?Angular momentum evolution for galaxies in a Λ-CDM scenario?

PEDROSA, S.E.; TISSERA, P. B.

Varsovia

Workshop; 1st Roman Juszkiewicz Symposium; 2015

Polish Astronomical Society

Galaxy formation in the current cosmological paradigm is a very complex process where inflows, outflows, interactions and mergers are common events. These processes can redistribute the angular momentum content of baryons. Recent observational results suggest that disc formed conserving angular momentum while elliptical galaxies,albeit losing angular momentum, determine a correlation between the specific angular momentum of the galaxy and the stellar mass. We aim at analysing the specific angular momentum content of the disc and bulge components as a function of virial mass, stellar mass and redshift. We also estimate the size of the simulated galaxies and confront them with observations. We use cosmological hydrodynamical simulations that include an effective, physically-motivated Supernova feedback which is able to regulate the star formation in haloes of different masses. We analysed the morphology and formation history of a sample of galaxies in a cosmological simulation by performing a bulge-disc decomposition of the analysed systems and their progenitors. The angular momentum content of the stellar and gaseous discs, stellar bulges and total baryons are estimated.In agreement with recent observational findings, our simulated galaxies have disc and spheroid components whose specific angular momentum contents determine correlations with the stellar and dark matter masses with the same slope, although the spheroidal components are off-set by a fixed fraction.The total specific angular momentum of galaxies do occupy different positions filling the gap between pure rotational-dominated and dispersion-dominated systems. The scaling relations derived for the simulated galaxies determine a similar relation with the virial radius in agreement with recent observations.