Second release of the CoRe database of binary neutron star merger waveforms

González, Alejandra; Zappa, Francesco; Breschi, M.; Bernuzzi, Sebastiano; Radice, David; Adhikari, Ananya; Camilletti, Alessandro; Chaurasia, Swami Vivekanandji; Doulis, Georgios; Surendra, Padamata,; Rashti, Alireza; Ujevic, Maximiliano; Brügmann, Bernd; Cook, William R.; Dietrich, Tim; Perego, Albino; Poudel, Amit; Tichy, Wolfgang

doi:10.48550/arxiv.2210.16366

Cited by 3 publications

(5 citation statements)

References 142 publications

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“…Instead, we select two sets of filter parameters (Table 1) based on obtaining good overlap (0.82) between our Filter 1 (red, Fig. 1) and the numericalrelativity simulation THC0036 (Dietrich et al 2018;Gonzalez et al 2022). This numerical-relativity waveform uses the SLy equation of state (Douchin & Haensel 2001) for a 1.35 + 1.35 M neutronstar merger (Fig 1,dashed line).…”

Section: Methodsmentioning

confidence: 99%

The effect of noise artefacts on gravitational-wave searches for neutron star post-merger remnants

Panther¹,

Lasky²

2023

Preprint

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Gravitational waves from binary neutron star post-merger remnants have the potential to uncover the physics of the hot nuclear equation of state. These gravitational-wave signals are high frequency (∼ kHz) and short lived (O (10 ms)), which introduces potential problems for data-analysis algorithms due to the presence of non-stationary and non-Gaussian noise artefacts in gravitational-wave observatories. We quantify the degree to which these noise features in LIGO data may affect our confidence in identifying post-merger gravitational-wave signals. We show that the combination of vetoing data with non-stationary glitches and the application of the Allen 𝜒 2 veto (usually reserved for long-lived lower-frequency gravitational-wave signals), allows one to confidently detect post-merger signals with signal-to-noise ratio 𝜌 8. We discuss the need to incorporate the data-quality checks and vetos into realistic post-merger gravitational-wave searches, and describe how one can incorporate them to calculate realistic false-alarm and false-dismissal rates.

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Section: Methodsmentioning

confidence: 99%

The effect of noise artefacts on gravitational-wave searches for neutron star post-merger remnants

Panther¹,

Lasky²

2023

Preprint

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“…We use a cold piecewise polytropic EOS [80] approximating the ALF2 EOS [81] for the neutron star. This prototypical stiff EOS predicts the radius of a 1.4 M ⊙ neutron star to be R 1.4 ∼ 12.32 km [82], has a maximum mass of ∼ 2.0M ⊙ for non-spinning stars [81], and is consistent with pulsar observations [83][84][85][86][87], with both electromagnetic and gravitational wave observations [88][89][90][91][92][93] of the binary neutron star event GW170817 [94], as well as the gravitational wave observations of GW190814 [95] and GW190425 [96]. Thermal effects are added to the zero-temperature polytrope with an additional pressure contribution of the form p th = (Γ th − 1)ρϵ.…”

Section: B Initial Data and Cases Consideredmentioning

confidence: 98%

Nonlinear studies of binary black hole mergers in Einstein-scalar-Gauss-Bonnet gravity

2023

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Gravitational wave observations of black hole-neutron star binaries, particularly those where the black hole has a lower mass compared to other observed systems, have the potential to place strong constraints on modifications to general relativity that arise at small curvature length scales. Here we study the dynamics of black hole-neutron star mergers in shift-symmetric Einstein-scalar-Gauss-Bonnet gravity, a representative example of such a theory, by numerically evolving the full equations of motion. We consider quasi-circular binaries with different mass-ratios that are consistent with recent gravitational wave observations, including cases with and without tidal disruption of the star, and quantify the impact of varying the coupling controlling deviations from general relativity on the gravitational wave signal and scalar radiation. We find that the main effect on the late inspiral is the accelerated frequency evolution compared to general relativity, and that-even considering Gauss-Bonnet coupling values approaching those where the theory breaks down-the impact on the merger gravitational wave signal is mild, predominately manifesting as a small change in the amplitude of the ringdown. We compare our results to current post-Newtonian calculations and find consistency throughout the inspiral.

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“…We adopt a description of the time-domain waveform, similar to that in [26], with the assumption that we can write the source emission as a multipolar expansion of oscillatory mode functions. Specifically, we assume the h + and h × emitted along a line of observation from a given source can be characterized by an expansion in spin-weighted spherical harmonics [27,28]:…”

Section: Waveform Assumptions and Model Implicationsmentioning

confidence: 99%

“…To illustrate the size of current modeling uncertainties, however, we show an example comparing waveform models from lalsimulation [39] and simulations from the CoRe library [28]. This illustrates both the current model differences as well as a possible application of this error budget calculation A(f ) and ϕ(f ).…”

Section: Uncertainty Estimates For Current Modelsmentioning

confidence: 99%

“…Many thanks to the IGWN Conda Distribution, numpy [81], pandas [82], watpy [28], lalsimulation [39], pycbc [72], bilby [83], pesummary [69], and the work of everyone that supports computational infrastructure for the LIGO-Virgo-Kagra collaborations and the gravitational-wave community. I thank David Radice, Wynn Ho, Sanjay Reddy, Josh Smith, Nils Andersson and the Caltech LIGO group for helpful discussion.…”

Section: Acknowledgmentsmentioning

confidence: 99%

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Waveform uncertainty quantification and interpretation for gravitational-wave astronomy

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2023

Class. Quantum Grav.

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We demonstrate how to quantify the frequency-domain amplitude and phase accuracy of waveform models, $\delta A$ and $\delta \phi$, in a form that could be marginalized over in gravitational-wave inference using techniques currently applied for quantifying calibration uncertainty. For concreteness, waveform uncertainties affecting neutron-star inspiral measurements are considered, and post-hoc error estimates from a variety of waveform models are made by comparing time-domain and frequency-domain analytic models with multiple-resolution numerical simulations. These waveform uncertainty estimates can be compared to GW170817 calibration envelopes or to Advanced LIGO and Virgo calibration goals. Signal-specific calibration and waveform uncertainties are compared to statistical fluctuations in gravitational-wave observatories, giving frequency-dependent modeling requirements for detectors such as Advanced LIGO Plus, Cosmic Explorer, or Einstein Telescope. Finally, the distribution of waveform error for the GW170817 posterior is computed from tidal models and compared to the constraints on $\delta \phi$ or $\delta A$ from GWTC-1 by Edelman et. al. In general, $\delta \phi$ and $\delta A$ can also be interpreted in terms of unmodeled astrophysical energy transfer within or from the source system.

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Second release of the CoRe database of binary neutron star merger waveforms

Cited by 3 publications

References 142 publications

The effect of noise artefacts on gravitational-wave searches for neutron star post-merger remnants

The effect of noise artefacts on gravitational-wave searches for neutron star post-merger remnants

Nonlinear studies of binary black hole mergers in Einstein-scalar-Gauss-Bonnet gravity

Waveform uncertainty quantification and interpretation for gravitational-wave astronomy

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