  We perform cooling simulations for isolated neutron stars using recently
developed equations of state for their core. The equations of state are
obtained from new parametrizations of the FSU2 relativistic mean-field
functional that reproduce the properties of nuclear matter and finite nuclei,
while fulfilling the restrictions on high-density matter deduced from heavy-ion
collisions, measurements of massive 2$M_{\odot}$ neutron stars, and neutron
star radii below 13 km. We find that two of the models studied, FSU2R (with
nucleons) and in particular FSU2H (with nucleons and hyperons), show very good
agreement with cooling observations, even without including extensive nucleon
pairing. This suggests that the cooling observations are more compatible with
an equation of state that produces a soft nuclear symmetry energy and, hence,
generates small neutron star radii. However, both models favor large stellar
masses, above $1.8 M_{\odot}$, to explain the colder isolated neutron stars
that have been observed, even if nucleon pairing is present.
