We release neutron star merger waveforms computed using fully general relativistic simulations of equal and unequal-mass binaries drawn from the galactic population. The simulations employ finite-temperature microphysical equations of state (LS220, DD2, and SFHo) and neutrino cooling. Please, see http://arxiv.org/abs/1512.06397 for details. Each tarball refers to a simulation and contains Curvature multipolar waveform \(\psi^{(4)}_{\ell m}\) Metric multipolar waveform \(h_{\ell m}\) Radiated energy and angular momentum Files: waveforms/Psi4_l?_m?_r200.txt Columns: \(t,\ \Re{(\psi^{(4)}_{\ell m})},\ \Im{(\psi^{(4)}_{\ell m})} \) waveforms/Rh_l?_m?_r200.txt Columns: \(u/M,\ \Re{(h_{\ell m})}/M,\ \Im{(h_{\ell m})}/M,\ \Re{(\dot{h}_{\ell m})},\ \Im{(\dot{h}_{\ell m}}),\ M\omega_{\ell m},\ A_{\ell m}/M,\ \phi_{\ell m},\ t \) waveforms/Ej_r200.txt Columns: \(E_b,\ j,\ E_\text{rad},\ J_\text{rad},\ t \) where \(t\) simulation time \(u\) retarded time \(M\) binary mass \(\omega_{\ell m}\) wave frequency \(A_{\ell m}\) wave amplitude \(\phi_{\ell m}\) wave phase \(E_\text{GW}\) radiated energy \(J_\text{GW}\) radiated angular momentum \(E_b\) binary energy \(j\) binary specific angular momentum Please refer to the paper and references therein for the definition of the different quantities. Units \(c=G=M_\text{Sun}=1\)

{"references": ["How loud are neutron star mergers? Sebastiano Bernuzzi, David Radice, Christian D. Ott, Luke F. Roberts, Philipp M\u00f6sta, and Filippo Galeazzi, Phys. Rev. D 94, 024023, 2016. http://arxiv.org/abs/1512.06397"]}