Speaker
Description
We present our analysis of the factors that impact the reconstruction of density profiles in galaxy clusters, which are a fundamental tool for studying the properties of the intra-cluster medium and a key ingredient for measuring the total mass radial profiles under the assumption of hydrostatic equilibrium.
We used a sample of 105 galaxy clusters drawn from cosmological simulations mirroring the CHEX-MATE representative sample of 118 clusters selected via the SZ effect. Each simulated cluster's X-ray emission was projected along 40 lines of sight. We leveraged this unique dataset to discriminate and quantify, for the first time, the impact of factors such as intrinsic dynamical state.
We derived density profiles using both the azimuthal mean and median methods and found that, on average, both provide a robust retrieval of the true gas density. However, density reconstruction becomes less reliable as a cluster becomes more morphologically or dynamically disturbed.
We also investigate whether the mean-to-median density method can be used to probe clumpiness. While we find no correlation with cluster dynamical state, there is a clear radial trend, suggesting that this method is not reliable on an individual cluster basis. Finally, these results have been used to interpret the statistical properties of the CHEX-MATE density profiles.
| Would you be interested in presenting a poster if the conference is oversubcribed? | No |
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