Constraining AGN feedback model with SZ profile

¹ Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale, Bâtiment 121, 91405 Orsay, France
² Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, Canada
³ Canadian Institute for Advanced Research, 180 Dundas St W, Toronto, ON M5G 1Z8, Canada
⁴ Canada Research Chair in Observational Cosmology
⁵ Astrophysics Research Institute, Liverpool John Moores University, Liverpool, L3 5RF, United Kingdom
⁶ Astrophysics and Cosmology Research Unit, School of Chemistry and Physics University of KwaZulu-Natal, Durban, South Africa
⁷ NAOC-UKZN Computational Astrophysics Center (NUCAC), University of KwaZulu-Natal, Durban, 4000
⁸ Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK
⁹ Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK
¹⁰ Instituto de Fisica, Universidade Federal do Rio de Janeiro, 21941-972, Rio de Janeiro, RJ, Brazil

^* e-mail: hideki.tanimura@ias.u-psud.fr

Published online: 17 January 2022

Abstract

Relativistic jets from AGN have a wide range of impacts on galaxy groups and clusters and are key for understanding their formation and physical properties. However, this non-gravitational process is not well understood. Galaxy groups with shallow gravitational potentials are ideal laboratories to study and constrain the AGN feedback model. We studied hot gas in ∼66,000 SDSS LRG halos with an average halo mass of 3×10¹³ M_⊙ using the Planck tSZ map. We have detected their average tSZ radial profile at ∼17σ and compared it with the cosmo-OWLS cosmological hydrodynamical simulations with different AGN feedback models. The best agreement has been obtained for the AGN 8.0 model in the simulations. We have also compared our measured tSZ profile with the prediction from the universal pressure profile assuming the self-similar relation and found them consistent if the model accounts for the clustering of neighboring haloes via a two-halo term.