The Tully-Fisher Relation and the dynamical evolution of galaxies

M. E. DE ROSSI; P. B. TISSERA; S. E. PEDROSA

San Juán

Congreso; Primera Reunión Anual Binacional entre la Asociación Argentina de Astronomía y la Sociedad Chilena de Astronomía; 2011

Asociación Argentina de Astronomía

We studied the dynamical and kinematical properties of galaxies since z ∼ 3 by performing numerical simulations in a ΛCDM universe. Our results suggest that the maximum gas-phase rotation velocity of the disc com- ponent is a good proxy for the circular velocity at that radius regardless of the galaxy morphology. We also found that velocity scales which combine dis- persion and rotation velocity in their definition lead to a tighter Tully-Fisher Relation. In particular, the lowest scatter in the correlation between mass and velocity is obtained if the kinematical indicator is evaluated at the radius cor- responding to the maximum of the rotation curve. In these simulations, the evolution of the scatter of the Tully-Fisher Relation seems to be strongly mod- ulating by galaxy interactions and mergers which can drive gas inflows and outflows regulating the star formation process and feedback mechanisms inside these systems.