Abstract
We present MG-MAMPOSSt, a license-free code to constrain modified gravity models by reconstructing the mass profile of galaxy clusters with the kinematics of the cluster’s member galaxies. We describe the main features of the code and we show the capability of the method when the kinematic information is combined with lensing data. We discuss recent results and forecasts on two classes of models currently implemented in the code, characterized by different screening mechanisms, namely, chameleon and Vainshtein screening. We further explore the impact of possible systematics in view of application to the data from upcoming surveys.
Highlights
We developed MG-MAMPOSS T, a FORTRAN code which determines cluster mass profiles in modified gravity from the kinematics of cluster members; the program is based upon the MAMPOSS T method of [12]
We assume that all the systematics are under control, i.e., particles in each halo follow an NFW distribution and their velocity is assigned by assuming that σr2 is given by Equation (6)
We considered a total of 20 synthetic massive cluster-size haloes generated in GR5, as a reasonable number of relaxed galaxy clusters for which high-quality data could be available from upcoming surveys
Summary
In order to match observational constraints on small scales and dense environments, the fifth force should be further suppressed through a so-called screening mechanism, which relies on the non-linear interaction of the scalar field (e.g., [5]) In this framework, galaxy clusters constitute a powerful tool to investigate modification of gravity at large scales (see [6] for a recent review); in particular, with the combination of the cluster’s mass profiles derived with lensing and internal kinematic analyses of the hot intra-cluster gas (e.g., [7–9]) and of cluster’s member galaxies (e.g., [10,11]), it is possible to constrain departures from General Relativity (GR) in a complementary way with respect to other cosmological and astrophysical observations.
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