The link between angular momentum and optical morphology


Cortese, L.; Fogarty, L. M. R.; Bekki, K.; van de Sande, J.; Couch, W.; Catinella, B.; Colless, M.; Obreschkow, D.; Taranu, D.; Tescari, E.; Barat, D.; Bland-Hawthorn, J.; Bloom, J.; Bryant, J. J.; Cluver, M.; Croom, S. M.; Drinkwater, M. J.; d'Eugenio, F.; Konstantopoulos, I. S.; Lopez-Sanchez, A.; Mahajan, S.; Scott, N.; Tonini, C.; Wong, O. I.; Allen, J. T.; Brough, S.; Goodwin, M.; Green, A. W.; Ho, I.-T.; Kelvin, L. S.; Lawrence, J. S.; Lorente, N. P. F.; Medling, A. M.; Owers, M. S.; Richards, S.; Sharp, R.; Sweet, S. M.


We investigate the relationship between stellar and gas specific angular momentum j, stellar mass $M_*$ and optical morphology for a sample of 488 galaxies extracted from the SAMI Galaxy Survey. We find that j, measured within one effective radius, monotonically increases with $M_*$ and that, for $M_*>10^{9.5} M_{\odot}$, the scatter in this relation strongly correlates with optical morphology (i.e., visual classification and Sérsic index). These findings confirm that massive galaxies of all types lie on a plane relating mass, angular momentum and stellar light distribution, and suggest that the large-scale morphology of a galaxy is regulated by its mass and dynamical state. We show that the significant scatter in the $M_*-j$ relation is accounted for by the fact that, at fixed stellar mass, the contribution of ordered motions to the dynamical support of galaxies varies by at least a factor of three. Indeed, the stellar spin parameter (quantified via $\lambda_R$) correlates strongly with Sérsic and concentration indices. This correlation is particularly strong once slow-rotators are removed from the sample, showing that late-type galaxies and early-type fast rotators form a continuous class of objects in terms of their kinematic properties.

Publication Date: 
July 2016
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