The mass probability distribution of merger remnants (left panel) and the range of M_crit as a function of the adopted value for the ejecta mass, M_ej (right panel). The mass distribution of merger remnants is obtained by assuming (i) a double-peaked Gaussian mass distribution for binary NS components, with one peak at μ₁ = 1.34 M_⊙ (σ₁ = 0.07 M_⊙) and one at μ₂ = 1.8 M_⊙ (σ₂ = 0.21 M_⊙), (ii) a quasi-EOS-independent relation between gravitational and baryonic mass (Eq. (5)), and (iii) a fiducial ejecta mass of ∼0.05 M_⊙. The yellow-shaded area indicates the M_rem range for which the cumulative distribution function yields a probability of ∼0.15–0.26 (i.e. our f_mag range). It defines our estimated range for M_crit, that is the maximum mass of NS remnants that remain stable or do not collapse into a BH for at least a time long enough to power plateaus lasting > 200 s, such as those found in our sample.