The Three Hundred Project: The stellar angular momentum evolution of cluster galaxies

Abstract

Using 324 numerically modelled galaxy clusters as provided by THE THREE HUNDRED project, we study the evolution of the kinematic properties of the stellar component of haloes on first infall. We selected objects with Mstar > 5 × 1010 h−1 M⊙ within 3R200 of the main cluster halo at z = 0 and followed their progenitors. We find that although haloes are stripped of their dark matter and gas after entering the main cluster halo, there is practically no change in their stellar kinematics. For the vast majority of our ‘galaxies’ – defined as the central stellar component found within the haloes that form our sample – their kinematic properties, as described by the fraction of ordered rotation, and their position in the specific stellar angular momentum−stellar mass plane jstar − Mstar are mostly unchanged by the influence of the central host cluster. However, for a small number of infalling galaxies, stellar mergers and encounters with remnant stellar cores close to the centre of the main cluster, particularly during pericentre passage, are able to spin up their stellar component by z = 0.

The THREEHUNDRED project: the effect of baryon processes at galaxy cluster scale

“…Furthermore, the cluster backsplash galaxies [19,20] and shock radius [21] have also been well addressed. The advanced baryon models in hydrodynamic simulations allow us to perform a detailed investigation on the cluster properties, such as profiles [22,23], substructure and its baryonic content [24][25][26][27], dynamical state and morphology [28,29], cluster (non-)thermalization [30,31], the fundamental plane [32], and the cluster mass biases [33, for hydrostatic-equilibrium assumption], [34, for sigma-mass relation] and [35, for weaklensing]. Lastly, comparing to the void/field region runs in this project allows us to study the effect of environment [36]; including the self-interacting dark matter run allow us to constrain the dark matter cross-section [37]; It further help us to examine the chameleon gravity [38].…”