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Successive releases of Planck data have demonstrated the strength of theSunyaev--Zeldovich (SZ) effect in detecting hot baryons out to the galaxycluster peripheries. To infer the hot gas pressure structure from nearby galaxyclusters to more distant objects, we developed a parametric method that modelsthe spectral energy distribution and spatial anisotropies of both the Galacticthermal dust and the Cosmic Microwave Background, that are mixed-up with thecluster SZ and dust signals. Taking advantage of the best angular resolution ofthe High Frequency Instrument channels (5 arcmin) and using X-ray priors in theinnermost cluster regions that are not resolved with Planck, this modellingallowed us to analyze a sample of 61 nearby members of the Planck catalog of SZsources ($0 < z < 0.5$, $\tilde{z} = 0.15$) using the full mission data, aswell as to examine a distant sample of 23 clusters ($0.5 < z < 1$, $\tilde{z} =0.56$) that have been recently followed-up with XMM-Newton and Chandraobservations. We find that (i) the average shape of the mass-scaled pressureprofiles agrees with results obtained by the Planck collaboration in the nearbycluster sample, and that (ii) no sign of evolution is discernible betweenaveraged pressure profiles of the low- and high-redshift cluster samples. Inline with theoretical predictions for these halo masses and redshift ranges,the dispersion of individual profiles relative to a self-similar shape stayswell below 10 % inside $r_{500}$ but increases in the cluster outskirts.

Pressure profiles of distant galaxy clusters in the Planck catalog