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.
Highlights
A power-law relation between the electron pressure and mass, P − M2/3, is valid under the assumption that the galaxy-formation process is dominated by gravity, called selfsimilar relation
We have 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
The gas deficit may be caused by AGN feedback: the response of the intracluster medium (ICM) to the relativistic plasma ejected by the active galactic nuclei (AGN) [6]
Summary
A power-law relation between the electron (or gas) pressure and mass, P − M2/3, is valid under the assumption that the galaxy-formation process is dominated by gravity, called selfsimilar relation. Any deviation from this relation points to the presence of more complex processes such as baryonic feedback effects. Numerous X-ray observations find a deficit of baryonic gas inside low-mass halos compared to the cosmic average baryon fraction [2–5], implying the deviation from the self-similar scaling relation. The AGN feedback is key for understanding the evolution of galaxies and the formation of large-scale structures; not well understood
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