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

A new temperature dependent hyperonic equation of state: application to rotating neutron star models and I-Q-relations