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We investigate the possibility that GW170817 has not been the merger of twoconventional neutron stars (NS) but involved at least one if not two hybridstars with a quark matter core which might even belong to a third family ofcompact stars. To this end, we develop a Bayesian analysis method for selectingthe most probable equation of state (EoS) under a set of constraints fromcompact star physics, which now also include the tidal deformability fromGW170817 and the first result for the mass and radius determination for PSRJ0030+0451 by NICER. We apply this method for the first time to a two-parameterfamily of hybrid EoS based on the DD2 model with nucleonic excluded volume forhadronic matter and the color superconducting generalized nlNJL model for quarkmatter. The model has a variable onset of deconfinement and can mimic theeffects of pasta phases with the possibility of a third family of hybrid starsin the mass-radius ($M-R$) diagram. The main findings of this study are that:1) the presence of multiple configurations for a given mass (twins) correspondsto a set of disconnected lines in the diagram of tidal deformabilities forbinary mergers, so that merger events from the same mass range may result in aprobability landscape with different peak positions; 2) the Bayesian analysiswith the above observational constraints favors an early onset of thedeconfinement transition, at masses of $M_{\rm onset}\le 0.8~M_\odot$ with a$M-R$ relationship that in the range of observed neutron star masses is almostindistinguishable from that of a soft hadronic APR EoS; 3) a few yet fictitiousmeasurements of the NICER experiment with a $1\sigma$ range that is half of thepresent value and different mass and radius would change the posteriorlikelihood so that hybrid EoS with a phase transition onset in the range$M_{\rm onset} = 1.1 - 1.6~M_\odot $ would be favored.

Was GW170817 a canonical neutron star merger? Bayesian analysis with a third family of compact stars