Angular momentum evolution for galaxies in a Λ-CDM scenario

PEDROSA, SUSANA; PATRICIA B. TISSERA

ASTRONOMY & ASTROPHYSICS. SUPPLEMENT SERIES (PRINT)

EDP sciencies

Lugar: Paris; Año: 2015 vol. 584

0365-0138

Context. Galaxy formation in the current cosmological paradigm is a verycomplex process in which inflows, outflows, interactions, and mergersare common events. These processes can redistribute the angular momentumcontent of baryons. Recent observational results suggest that discformed conserving angular momentum while elliptical galaxies, althoughthey lose angular momentum, determine a correlation between the specificangular momentum of the galaxy and the stellar mass. These observationsprovide stringent constraints for galaxy formation models in ahierarchical clustering scenario. Aims: We aim to analyse thespecific angular momentum content of the disc and bulge components as afunction of virial mass, stellar mass, and redshift. We also estimatethe size of the simulated galaxies and compare them with observations. Methods: We use cosmological hydrodynamical simulations thatinclude an effective, physically motivated supernova feedback which isable to regulate the star formation in haloes of different masses. Weanalyse the morphology and formation history of a sample of galaxies ina cosmological simulation by performing a bulge-disc decomposition ofthe analysed systems and their progenitors. We estimate the angularmomentum content of the stellar and gaseous discs, stellar bulges, andtotal baryons. Results: In agreement with recent observationalfindings, our simulated galaxies have disc and spheroid components whosespecific angular momentum content determine correlations with thestellar and dark matter masses with the same slope, although thespheroidal components are offset by a fixed fraction. The averageangular momentum efficiency for the simulated discs is η ~ 1, whilefor bulges it is η ~ 0.10-0.20. For the simulated sample, thecorrelations found for the specific angular momentum content as afunction of virial mass or stellar mass are found not to evolvesignificantly with redshift (up to z ~ 2). Both dynamical componentsseem to move along the correlations as they evolve. The total specificangular momentum of galaxies occupy different positions filling the gapbetween pure rotational-dominated and dispersion-dominated systems. Thescaling relations derived from the simulated galaxies determine asimilar relation with the virial radius, which is in agreement withrecent observations.