The SAMI Galaxy Survey: Asymmetry in Gas Kinematics and its links to Stellar Mass and Star Formation

J. V. Bloom, L. M. R. Fogarty, S. M. Croom, A. Schaefer, J. J. Bryant, L. Cortese, S. Richards, J. Bland-Hawthorn, I-T. Ho, N. Scott, G. Goldstein, A. Medling, S. Brough, S. M. Sweet, G. Cecil, A. Lopez-Sanchez, K. Glazebrook, Q. Parker, J. T. Allen, M. Goodwin, A. W. Green, I. S. Konstantopoulos, J. S. Lawrence, N. Lorente, M. S. Owers, R. Sharp

Published 2016-10-10Version 1

We study the properties of kinematically disturbed galaxies in the SAMI Galaxy Survey using a quantitative criterion, based on kinemetry (Krajnovic et al.). The approach, similar to the application of kinemetry by Shapiro et al. uses ionised gas kinematics, probed by H{\alpha} emission. By this method 23+/-7% of our 360-galaxy sub-sample of the SAMI Galaxy Survey are kinematically asymmetric. Visual classifications agree with our kinemetric results for 90% of asymmetric and 95% of normal galaxies. We find stellar mass and kinematic asymmetry are inversely correlated and that kinematic asymmetry is both more frequent and stronger in low-mass galaxies. This builds on previous studies that found high fractions of kinematic asymmetry in low mass galaxies using a variety of different methods. Concentration of star forma- tion and kinematic disturbance are found to be correlated, confirming results found in previous work. This effect is stronger for high mass galaxies (log(M*) > 10) and indicates that kinematic disturbance is linked to centrally concentrated star formation. Comparison of the inner (within 0.5Re) and outer H{\alpha} equivalent widths of asymmetric and normal galaxies shows a small but significant increase in inner equivalent width for asymmetric galaxies.