Connecting galaxy evolution in clusters with their radial profiles and phase space distribution: results from the IllustrisTNG hydrodynamical simulations

• DOI: 10.1093/mnras/stac392
• Publication Date: 2022-02-11T04:12:53Z
• Authors: Tara Dacunha; Matthew Belyakov; Susmita Adhikari; Tae-hyeon Shin; Samuel Goldstein; Bhuvnesh Jain
• Keywords: Cosmology and Nongalactic Astrophysics (astro-ph.CO); galaxies: clusters: general –galaxies: evolution –galaxies: kinematics and dynamics –galaxies: star formation; FOS: Physical sciences; Astronomy and Astrophysics; 530; Astrophysics - Astrophysics of Galaxies; 01 natural sciences; 520; Space and Planetary Science; Astrophysics of Galaxies (astro-ph.GA); 0103 physical sciences; Astrophysics - Cosmology and Nongalactic Astrophysics

ABSTRACT We study the population of galaxies around galaxy clusters in hydrodynamic simulation suite IllustrisTNG 300-1 to signatures their evolutionary history on observable properties. measure radial number density profile, phase space distribution, and splashback radius for different masses colours over redshift range z = 0−1. The three primary physical effects which shape distribution within are quenching, angular momentum dynamical friction. find distinct populations by applying a Gaussian mixture model colour mass. They have histories leave cluster haloes. that low-mass red show most concentrated largest radius, while high-mass less smaller radius. Blue galaxies, mostly quench into population, shallowest clusters, with those orbits quenched rapidly before reaching pericentre. Comparison from Dark Energy Survey survey Sunyaev–Zeldovich Atacama Cosmology Telescope South Pole surveys shows evidence differences evolution between simulations data.