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Gravitational wave signals from compact astrophysical sources such as thoseobserved by LIGO and Virgo require a high-accuracy, theory-based waveform modelfor the analysis of the recorded signal. Current inspiral-merger-ringdownmodels are calibrated only up to moderate mass ratios, thereby limiting theirapplicability to signals from high-mass ratio binary systems. We presentEMRISur1dq1e4, a reduced-order surrogate model for gravitational waveforms of13,500M in duration and including several harmonic modes for non-spinning blackhole binary systems with mass-ratios varying from 3 to 10,000 thus vastlyexpanding the parameter range beyond the current models. This surrogate modelis trained on waveform data generated by point-particle black hole perturbationtheory (ppBHPT) both for large mass-ratio and comparable mass-ratio binaries.We observe that the gravitational waveforms generated through a simpleapplication of ppBHPT to the comparable mass-ratio cases agree remarkably (andsurprisingly) well with those from full numerical relativity after a rescalingof the ppBHPT's total mass parameter. This observation and the EMRISur1dq1e4surrogate model will enable data analysis studies in the high-mass ratioregime, including potential intermediate mass-ratio signals from LIGO/Virgo andextreme-mass ratio events of interest to the future space-based observatoryLISA.

A Surrogate Model for Gravitational Wave Signals from Comparable- to Large- Mass-Ratio Black Hole Binaries