Evolution of compact and fossil groups of galaxies from semi-analytical
  models of galaxy formation
  We compare the mean mass assembly histories of compact and fossil galaxy
groups in the Millennium dark matter simulation and an associated semi-analytic
galaxy formation model. Tracing the halo mass of compact groups (CGs) from z=0
to z=1 shows that, on average, 55 per cent of the halo mass in compact groups
is assembled since z~1, compared to 40 per cent of the halo mass in fossil
groups (FGs) in the same time interval, indicating that compared to FGs, CGs
are relatively younger galaxy systems. At z=0, for a given halo mass, fossil
groups tend to have a larger concentration than compact groups. Investigating
the evolution of CG's parameters show that they become more compact with time.
CGs at z=0.5 see their magnitude gaps increase exponentially, but it takes ~10
Gyr for them to reach a magnitude gap of 2 magnitudes. The slow growth of the
magnitude gap leads to only a minority (~41 per cent) of CGs selected at z=0.5
turning into a FG by z=0. Also, while three-quarters of FGs go through a
compact phase, most fail to meet the CG isolation criterion, leaving only ~30
per cent of FGs fully satisfying the CG selection criteria. Therefore, there is
no strong link of CGs turning into FGs or FGs originating from CGs. The
relation between CGs and FGs is thus more complex, and in most cases, FGs and
CGs follow different evolutionary tracks.
