Field spheroid-dominated galaxies in a {\Lambda}-CDM Universe
  Understanding the formation and evolution of early-type, spheroid-dominated
galaxies is an open question within the context of the hierarchical clustering
scenario, particularly, in low-density environments. Our goal is to study the
main structural, dynamical, and stellar population properties and assembly
histories of field spheroid-dominated galaxies formed in a LCDM scenario to
assess to what extend they are consistent with observations. We selected
spheroid-dominated systems from a LCDM simulation that includes star formation,
chemical evolution and Supernova feedback. A sample of 18 field systems with
Mstar <= 6x10^10 Msun that are dominated by the spheroid component. For this
sample we estimate the fundamental relations of ellipticals and then compared
with current observations. The simulated spheroid galaxies have sizes in good
agreement with observations. The bulges follow a Sersic law with Sersic indexes
that correlate with the bulge-to-total mass ratios. The structural-dynamical
properties of the simulated galaxies are consistent with observed
Faber-Jackson, Fundamental Plane, and Tully-Fisher relations. However, the
simulated galaxies are bluer and with higher star formation rates than observed
isolated early-type galaxies. The archaeological mass growth histories show a
slightly delayed formation and more prominent inside-out growth mode than
observational inferences based on the fossil record method. The main structural
and dynamical properties of the simulated spheroid-dominated galaxies are
consistent with observations. This is remarkable since none of them has been
tuned to be reproduced. However, the simulated galaxies are blue and
star-forming, and with later stellar mass growth histories as compared to
observational inferences. This is mainly due to the persistence of extended
discs in the simulations. Abridged
