  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 and the Cosmic Microwave Background, that are mixed-up 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 modelling
allowed us to analyze a sample of 61 nearby members of the Planck catalog 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.
