Final NS mass for various EoS as a function of baryonic mass loss in a DNS merger event for a system similar to PSR J1411+2551. Only the AP3, MPA1, and PAL1 EoS models are able to leave behind a stable (slowly rotating) NS if the baryonic mass loss is less than about 0.05 M⊙. For the different EoSs, see Lattimer & Prakash (2001). Note, the EoS models H4 and PAL1 correspond to rather large neutron stars (typical radii ∼14 km) and are therefore disfavored by the GW170817 merger event (Abbott et al. 2017).