TY - JOUR
T1 - The Three Hundred Project
T2 - The stellar angular momentum evolution of cluster galaxies
AU - Mostoghiu, R.
AU - Knebe, A.
AU - Pearce, F. R.
AU - Power, C.
AU - Lagos, C. D.P.
AU - Cui, W.
AU - Borgani, S.
AU - Dolag, K.
AU - Murante, G.
AU - Yepes, G.
PY - 2021/8/1
Y1 - 2021/8/1
N2 - 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 × 1010h-1Mpdbl 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.
AB - 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 × 1010h-1Mpdbl 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.
KW - Galaxies: clusters: general
KW - Galaxies: evolution
KW - Galaxies: kinematics and dynamics
KW - Methods: numerical
UR - http://www.scopus.com/inward/record.url?scp=85111967332&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202038425
DO - 10.1051/0004-6361/202038425
M3 - Article
AN - SCOPUS:85111967332
SN - 0004-6361
VL - 652
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A10
ER -