The SAMI Galaxy Survey: mass as the driver of the kinematic morphology - density relation in clusters

Sarah Brough, Jesse van de Sande, Matt S. Owers, Francesco d'Eugenio, Rob Sharp, Luca Cortese, Nicholas Scott, Scott M. Croom, Rob Bassett, Kenji Bekki, Julia J. Bryant, Roger Davies, Michael J. Drinkwater, Simon P. Driver, Caroline Foster, Gregory Goldstein, A. R. Lopez-Sanchez, Anne M. Medling, Sarah M. Sweet, Dan S. Taranu, Chiara Tonini, Sukyoung K. Yi, Michael Goodwin, J. S. Lawrence, Samuel N. Richards

Published 2017-04-04Version 1

We examine the kinematic morphology of early-type galaxies (ETGs) in eight galaxy clusters in the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey. The clusters cover a mass range of 14.2<log(M_200/M_sun)<15.2 and we measure spatially-resolved stellar kinematics for 293 cluster members within 1R_200 of the cluster centers. We calculate the spin parameter, lambda_R for these galaxies and use that to classify the kinematic morphology of the galaxies as fast (high spin parameter) or slow (low spin parameter) rotators. The total fraction of slow rotators in the early-type galaxy population, F_SR=0.14+/-0.02 and does not depend on host cluster mass. Across the eight clusters, the fraction of slow rotators increases with increasing local environmental overdensity. We also find that the slow-rotator fraction increases at small clustercentric radii (R_cl<0.3R_200), and note that there is also an enhancement in slow-rotator fraction at R_cl~0.6R_200 in cluster substructure. We find the strongest increase in slow-rotator fraction occurs with increasing stellar mass. After accounting for the strong correlation with stellar mass, we find no significant relationship between spin parameter and local overdensity in the cluster environment. We therefore conclude that the primary driver for the kinematic morphology--density relationship in galaxy clusters is the changing distribution of galaxy stellar mass with local environment. The presence of slow rotators in cluster substructure suggests that the cluster kinematic morphology--density relationship is a result of mass segregation of slow-rotating galaxies forming in galaxy groups that later merge with clusters and sink to the cluster center via dynamical friction.