The Sami Galaxy Survey: revisiting galaxy classification through high-order stellar kinematics

• Main Authors: van De Sande, Jesse, Bland-Hawthorn, Joss, Cecil, Gerard, Colless, Matthew, Couch, Warrick J., Davies, Roger, Elahi, Pascal J., Foster, Caroline, Goldstein, Gregory, Goodwin, Michael, Groves, Brent, Ho, I.-Ting, Fogarty, Lisa M. R., Jeong, Hunjin, Jones, D. Heath, Cortese, Luca, D'Eugenio, Francesco, Croom, Scott M., Scott, Nicholas, Allen, James T., Brough, Sarah, Bryant, Julia J.
• Other Authors: The University of Newcastle. Academic Division, Centre for English Language and Foundation Studies
• Format: Article in Journal/Newspaper
• Language: English
• Published: Institute of Physics Publishing 2017
• Subjects: cosmology; galaxies; galaxy evolution; galaxy formation; kinematics; stellar content; galaxy structure; sami
• Online Access: http://hdl.handle.net/1959.13/1399011

Recent cosmological hydrodynamical simulations suggest that integral field spectroscopy can connect the high-order stellar kinematic moments h₃ (~skewness) and h₄ (~kurtosis) in galaxies to their cosmological assembly history. Here, we assess these results by measuring the stellar kinematics on a sample of 315 galaxies, without a morphological selection, using two-dimensional integral field data from the SAMI Galaxy Survey. Proxies for the spin parameter (λ Rₑ ) and ellipticity (ϵₑ) are used to separate fast and slow rotators; there exists a good correspondence to regular and non-regular rotators, respectively, as also seen in earlier studies. We confirm that regular rotators show a strong h₃ versus V/σ anti-correlation, whereas quasi-regular and non-regular rotators show a more vertical relation in h₃ and V/σ. Motivated by recent cosmological simulations, we develop an alternative approach to kinematically classify galaxies from their individual h₃ versus V/σ signatures. Within the SAMI Galaxy Survey, we identify five classes of high-order stellar kinematic signatures using Gaussian mixture models. Class 1 corresponds to slow rotators, whereas Classes 2-5 correspond to fast rotators. We find that galaxies with similar λ Rₑ - ϵₑ values can show distinctly different h₃ - V/σ signatures. Class 5 objects are previously unidentified fast rotators that show a weak h₃ versus V/σ anti-correlation. From simulations, these objects are predicted to be disk-less galaxies formed by gas-poor mergers. From morphological examination, however, there is evidence for large stellar disks. Instead, Class 5 objects are more likely disturbed galaxies, have counter-rotating bulges, or bars in edge-on galaxies. Finally, we interpret the strong anti-correlation in h₃ versus V/σ as evidence for disks in most fast rotators, suggesting a dearth of gas-poor mergers among fast rotators.