Hybrid stars among mass gap objects are excluded by twin stars at $1.4M_{\odot }$

We investigate the question whether compact objects in the so called mass gap ($2.5<M\mathrm{/}{M}_{\odot }<5.0$) can be neutron stars or hybrid stars. Using a generic hybrid star equation of state with a first-order deconfinement transition, we map the allowed parameter space in a Seidov-type diagram and confront it with modern mass–radius constraints. We find that mass-gap hybrid stars require an extremely early onset of deconfinement and very stiff quark matter. The Bayesian analysis, however, favors equations of state with deconfinement at typical neutron-star masses around $1.4M_{\odot }$ with mass-twin stars that, if confirmed, would rule out hybrid stars as candidates for observed mass-gap compact objects.