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The gravitational wave data of GW170817 favor the equation of state (EoS)models that predict compact neutron stars (NSs), consistent with the radiusconstraints from X-ray observations. Motivated by such a remarkable progress,we examine the fate of the remnants formed in NS mergers and focus on the rolesof the angular momentum and the mass distribution of the binary NSs. In themass shedding limit (for which the dimensionless angular momentum equals to theKeplerian value, i.e., $j=j_{\rm Kep}$), the adopted { seven EoS models, exceptH4 and ALF2,} yield supramassive NSs in more than half of the mergers. However,for $j\lesssim 0.7j_{\rm Kep}$, the presence or absence of a non-negligiblefraction of supramassive NSs formed in the mergers depends sensitively on boththe EoS and the mass distribution of the binary systems. The NS mergers with atotal gravitational mass $\leq 2.6M_\odot$ are found to be able to shedvaluable light on both the EoS model and the angular momentum of the remnantsif supramassive NSs are still absent. We have also discussed the uncertainty onestimating the maximum gravitational mass of non-rotating NSs ($M_{\rm max}$)due to the unknown $j$ of the pre-collapse remnants. With the data of GW170817and the assumption of the mass loss of $0.03M_\odot$, we have $M_{\rmmax}<(2.19,~2.32)M_\odot$ (90\% confidence level) for $j=(1.0,~0.8)j_{\rmKep}$, respectively.

GW170817 and the prospect of forming supramassive remnants in neutron star mergers