from binary neutron stars would yield a wealth of information about the chirp mass, the orientation, and the localization of the binary but also possibly the mass, spin and radius of the individual stars [@Andersson:2009yt; @Weinstein2012]. In turn, this information could set constraints on the equation of state (EOS) of the matter in their interior. Indeed, a number of recent investigations have revealed that it is possible to set serious constraints on the properties of the neutron-star structure and EOS, either when using the inspiral signal only [@Read2013; @DelPozzo2013], or when exploiting the rich spectral features of the postmerger signal [@Bauswein2011; @Bauswein2012; @Hotokezaka2013c; @Takami2014; @Takami2015].

At the same time, the merger of a binary system containing at least one neutron star represents arguably the most attractive scenario to explain the complex phenomenology associated with short gamma-ray bursts (SGRBs), although many alternatives exist \[see Ref. [@Berger2013b] for a recent review\]. While such a scenario was suggested already 30 years ago [@Eichler89; @Narayan92], numerical simulations (see, [e.g., ]{}Refs. [@Shibata99d; @Baiotti08; @Anderson2007; @Bernuzzi2011; @Paschalidis2014]) and new observations [@Giacomazzo2012b; @Berger2013b] have put this scenario on firmer grounds. In particular, what these simulations have shown is that the merger of a binary system of neutron 