A new preprint on arXiv (2606.02593) maps hybrid equations of state with first-order deconfinement transitions onto a Seidov diagram and shows that any hybrid star sitting inside the 2.5–5 solar-mass gap demands an unrealistically early onset of quark matter plus extremely stiff quark-matter cores. Bayesian inference, however, prefers models in which the transition occurs near 1.4 solar masses, producing mass-twin pairs that are already marginally consistent with NICER radius data. The study therefore concludes that confirmed twins at canonical mass would exclude hybrids as mass-gap candidates. This result directly challenges earlier interpretations of GW190814, whose 2.6-solar-mass secondary was sometimes modeled as a hybrid star; the twin-star constraint implies that object was instead a low-mass black hole. The analysis rests on a generic parameterization rather than full QCD lattice input, and the sample of radius measurements remains modest (NICER PSR J0030+0451 and J0740+6620). No peer-reviewed follow-up yet exists. Related work in Phys. Rev. D 103, 023008 (2021) on GW170817 tidal deformability and the 2023 ApJ study of the Galactic neutron-star mass distribution both reinforce the same Bayesian preference for an early transition. If future NICER or SKA observations lock in a 1.4-solar-mass twin pair, gravitational-wave catalogs will require wholesale reclassification of the lower mass gap, shrinking the allowed parameter space for exotic compact-object formation channels.