Debiased Galaxy Cluster Pressure Profiles from XRay Observations and Simulations
Abstract
We present an updated model for the average cluster pressure profile, adjusted for hydrostatic mass bias by combining results from Xray observations with cosmological simulations. Our model estimates this bias by fitting a power law to the relation between the "true" halo mass and Xray cluster mass in hydrodynamic simulations (IllustrisTNG, BAHAMAS, and MACSIS). As an example application, we consider the REXCESS Xray cluster sample and the universal pressure profile derived from scaled and stacked pressure profiles. We find adjusted masses, M_{500c}, that are ≲15% higher and scaled pressures P/P_{500c} that have ≲35% lower normalization than previously inferred. Our debiased pressure profile (DPP) is wellfit by a generalized NavarroFrenkWhite function, with parameters [P_{0}, c_{500}, α, β, γ] = [5.048, 1.217, 1.192, 5.490, 0.433] and does not require a massdependent correction term. When the DPP is used to model the SunyaevZel'dovich (SZ) effect, we find that the integrated Compton YM relation has only minor deviations from selfsimilar scaling. The thermal SZ angular power spectrum is lower in amplitude by approximately 30%, assuming nominal cosmological parameters (e.g., Ω_{m} = 0.3, σ_{8} = 0.8), and is broadly consistent with recent Planck results without requiring additional bias corrections.
 Publication:

The Astrophysical Journal
 Pub Date:
 February 2021
 DOI:
 10.3847/15384357/abd0ff
 arXiv:
 arXiv:2008.04334
 Bibcode:
 2021ApJ...908...91H
 Keywords:

 Galaxy clusters;
 Largescale structure of the universe;
 Observational cosmology;
 Cosmology;
 Intracluster medium;
 584;
 902;
 1146;
 343;
 858;
 Astrophysics  Cosmology and Nongalactic Astrophysics
 EPrint:
 13 pages, 5 figures, 3 tables