Effective-one-body waveforms for binary neutron stars using surrogate models

Understand

Gravitational-wave observations of binary neutron star systems can provide information about the masses, spins, and structure of neutron stars.

• However, this requires accurate and computationally efficient waveform models that take <1s to evaluate for use in Bayesian parameter estimation codes that perform 10^7 - 10^8 waveform evaluations.
• We present a surrogate model of a nonspinning effective-one-body waveform model with l = 2, 3, and 4 tidal multipole moments that reproduces waveforms of binary neutron star numerical simulations up to merger.
• The surrogate is built from compact sets of effective-one-body waveform amplitude and phase data that each form a reduced basis.