The SAMI Galaxy Survey: Revisiting Galaxy Classification Through High-Order Stellar Kinematics

• Main Authors: van de Sande, Jesse, Bland-Hawthorn, Joss, Fogarty, Lisa M. R., Cortese, Luca, d'Eugenio, Francesco, Croom, Scott M., Scott, Nicholas, Allen, James T., Brough, Sarah, Bryant, Julia J., Cecil, Gerald, Colless, Matthew, Couch, Warrick J., Davies, Roger, Elahi, Pascal J., Foster, Caroline, Goldstein, Greg, Goodwin, Michael, Groves, Brent, Ho, I-Ting, Jeong, Hyunjin, Jones, D. Heath, Konstantopoulos, Iraklis S., Lawrence, Jon S., Leslie, Sarah K., Lopez-Sanchez, Angel R., McDermid, Richard M., McElroy, Rebecca, Medling, Anne M., Oh, Sree, Owers, Matt S., Richards, Samuel N., Schaefer, Adam L., Sharp, Rob, Sweet, Sarah M., Taranu, Dan, Tonini, Chiara, Walcher, C. Jakob, Yi, Sukyoung K.
• Format: Text
• Language: unknown
• Published: arXiv 2016
• Subjects: Astrophysics of Galaxies astro-ph.GA; FOS Physical sciences; sami
• Online Access: https://dx.doi.org/10.48550/arxiv.1611.07039; https://arxiv.org/abs/1611.07039

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 2D integral field data from the SAMI Galaxy Survey. A proxy for the spin parameter ($λ_{R_e}$) and ellipticity ($ε_e$) 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. 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 $λ_{R_e}-ε_e$ 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. 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. : Accepted for Publication in The Astrophysical Journal. 35 pages and 30 figures, abstract abridged for arXiv submission. The key figures of the paper are: 7, 11, 12 , and 14