Are hierarchically formed embedded star clusters surviving gas expulsion
  depending on their initial conditions?
  We investigate the dissolution process of young embedded star clusters with
different primordial mass segregation levels using fractal distributions by
means of N-body simulations. We combine several star clusters in virial and
subvirial global states with Plummer and uniform density profiles to mimic the
gas. The star clusters have masses of Mstars = 500 Mo which follow an initial
mass function where the stars have maximum distances from the centre of r = 1.5
pc. The clusters are placed in clouds which at the same radius have masses of
Mcloud = 2000 Mo, resulting in star formation efficiency of 0.2. We remove the
background potential instantaneously at a very early phase, mimicking the most
destructive scenario of gas expulsion. The evolution of the fraction of bound
stellar mass is followed for a total of 16 Myr for simulations with stellar
evolution and without. We compare our results with previous works using
equal-mass particles where an analytical physical model was used to estimate
the bound mass fraction after gas expulsion. We find that independent of the
initial condition, the fraction of bound stellar mass can be well predicted
just right after the gas expulsion, but tends to be lower at later stages, as
these systems evolve due to the stronger two-body interactions resulting from
the inclusion of a realistic initial mass function. This discrepancy is
independent of the primordial mass segregation level.
