Pressure Profiles of Distant Galaxy Clusters in the Planck Catalogue

Successive releases of Planck data have demonstrated the strength of the Sunyaev-Zeldovich (SZ) effect in detecting hot baryons out to the galaxy cluster peripheries. To infer the hot gas pressure structure from nearby galaxy clusters to more distant objects, we developed a parametric method that models the spectral energy distribution and spatial anisotropies of both the Galactic thermal dust (GTD) and the cosmic microwave background (CMB), which are combined with the cluster SZ and dust signals. Taking advantage of the best angular resolution of the High Frequency Instrument channels (5 arcmin) and using X-ray priors in the innermost cluster regions that are not resolved with Planck, this modeling allowed us to analyze a sample of 61 nearby members of the Planck Catalogue of SZ sources (0< z< 0.5, \tilde{z}=0.15) using the full mission data, as well 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 Chandra observations. We find that (I) the average shape of the mass-scaled pressure profiles agrees with results obtained by the Planck Collaboration in the nearby cluster sample, and that (II) no sign of evolution is discernible between averaged pressure profiles of the low- and high-redshift cluster samples. In line with theoretical predictions for these halo masses and redshift ranges, the dispersion of individual profiles relative to a self-similar shape stays well below 10% inside r ₅₀₀ but increases in the cluster outskirts.