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The LIGO/Virgo Scientific Collaboration (LVC) recently announced thedetection of a compact object binary merger, GW190425, with a total mass of$3.4^{+0.3}_{-0.1}$ M$_{\odot}$, and individual component masses in the rangeof about 1.1 to 2.5 $M_{\odot}$. If the constituent compact objects are neutronstars, then the total mass is five standard deviations higher than the mean of$2.66\pm 0.12$ M$_{\odot}$ for Galactic binary neutron stars (BNSs). LVCsuggests such massive BNS systems are born from a fast-merging channel, andtherefore, their non-detection in the Galaxy to be due to a selection effect.However, we are unable to reconcile the inferred formation efficiency from thereported merger rate, $\mathcal{R}_{\rm GW190425}=460^{+1050}_{-390}$ yr$^{-1}$Gpc$^{-3}$, with predictions from our own study for fast-merging BNS systems.Moreover, the comparable merger rates of GW190425, and GW170817 are possibly intension with our results for two reasons: (i) more massive systems are expectedto have a lower formation rate, and (ii) fast merging channels shouldconstitute $\lesssim 10\%$ of the total BNS systems if case BB unstable masstransfer is permitted to take place as a formation pathway. We argue that toaccount for the high merger rate of GW190425 as a BNS system requires: (i)revisiting our understanding of NS formation in supernova explosions, or (ii):that more massive NSs need to be preferentially born with either very weak orvery high magnetic fields so that they would be undetectable in the radiosurveys. Perhaps massive NSs detected in NS-white dwarf binaries are our cluesto the formation path of GW190425 systems.

Does GW190425 require an alternative formation pathway than a fast-merging channel?