Detection and characterization of eccentric compact binary coalescence at the interface of numerical relativity, analytical relativity and machine learning
Abstract
We present ENIGMA, a time domain, inspiral-merger-ringdown waveform model that describes non-spinning binary black holes systems that evolve on moderately eccentric orbits (https://arxiv.org/abs/1711.06276). The inspiral evolution is described using a consistent combination of post-Newtonian theory, self-force and black hole perturbation theory. Assuming moderately eccentric binaries that circularize prior to coalescence, we smoothly match the eccentric inspiral with a stand-alone, quasi-circular merger, which is constructed using machine learning algorithms that are trained with quasi-circular numerical relativity waveforms. We show that ENIGMA reproduces with excellent accuracy the dynamics of quasi-circular compact binaries, and numerical relativity waveforms that describe eccentric binary black hole mergers with mass-ratios 1 < q < 5 . 5 , and eccentricities e < 0 . 2 ten orbits before merger. We use ENIGMA to show that if the gravitational wave events GW150914, GW151226, GW170104 and GW170814 have eccentricities e 0 . 1 at 10 Hz, they can be misclassified as quasi-circular binaries due to parameter space degeneracies between eccentricity and spin corrections.
This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the State of Illinois.- Publication:
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APS April Meeting Abstracts
- Pub Date:
- 2018
- Bibcode:
- 2018APS..APRS13006H