  In this work we present a newly constructed equation of state (EoS)
--applicable to stellar core collapse and neutron star mergers--, including the
entire baryon octet. Our EoS is compatible with the main constraints from
nuclear physics and, in particular, with a maximum mass for cold
beta-equilibrated neutron stars of 2 solar masses in agreement with recent
observations. As an application of our new EoS, we compute numerical stationary
models for rapidly (rigidly) rotating hot neutron stars. We consider maximum
masses of hot stars, such as proto-neutron stars or hypermassive neutron stars
in the post-merger phase of binary neutron star coalescence. The universality
of I-Q-relations at nonzero temperature for fast rotating models, comparing a
purely nuclear EoS with its counterparts containing Lambda-hyperons or the
entire baryon octet, respectively, is discussed, too. We find that the I-Q
universality is broken when thermal effects become important, whatever the
value of entropy gradients in our models. Thus, the use of I-Q relations for
the analysis of proto-neutron stars or merger remnant data, including
gravitational wave signals from the last stages of binary neutron star mergers,
should be regarded with care.
