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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
Monthly notices of the Royal Astronomical Society, 11/2016, Volume: 463, Issue: 1Journal Article
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 Sydney-AAO Multi-object Integral field Galaxy Survey. We find that j, measured within one effective radius, monotonically increases with M * and that, for M * > 109.5 M⊙, 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 3. Indeed, the stellar spin parameter (quantified via λ 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.
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