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We perform a Bayesian analysis of the maximum mass $M_{\rm TOV}$ of neutronstars with a quark core, incorporating the observational data from tidaldeformability of the GW170817 binary neutron star merger as detected byLIGO/Virgo and the mass and radius of PSR J0030+0451 as detected by \nicer. Theanalysis is performed under the assumption that the hadron-quark phasetransition is of first order, where the low-density hadronic matter describedin a unified manner by the soft QMF or the stiff DD2 equation of state (EOS)transforms into a high-density phase of quark matter modeled by the generic"Constant-sound-speed" (CSS) parameterization. The mass distribution measuredfor the $2.14 \,{\rm M}_{\odot}$ pulsar, MSP J0740+6620, is used as the lowerlimit on $M_{\rm TOV}$. We find the most probable values of the hybrid starmaximum mass are $M_{\rm TOV}=2.36^{+0.49}_{-0.26}\,{\rm M}_{\odot}$($2.39^{+0.47}_{-0.28}\,{\rm M}_{\odot}$) for QMF (DD2), with an absolute upperbound around $2.85\,{\rm M}_{\odot}$, to the $90\%$ posterior credible level.Such results appear robust with respect to the uncertainties in the hadronicEOS. We also discuss astrophysical implications of this result, especially onthe post-merger product of GW170817, short gamma-ray bursts, and other likelybinary neutron star mergers.

Constraints on the maximum mass of neutron stars with a quark core from GW170817 and NICER PSR J0030+0451 data