  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-While 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
($\beta$) and asymptotic value of the chameleon field ($\phi_\infty$) 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.
