Navarro-Frenk-White profile provides the best-fit in nine cases out of 13, 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, with an intrinsic scatter on the hydrostatic masses of 0.15 dex. We compare them with the estimates of the total gravitational mass obtained through X-ray scaling relations applied to $Y_X$, gas fraction and $Y_{SZ}$, 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 $R_{200}$ (with differences below 15%), 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 the Cold Dark Matter, like the "Emergent Gravity" and MOND scenarios. Show Chinese abstract

Abstract: 我们展示了在X射线最亮星系团的重力质量分布重建，这些星系团被映射到$R_{200}$范围内的X射线和SZ信号，属于XMM星系团外围项目（X-COP）。 利用分别在中值为0.9$R_{500}$、1.8$R_{500}$和2.3$R_{500}$处解析得到的气体温度、密度和压力剖面，我们能够用几种方法并采用不同的质量模型恢复出重力质量分布。重力质量在$R_{500}$处以相对（统计）中值误差3%恢复，在$R_{200}$处以相对中值误差6%恢复。 通过使用几种不同的方法来求解流体静力平衡方程，我们评估了一些系统不确定度，在$R_{500}$和$R_{200}$处的量级约为 5%。 Navarro-Frenk-White（NFW）分布模型在 13 种情况中有 9 种提供了最佳拟合，其余 4 种情况并未显示出与该模型有显著统计学上的矛盾。 质量浓度的分布遵循总质量与数值模拟预测的相关性，其分散程度为 0.18 dex，流体静力学质量的固有分散程度为 0.15 dex。 我们将它们与通过 X 射线尺度关系估算的总引力质量进行比较，这些关系应用于$Y_X$、气体分数和$Y_{SZ}$，并从弱透镜技术和星系动力学技术中获得，并测量出与尺度定律的结果有实质性的符合，与$R_{500}$和$R_{200}$处的弱透镜（WL）结果一致（差异低于 15%），以及与星团速度弥散一致，但与倾向于在$R_{200}$处低估流体静力学质量 40% 的激波质量存在显著矛盾。 我们还把这些测量结果与冷暗物质替代模型的预测进行比较，比如“涌现引力”和 MOND 场景。