The chameleon screening mechanism has been constrained many a time using dynamic and kinematic galaxy cluster observables. Current constraints are, however, insensitive to different mass components within galaxy clusters and have been mainly focused on a single mass density profile, the Navarro-Frenk-White mass density model. In this work, we extend the study of the Chameleon screening mechanism in galaxy clusters by considering a series of mass density models, namely: generalized-Navarro-Frenk-While, b-Navarro-Frenk-While, Burket, Isothermal and Einasto. The coupling strength (β) and asymptotic value of the chameleon field (ϕ _∞) are constrained by using kinematics analyses of simulated galaxy clusters, generated both assuming General Relativity and a strong chameleon scenario. By implementing a Bayesian analysis we comprehensively show that the biases introduced due to an incorrect assumption of the mass model are minimal. Similarly, we also demonstrate that a spurious detection of evidence for modifications to gravity is highly unlikely when utilizing the kinematics of galaxy clusters.

中文翻译：

---

修正引力下星系团的质量建模和运动学


变色龙筛选机制已经多次使用动力学和运动学星系团可观测对象受到限制。然而，目前的约束对星系团中的不同质量分量不敏感，并且主要集中在单一的质量密度剖面上，即 Navarro-Frenk-White 质量密度模型。在这项工作中，我们通过考虑一系列质量密度模型来扩展对星系团中变色龙筛选机制的研究，即：广义的 Navarro-Frenk-While、b-Navarro-Frenk-While、Burket、Isothermal 和 Einasto。变色龙场的耦合强度 （β） 和渐近值 （φ_∞） 通过使用模拟星系团的运动学分析来约束，该分析在假设广义相对论和强变色龙情景下生成。通过实施贝叶斯分析，我们全面表明，由于质量模型的错误假设而引入的偏差是最小的。同样，我们还证明，当利用星系团的运动学时，对引力改变证据的虚假检测是极不可能的。