Pact

Abstract

The pressure of hot gas in groups and clusters of galaxies is a key physical quantity, which is directly linked to the total mass of the halo and several other thermodynamical properties. In the wake of previous observational works on the hot gas pressure distribution in massive halos, we have investigated a sample of 31 clusters detected in both the Planck and Atacama Cosmology Telescope (ACT), MBAC surveys. We made use of an optimised Sunyaev-Zeldovich (SZ) map reconstructed from the two data sets and tailored for the detection of the SZ effect, taking advantage of both Planck coverage of large scales and the ACT higher spatial resolution. Our average pressure profile covers a radial range going from 0.04 × R500 in the central parts to 2.5 × R500 in the outskirts. In this way, it improves upon previous pressure-profile reconstruction based on SZ measurements. It is compatible, as well as competitive, with constraints derived from joint X-ray and SZ analysis. This work demonstrates the possibilities offered by large sky surveys of the SZ effect with multiple experiments with different spatial resolutions and spectral coverages, such as ACT and Planck.

The gravitational field of X-COP galaxy clusters

“…with P 0 , r s , α, β, and γ as free parameters. This functional form was found to provide a good representation of gas pressure profiles determined from both X-ray and SZ observations (Arnaud et al 2010;Planck Collaboration V 2013;Sayers et al 2013;Bourdin et al 2017;Ghirardini et al 2019;Pointecouteau et al 2021). The pressure gradient can be computed analytically from the reconstructed functional form to recover the mass profile from Eq.…”

Exploring the Mass and Redshift Dependencies of the Cluster Pressure Profile with Stacks on Thermal Sunyaev–Zel’dovich Maps

“…In Pointecouteau et al (2021), the cluster sample consisted of 31 clusters with M 500 ä [3.4, 13.1] × 10 14 M e at z < 0.71, which had been previously listed as SZ sources in both Planckand ACT-based catalogs. A major novelty of this work is that the SZ signal was measured on a joint Planck-ACT Compton parameter map, built from a linear combination of the individual frequency maps resulting from the two surveys, as described in Aghanim et al (2019).…”

“…A summary of the results for the fitted UPP parameters from these works is presented in Table 1, while for a more comprehensive summary, we redirect the reader to Appendix A. Most of these studies have employed a limited set of well-characterized and high-significance clusters in order to measure the cluster pressure profile (Arnaud et al 2010;Planck Collaboration et al 2013;Sayers et al 2016;He et al 2021;Pointecouteau et al 2021). A substantially different approach was adopted in Gong et al (2019;hereafter, G19), with the UPP parameters being fitted over a stack of a large number (∼10 5 ) of regions surrounding luminous red galaxies (LRGs) at z  0.5, assuming the latter to be good tracers of massive dark matter halos.…”

The Evolution and Mass Dependence of Galaxy Cluster Pressure Profiles at 0.05 ≤ z ≤ 0.60 and 4 × 1014 M ⊙ ≤ M 500 ≤ 30 × 1014 M ⊙

“…This lack of consensus exists between the various simulations, between different observational results, and when comparing the simulations to observations. To address this situation better, recent observational studies have demonstrated the power of combining data from different facilities to probe a wide range of radial scales (Planck Collaboration et al 2013;Bartalucci et al 2017;Bourdin et al 2017;Romero et al 2017;Ghirardini et al 2019;Pointecouteau et al 2021), and such data are now becoming available for large samples with well-defined selections. In addition, mock observations of similarly selected samples from large volume simulations are increasingly being used for comparison in order to mitigate systematics related to analysis methods and population statistics (Gianfagna et al 2021;Paliwal et al 2022).…”