  We present three-dimensional simulations of the dynamics of binary neutron
star (BNS) mergers from the late stage of the inspiral process up to $\sim 20$
ms after the system has merged, either to form a hyper-massive neutron star
(NS) or a rotating black hole (BH). We investigate five equal-mass models of
total gravitational mass $2.207$, $2.373$, $2.537$, $2.697$ and $2.854
M_\odot$, respectively, and four unequal mass models with
$M_{\mathrm{ADM}}\simeq 2.53\ M_\odot$ and $q\simeq 0.94$, $0.88$, $0.82$, and
$0.77$ (where $q = M^{(1)}/M^{(2)}$ is the mass ratio). We use a semi-realistic
equation of state (EOS) namely, the seven-segment piece-wise polytropic SLyPP
with a thermal component given by $\Gamma_{th} = 1.8$. We have also compared
the resulting dynamics (for one model) using both, the BSSN-NOK and CCZ4
methods for the evolution of the gravitational sector, and also different
reconstruction methods for the matter sector, namely PPM, WENO and MP5. Our
results show agreement and high resolution, but superiority of BSSN-NOK
supplemented by WENO reconstruction at lower resolutions.
  One of the important characteristics of the present investigation is that,
for the first time, this has been done using only publicly available open
source software, in particular, the Einstein Toolkit code deployed for the
dynamical evolution and the LORENE code for the generation of the initial
models. All of the source code and parameters used for the simulations have
been made publicly available. This not only makes it possible to re-run and
re-analyze our data; it also enables others to directly build upon this work
for future research.
