Galaxy clusters pressure profiles

This is a complete sample of 55 clusters, with 0.05<z<0.30 and M500>4*10^14^M_{sun}_, enabling subdivision into sizable morphological classes based on eROSITA data. Fitting is computationally feasible within a few days on a modern (2024) personal computer. The shape of the population-averaged pressure profile, at our 250kpc FWHM resolution, closely resembles the universal pressure profile, despite the flexibility of our model to accommodate alternative shapes, with a 12% lower normalization, similar to what is needed to alleviate the tension between cosmological parameters derived from the cosmic microwave background and Planck SZ cluster counts.

Beyond r500, our pressure profile is steeper than previous determinations. The intrinsic scatter is consistent with or lower than previous estimates, despite the broader diversity expected from our SZ selection. Our flexible pressure modelization identifies a few clusters with non-standard concavity in their radial profiles but no outliers in amplitude.

When dividing the sample by morphology, we find remarkably similar pressure profiles across classes, though regular clusters show evidence of lower scatter and a more centrally peaked profile compared to disturbed ones.