  Differences in the equation of state (EOS) of dense matter translate into
differences in astrophysical simulations and their multi-messenger signatures.
Thus, extending the number of EOSs for astrophysical simulations allows us to
probe the effect of different aspects of the EOS in astrophysical phenomena. In
this work, we construct the EOS of hot and dense matter based on the Akmal,
Pandharipande, and Ravenhall (APR) model and thereby extend the open-source
SROEOS code which computes EOSs of hot dense matter for Skyrme-type
parametrizations of the nuclear forces. Unlike Skrme-type models, in which
parameters of the interaction are fit to reproduce the energy density of
nuclear matter and/or properties of heavy nuclei, the EOS of APR is obtained
from potentials resulting from fits to nucleon-nucleon scattering and
properties of light nuclei. In addition, this EOS features a phase transition
to a neutral pion condensate at supra-nuclear densities. We show that
differences in the effective masses between EOSs have consequences for the
properties of nuclei in the sub-nuclear inhomogeneous phase of matter. We also
test the new EOS of APR in spherically symmetric core-collapse of massive stars
with $15M_\odot$ and $40M_\odot$, respectively. We find that the phase
transition in the EOS of APR speeds up the collapse of the star. However, this
phase transition does not generate a second shock wave or another neutrino
burst as reported for the hadron-to-quark phase transition. The reason for this
difference is that the onset of the phase transition in the EOS of APR occurs
at larger densities than for the quark-to-hadron transition employed earlier
which results in a significantly smaller softening of the high density EOS.
