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A class of hybrid compact star equations of state is investigated that joinsby a Maxwell construction a low-density phase of hadronic matter, modeled by arelativistic meanfield approach with excluded nucleon volume, with ahigh-density phase of color superconducting two-flavor quark matter, describedwithin a nonlocal covariant chiral quark model. We find the conditions on thevector meson coupling in the quark model under which a stable branch of hybridcompact stars occurs in the cases with and without diquark condensation. Weshow that these hybrid stars do not form a third family disconnected from thesecond family of ordinary neutron stars unless additional (de)confining effectsare introduced with a density-dependent bag pressure. A suitably chosen densitydependence of the vector meson coupling assures that at the same time the$2~$M$_\odot$ maximum mass constraint is fulfilled on the hybrid star branch. Atwofold interpolation method is realized which implements both, the densitydependence of a confining bag pressure at the onset of the hadron-to-quarkmatter transition as well as the stiffening of quark matter at higher densitiesby a density-dependent vector meson coupling. For three parametrizations ofthis class of hybrid equation of state the properties of corresponding compactstar sequences are presented, including mass twins of neutron and hybrid starsat 2.00, 1.39 and 1.20 $M_\odot$, respectively. The sensitivity of the hybridequation of state and the corresponding compact star sequences to variations ofthe interpolation parameters at the 10% level is investigated and it is foundthat the feature of third family solutions for compact stars is robust againstsuch a variation. This advanced description of hybrid star matter allows tointerpret GW170817 as a merger not only of two neutron stars but also of aneutron star with a hybrid star or of two hybrid stars.

Third family of compact stars within a nonlocal chiral quark model equation of state