J/A+A/702/A105ivo://CDS.VizieR/J/A+A/702/A105doi:10.26093/cds/vizier/bc-ny/lbafCDSCastagna F.Andreon S.Landoni M.Trombetta A.2026-08-03T06:57:38Z2025-10-10T11:27:26ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxy-clustersredshiftedastronomical-modelsGalaxy clusters exhibit heterogeneity in their pressure profiles, even after rescaling, highlighting the need for adequately sized samples to accurately capture variations across the cluster population. We present a Bayesian hierarchical model that simultaneously fits individual cluster parameters and the underlying population distribution, providing estimates of the population-averaged pressure profile and the intrinsic scatter, as well as accurate pressure estimates for individual objects. We introduce a highly flexible, low-covariance, and interpretable parameterization of the pressure profile based on restricted cubic splines. We model the scatter properly accounting for outliers, and we incorporate corrections for beam and transfer function, as required for Sunyaev-Zel'dovich (SZ) data. Our model is applied to the largest non-stacked sample of individual cluster radial profiles, extracted from SPT+Planck Compton-y maps. 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.2025A&A...702A.105Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/702/A105CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/702/A105https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/702/A105http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/702/A105https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/702/A105https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/702/A105http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/702/A105GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/702/A105/table2 (Galaxy clusters and estimated parameters in the population analysis)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/702/A105/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/702/A105/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/702/A105/table2?GETtext/xml+votable180.050000true5.5489-41.73660.0055555555555555566/33224 33235 33509 33515 33540 33594 33614 33718 33765 33826 33894 33989 34001 34087 34181 34202 34323 34891 34910 35007 35121 35147 35168 35171 35209 35346 35493 38966 38973 38975 39067-39068 39443 39463 39531 39552 39577 45421 45433 45498 45543 45963 45965-45966 45973 45984 46009 46045 46127 46139 46272 46301 46484 46499 46612 46739 46770 47509https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/702/A105?format=asciidefaultJ/A+A/702/A105/table2Galaxy clusters and estimated parameters in the population analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of the cluster, SPT-CLJHHMM+DDMMmeta.id;meta.maincharRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainzRedshiftsrc.redshiftfloatM500M5001e+14solMassphys.massfloatE_M500M500 upper error1e+14solMassstat.error;stat.maxfloate_M500M500 lower error1e+14solMassstat.errorfloatY500Y5000.0001Mpc**2stat.fit.paramfloatE_Y500Y500 upper error0.0001Mpc**2stat.error;stat.maxfloate_Y500Y500 lower error0.0001Mpc**2stat.errorfloatYSZIntegrated Compton parameter within 0.75'0.0001arcmin**2stat.fit.paramfloatE_YSZIntegrated Compton parameter upper error0.0001arcmin**2stat.error;stat.maxfloate_YSZIntegrated Compton parameter lower error0.0001arcmin**2stat.errorfloatlogP0? log10 of the scaled pressure estimate at knot 0 (r=0.1*r500)phys.pressurefloatnullableE_logP0? logP0 upper errorstat.error;stat.maxfloatnullablee_logP0? logP0 lower errorstat.errorfloatnullablelogP1? log10 of the scaled pressure estimate at knot 1 (r=0.4*r500)phys.pressurefloatnullableSimbadSimbad column added by the CDSmeta.ref.urlcharE_logP1? logP1 upper errorstat.error;stat.maxfloatnullablee_logP1? logP1 lower errorstat.errorfloatnullablelogP2? log10 of the scaled pressure estimate at knot 2 (r=0.7*r500)phys.pressurefloatnullableE_logP2? logP2 upper errorstat.error;stat.maxfloatnullablee_logP2? logP2 lower errorstat.errorfloatnullablelogP3? log10 of the scaled pressure estimate at knot 3 (r=r500)phys.pressurefloatnullableE_logP3? logP3 upper errorstat.error;stat.maxfloatnullablee_logP3? logP3 lower errorstat.errorfloatnullablelogP4? log10 of the scaled pressure estimate at knot 4 (r=1.3*r500)phys.pressurefloatnullableE_logP4? logP4 upper errorstat.error;stat.maxfloatnullablee_logP4? logP4 lower errorstat.errorfloatnullable