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.
