Orateur
Description
The gas mass fraction in galaxy clusters is a convenient probe to use in cosmological studies, as it can help derive constraints on a collection of cosmological parameters.
It is however subject to various effects from the baryonic physics inside galaxy clusters, which may bias the obtained cosmological constraints.
Among different aspects of the baryonic physics, in this presentation I focus on the impact of the hydrostatic equilibrium assumption.
I analyse the hydrostatic mass bias $B$, constraining a possible mass and redshift evolution of this quantity and its impact on the cosmological constraints.
To that end I consider cluster observations of the $Planck$-ESZ sample and evaluate the gas mass fraction using X-ray counterpart observations.
I show a degeneracy between the redshift dependence of the bias and cosmological parameters.
In particular I find a $3.8 \sigma$ evidence for a redshift dependence of the bias when assuming a $Planck$ prior on $\Omega_m$.
On the other hand, assuming a constant mass bias would lead to the extreme large value of $\Omega_m > 0.860$.
I however show that these results are entirely dependent on the cluster sample I consider.
In particular, the mass and redshift trends that I find for the lowest mass-redshift and highest mass-redshift clusters of our sample are not compatible.
Nevertheless, in all the analyses I find a value for the amplitude of the bias that is consistent with $B \sim 0.8$, as expected from hydrodynamical simulations and local measurements, but still in tension with the low value of $B \sim 0.6$ derived from the combination of cosmic microwave background primary anisotropies with cluster number counts.
I will also discuss cosmological constraints obtained from gas fraction data, combined with other probes like cluster number counts.
