Morphology of galaxies with quiescent recent assembly history in a
  Lambda-CDM universe
  The standard disc formation scenario postulates that disc forms as the gas
cools and flows into the centre of the dark matter halo, conserving the
specific angular momentum. Major mergers have been shown to be able to destroy
or highly perturb the disc components. More recently, the alignment of the
material that is accreted to form the galaxy has been pointed out as a key
ingredient to determine galaxy morphology. However, in a hierarchical scenario
galaxy formation is a complex process that combines these processes and others
in a non-linear way so that the origin of galaxy morphology remains to be fully
understood. We aim at exploring the differences in the formation histories of
galaxies with a variety of morphology, but quite recent merger histories, to
identify which mechanisms are playing a major role. We analyse when minor
mergers can be considered relevant to determine galaxy morphology. We also
study the specific angular momentum content of the disc and central spheroidal
components separately. We used cosmological hydrodynamical simulations that
include an effective, physically motivated supernova feedback that is able to
regulate the star formation in haloes of different masses. We analysed the
morphology and formation history of a sample of 15 galaxies of a cosmological
simulation. We performed a spheroid-disc decomposition of the selected galaxies
and their progenitor systems. The angular momentum orientation of the merging
systems as well as their relative masses were estimated to analyse the role
played by orientation and by minor mergers in the determination of the
morphology. We found the discs to be formed by conserving the specific angular
momentum in accordance with the classical disc formation model. The specific
angular momentum of the stellar central spheroid correlates with the dark
matter halo angular momentum and determines a power law. Abridged
