Description
Multiwavelength data on the most observed galaxy clusters allows for comprehensive mass modelling of each component: dark matter, intra-cluster gas, the galaxy's baryons, and the intra-cluster stars. Such modelling could be done with a combination of multiple mass probes, constraining the total mass of each individual baryonic component, but no method for such modelling has been released.
Recent studies have shown that it was possible to make a self-consistent mass distribution model separating the intra-cluster gas from the rest of the mass to benefit from X-ray constraints (Beauchesne et al., 2024). The first JWST observations demonstrated its ability to map the intra-cluster light in a fraction of the observing time previously required and allowed its inclusion into galaxy cluster mass models with an approach similar to the X-ray gas.
I will present a modified version of the method presented in Beauchesne et al. (2024), where we include a new mass component to reproduce the ICL. We extend the set of observables by adding direct constraints on the velocity dispersions for the cluster member and the ICL. The produced models can be split into each main cluster component, and each baryon component is fitted on specific observables jointly with the lensing. I will present the early results obtained on the cluster test case, Abell S1063. I will compare the stellar-mass-to-light ratio from the favoured mass model to its estimation with spectral energy density fit. In the case of Abell S1063, we found a relative agreement between those two probes.
