Assembly Bias of Dwarf-sized Dark Matter Haloes
  Previous studies indicate that assembly bias effects are stronger for lower
mass dark matter haloes. Here we make use of high resolution re-simulations of
rich clusters and their surroundings from the Phoenix Project and a large
volume cosmological simulation, the Millennium-II run, to quantify assembly
bias effects on dwarf-sized dark matter haloes. We find that, in the regions
around massive clusters, dwarf-sized haloes ($[10^9,10^{11}]\ms$) form earlier
($\Delta z \sim 2$ in redshift) and possess larger $V_{\rm max}$ ($\sim20%$)
than the field galaxies. We find that this environmental dependence is largely
caused by tidal interactions between the ejected haloes and their former hosts,
while other large scale effects are less important. Finally we assess the
effects of assembly bias on dwarf galaxy formation with a sophisticated
semi-analytical galaxy formation model. We find that the dwarf galaxies near
massive clusters tend to be redder ($\Delta(u-r) = 0.5$) and have three times
as much stellar mass compared to the field galaxies with the same halo mass.
These features should be seen with observational data.
