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tokens: be given elsewhere (D. Radice et al. 2017, in preparation). A summary of the simulations is given in Table 1 . Table 1 Gravitational and Baryonic Masses, Compactnesses, Tidal Deformability Parameters, BH Formation Time, and Disk and Ejecta Masses Notes. Disk and ejecta masses are given at the final simulation time. a NS gravitational mass. b NS baryonic mass. c NS compactness, . d Dimensionless quadrupolar tidal parameters, Equation ( 2 ). e Dimensionless tidal parameter, Equation ( 1 ). f Gravitationally bound material with outside of the apparent horizon. g Dynamic ejecta mass, computed as from the flux of unbound matter through the coordinate-sphere . h BH formation time, in milliseconds after merger. i Final simulation time, in milliseconds after merger. We compute the mass of the dynamic ejecta and of the remnant accretion disk for each model. Our results are shown in Table 1 and Figure 1 . The typical dynamic ejecta masses in our simulations are of the order of , in good qualitative agreement with previous numerical-relativity results. We do not find any clear indication of a trend in the dynamic ejecta masses as a function of the binary parameters or EOS. However, we find a clear correlation between the disk masses and the tidal parameter . According to our simulations, binaries with inevitably produce BHs with small accretion disks. These cases are incompatible with the infrared data for AT2017gfo, even under the assumption that all of the matter left outside of the event horizon will be ejected. Figure 1. Remnant disk plus dynamic ejecta masses (upper panel) and BH formation time (lower panel) plotted against the tidal parameter (Equation ( 1 )). For models that do not collapse during our simulation time, we give a lower limit. The horizontal dashed line shows a conservative lower limit for AT2017gfo, , obtained assuming that the entire disk is unbound. The vertical dotted line is . Errors on and are estimated following Equation ( 3 ) and are added in quadrature. The reason for this trend is easily understood from the lower panel of Figure 1 . The NS dimensionless quadrupolar tidal parameters depend on the negative-fifth power of the NS compactness ( Equation ( 2 )). Consequently, small values of are associated with binary systems having compact NSs that result in rapid or prompt BH formation. In these cases, the collapse happens on a shorter timescale than the hydrodynamic processes responsible for the formation of the disk. Consequently, only a small amount of mass is left outside of the event horizon at the end of the simulations. Binaries with larger values of produce more massive disks, up to , and longer lived remnants. In these cases, neutrino driven winds and viscous and magnetic processes in the disk are expected to unbind sufficient material to explain the optical and infrared observations for AT2017gfo (Perego et al. 2014 ; Wu et al. 2016 ; Siegel Metzger 2017 ). 4. Discussion On the basis of our simulations and the