  The equation of state (EOS) of dense matter is an essential ingredient for
numerical simulations of core-collapse supernovae and neutron star mergers. The
properties of matter near and above nuclear saturation density are uncertain,
which translates into uncertainties in astrophysical simulations and their
multi-messenger signatures. Therefore, a wide range of EOSs spanning the
allowed range of nuclear interactions are necessary for determining the
sensitivity of these astrophysical phenomena and their signatures to variations
in input microphysics. We present a new set of finite temperature EOSs based on
experimentally allowed Skyrme forces. We employ a liquid drop model of nuclei
to capture the non-uniform phase of nuclear matter at sub-saturation density,
which is blended into a nuclear statistical equilibrium EOS at lower densities.
We also provide a new, open-source code for calculating EOSs for arbitrary
Skyrme parametrizations. We then study the effects of different Skyrme
parametrizations on thermodynamical properties of dense astrophysical matter,
the neutron star mass-radius relationship, and the core collapse of 15 and 40
solar mass stars.
