  We present fully general relativistic simulations of binary neutron star
mergers, employing a new zero- temperature chiral effective field theory
equation of state, the BL EOS. We offer a comparison with respect to the older
GM3 EOS, which is based on standard relativistic mean field theory, and
separately determine the impact of the mass. We provide a detailed analysis of
the dynamics, with focus on the post-merger phase. For all models, we extract
the gravitational wave strain and the post-merger frequency spectrum. Further,
we determine the amount, velocity, and polar distribution of ejected matter,
and provide estimates for the resulting kilonova signals. We also study the
evolution of the disk while it is interacting with the hypermassive remnant,
and dis- cuss the merits of different disk mass definitions applicable before
collapse, with regard to the mass remaining after BH formation. Finally, we
investigate the radial mass distribution and rotation profile of the remnants,
which validate previous results and also corroborate a recently proposed
stability criterion.
