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<jats:title>Abstract</jats:title> <jats:p>Using four different suites of cosmological simulations, we generate synthetic spectra for galaxies with different Lyman-continuum escape fractions (<jats:italic>f</jats:italic> <jats:sub>esc</jats:sub>) at redshifts <jats:inline-formula> <jats:tex-math> <?CDATA $z\approx 7$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa58e3ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>–9, in the rest-frame wavelength range relevant for the <jats:italic>James Webb Space Telescope</jats:italic> (<jats:italic>JWST</jats:italic>) NIRSpec instrument. By investigating the effects of realistic star formation histories and metallicity distributions on the EW(H<jats:italic>β</jats:italic>)–<jats:italic>β</jats:italic> diagram (previously proposed as a tool for identifying galaxies with very high <jats:italic>f</jats:italic> <jats:sub>esc</jats:sub>), we find that neither of these effects are likely to jeopardize the identification of galaxies with extreme Lyman-continuum leakage. Based on our models, we expect that essentially all <jats:inline-formula> <jats:tex-math> <?CDATA $z\approx 7\mbox{--}9$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa58e3ieqn2.gif" xlink:type="simple" /> </jats:inline-formula> galaxies that exhibit rest-frame <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{EW}({\rm{H}}\beta )\lesssim 30$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa58e3ieqn3.gif" xlink:type="simple" /> </jats:inline-formula> Å to have <jats:inline-formula> <jats:tex-math> <?CDATA ${f}_{\mathrm{esc}}\gt 0.5$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa58e3ieqn4.gif" xlink:type="simple" /> </jats:inline-formula>. Incorrect assumptions concerning the ionizing fluxes of stellar populations or the dust properties of <jats:inline-formula> <jats:tex-math> <?CDATA $z\gt 6$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa58e3ieqn5.gif" xlink:type="simple" /> </jats:inline-formula> galaxies can in principle bias the selection, but substantial model deficiencies of this type should at the same time be evident from offsets in the observed distribution of <jats:inline-formula> <jats:tex-math> <?CDATA $z\gt 6$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa58e3ieqn6.gif" xlink:type="simple" /> </jats:inline-formula> galaxies in the EW(H<jats:italic>β</jats:italic>)–<jats:italic>β</jats:italic> diagram compared to the simulated distribution. Such offsets would thereby allow <jats:italic>JWST</jats:italic>/NIRSpec measurements of these observables to serve as input for further model refinement.</jats:p>