Hydrodynamical simulations of galaxy clusters in dark energy cosmologies: II. c-M relation

TL;DR

This study uses hydrodynamical simulations to analyze how different dark energy models affect the concentration-mass relation in galaxy clusters, revealing model-dependent variations influenced by baryon physics and relaxation states.

Contribution

It provides the first detailed comparison of the c-M relation across multiple dark energy cosmologies using hydrodynamical simulations, including baryonic effects and relaxation criteria.

Findings

The definition of concentration affects its measured value by up to 20%.

Relaxed objects show higher normalization and shallower slopes in the c-M relation.

Baryon physics impacts high-mass systems more significantly than low-mass ones.

Abstract

We use hydrodynamical simulations of different dark energy cosmologies to investigate the concentration-mass (c-M) relation in galaxy clusters. In particular, we consider a reference \Lambda CDM model, two quintessence models with inverse power-law potentials (RP and SUGRA), and two extended quintessence models, one with positive and one with negative coupling with gravity (EQp and EQn respectively). All the models are normalized in order to match CMB data from WMAP3. We fit both the dark matter only and the total mass profile with a NFW profile, and recover the concentration of each halo from the fit using different definition. We consider both the complete catalog of clusters and groups and subsamples of objects at different level of relaxation. We find that the definition itself of the concentration can lead to differences up to 20% in its value and that these differences are smaller when more relaxed objects are considered. The c-M relation of our reference \Lambda CDM model is in good agreement with the results in literature, and relaxed objects have a higher normalization and a shallower slope with respect to the complete sample. The inclusion of baryon physics is found to influence more high-mass systems than low-mass ones, due to a higher concentration of baryons in the inner regions of massive halos. For the different dark energy models, we find that for \Lambda CDM, RP and SUGRA the normalization of the c-M relation is linked to the growth factor, with models having a higher value of \sigma 8 D+ having also a higher normalization. This simple scheme is no longer valid for EQp and EQn because in these models a time dependent effective gravitational interaction, whose redshift evolution depends on the sign of the coupling, is present. This leads to a decrease (increase) of the expected normalization in the EQp (EQn) model. [Abridged]