  We present, for the first time, recoil velocity estimates for binary neutron
star mergers using data from numerical relativity simulations. We find that
binary neutron star merger remnants can have recoil velocity of the order of a
few tens of km/s and as high as $150$ km/s in our dataset. These recoils are
attained due to equivalent contributions from the anisotropic gravitational
wave emission as well as the asymmetric ejection of dynamical matter during the
merger. We provide fits for net recoil velocity as well as its ejecta component
as a function of the amount of ejected matter, which may be useful when
constraints on the ejected matter are obtained through electromagnetic
observations. We also estimate the mass and spin of the remnants and find them
to be in the range $[2.34, 3.38] M_{\odot}$ and $[0.63, 0.82]$ respectively,
for our dataset.
