Speaker
Description
In a self-similar paradigm of structure formation, the thermal pressure of the hot intra-cluster gas follows a universal distribution independent of the mass scale. Thus, this thermal pressure distribution is universal in every cluster once normalised to the proper mass and redshift dependencies. The reconstruction of such a universal pressure profile requires an individual estimate of the mass of each cluster. In this context, I will present a method to jointly fit the universal pressure profile and individual cluster masses over a sample of galaxy clusters, properly accounting for correlations between the profile shape and amplitude, and masses scaling the individual profiles. I will investigate the propagation of the uncertainties on the fitted masses and profiles onto the SZ power spectrum and subsequently on the cosmological parameters. I will present the results of the application of this framework to a subsample of 28 CHEX-MATE clusters.
| Would you be interested in presenting a poster if the conference is oversubcribed? | Yes |
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