The velocity field in MOND cosmology
  The recently developed code for N-body/hydrodynamics simulations in Modified
Newtonian Dynamics (MOND), known as RAyMOND, is used to investigate the
consequences of MOND on structure formation in a cosmological context, with a
particular focus on the velocity field. This preliminary study investigates the
results obtained with the two formulations of MOND implemented in RAyMOND, as
well as considering the effects of changing the choice of MOND interpolation
function, and the cosmological evolution of the MOND acceleration scale. The
simulations are contrived such that structure forms in a background cosmology
that is similar to $\Lambda$CDM, but with a significantly lower matter content.
Given this, and the fact that a fully consistent MOND cosmology is still
lacking, we compare our results with a standard $\Lambda$CDM simulation, rather
than observations. As well as demonstrating the effectiveness of using RAyMOND
for cosmological simulations, it is shown that a significant enhancement of the
velocity field is likely an unavoidable consequence of the gravitational
modification implemented in MOND, and may represent a clear observational
signature of such a modification. It is further suggested that such a signal
may be clearest in intermediate density regions such as cluster outskirts and
filaments.
