Cosmological constraints from the Planck cluster catalogue with DES shear profiles and Chandra observations

Abstract

We present cosmological constraints from the PSZ2 cosmological cluster sample, using weak-lensing shear profiles from Dark Energy Survey (DES) data and X-ray observations from the telescope for the mass calibration. We compute hydrostatic mass estimates for all clusters in the PSZ2 sample with a scaling relation between their integrated Sunyaev-Zeldovich signal and X-ray-derived hydrostatic mass, calibrated with the data. We introduce a method to correct these masses with a hydrostatic mass bias using shear profiles derived from wide-field galaxy surveys. We simultaneously fit the number counts of the PSZ2 sample and the mass calibration with the DES data, finding Ω_ =0.312^ Planck Chandra Chandra m +0.018 _ -0.024 , σ_8=0.777± 0.024, S_8≡ σ_8 =0.791^ Ω_ / 0.3 m +0.023 _ -0.021 , and $(1-b)=0.844^ +0.055 _ -0.062 $ for our baseline analysis when combined with baryon acoustic oscillation data. When considering a hydrostatic mass bias evolving with mass, we find Ω_ =0.353^ m +0.025 _ -0.031 , σ_8=0.751± 0.023, and S_8=0.814^ +0.019 _ -0.020 . We verify the robustness of our results by exploring a variety of analysis settings, with a particular focus on the definition of the halo centre used for the extraction of shear profiles. We compare our results with a number of other cosmological analyses, in particular two recent analyses of cluster samples obtained from SPT and eROSITA data that share the same mass calibration data set. We find that our results are in overall agreement with most late-time probes, in very mild tension with CMB results (1.6σ), and in significant tension with results from eROSITA clusters (2.9σ). We confirm that our mass calibration is consistent with the eROSITA analysis by comparing masses for clusters present in both and eROSITA samples, eliminating it as a potential cause of tension. We also compare our results with previous studies of the PSZ2 sample, finding a good agreement between the constraints derived in this work and previous constraints derived with the same sample, validating the use of wide-field lensing data for cluster mass calibration. Planck