Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 492, Issue 4, Pages 4945-4951Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa181
Keywords
gravitational waves; methods: statistical; stars: neutron
Categories
Funding
- Hoff Lu Fellowship at the University of Minnesota
- NSF [PHY-1806630]
- David and Ellen Lee Postdoctoral Fellowship at the California Institute of Technology
- ARC [DP180103155, FT160100112]
- National Science Foundation [PHY-0757058]
- [CE170100004]
- [FT150100281]
- Australian Research Council [FT150100281] Funding Source: Australian Research Council
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Binary neutron star mergers arc rich laboratories for physics, accessible with ground-based interferometric gravitational-wave detectors such as the Advanced LIGO and Advanced Virgo. If a neutron star remnant survives the merger, it can emit gravitational waves that might be detectable with the current or next generation detectors. The physics of the long-lived post-merger phase is not well understood and makes modelling difficult. In particular the phase of the gravitational-wave signal is not well modelled. In this paper, we explore methods for using long duration post-merger gravitational-wave signals to constrain the parameters and the properties of the remnant. We develop a phase-agnostic likelihood model that uses only the spectral content for parameter estimation and demonstrate the calculation of a Bayesian upper limit in the absence of a signal. With the millisecond magnetar model, we show that for an event like GW170817, the ellipticity of a long-lived remnant can be constrained to less than about 0.5 in the parameter space used.
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