Fig. 7.
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Probability that a BNS would satisfy our jet-launching conditions (Eq. (15)) as a function of the component masses M1 and M2, given our present knowledge of the EoS (encoded in the priors defined in Sect. 3.4). The masses of Galactic BNS systems that merge within a Hubble time and the two GW-detected BNS are shown for comparison, in the same way as in Fig. 5.
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