Fast and accurate inference on gravitational waves from precessing compact binaries

Smith, R. J. E.; Field, Scott E.; Blackburn, K.; Haster, C.-J.; Pürrer, M.; Raymond, V.; Schmidt, P.

doi:10.1103/physrevd.94.044031

Cited by 161 publications

(224 citation statements)

References 48 publications

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“…This suggests that a hybrid model where the numerical or the analytical SUA is called depending on the system's mass can achieve both high accuracy and numerical efficiency. Further improvement could be obtained through reduced order modeling and reduced order quadrature integration in data analysis implementations [69]. We leave such studies to future work.…”

Section: Discussionmentioning

confidence: 99%

Constructing gravitational waves from generic spin-precessing compact binary inspirals

et al. 2017

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The coalescence of compact objects is one of the most promising sources, as well as the source of the first detections, of gravitational waves for ground-based interferometric detectors, such as advanced LIGO and Virgo. Generically, compact objects in binaries are expected to be spinning with spin angular momenta misaligned with the orbital angular momentum, causing the orbital plane to precess. This precession adds rich structure to the gravitational waves, introducing such complexity that an analytic closed-form description has been unavailable until now. We here construct the first closed-form frequency-domain gravitational waveforms that are valid for generic spin-precessing quasicircular compact binary inspirals. We first construct time-domain gravitational waves by solving the post-Newtonian precession equations of motion with radiation reaction through multiple scale analysis. We then Fourier transform these time-domain waveforms with the method of shifted uniform asymptotics to obtain closed-form expressions for frequency-domain waveforms. We study the accuracy of these analytic, frequency-domain waveforms relative to waveforms obtained by numerically evolving the post-Newtonian equations of motion and find that they are suitable for unbiased parameter estimation for 99.2%(94.6%) of the binary configurations we studied at a signal-to-noise ratio of 10(25). These new frequency-domain waveforms could be used for detection and parameter estimation studies due to their accuracy and low computational cost.

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Section: Discussionmentioning

confidence: 99%

Constructing gravitational waves from generic spin-precessing compact binary inspirals

et al. 2017

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“…The calculation is carried out using LAL-Inference. We employ reduced order modeling and reduced order quadrature methods to control the computational cost of the analysis [27].…”

Section: Demonstration Using Gaussian Noisementioning

confidence: 99%

“…Figure 4 implies that, at design sensitivity, a realistic astrophysical background with an effective z < 0.77 duty cycle of (ξ true = 4 × 10 −4 ) could be detected using ≈ 17000 4 s data segments. At the time of writing, a typical run-time of LALInference on 4 s data segments is usually no more than 10 CPU hours [27]. To produce evi-dences in a two detector network, we perform three separate runs: a coherent analysis which produces (Z i S , Z i N ); and two incoherent analysis which produce (Z i,(j) S , Z i,(j) N ) where the index j labels the detector, j = (1, 2).…”

Section: Time To Detectionmentioning

confidence: 99%

Optimal Search for an Astrophysical Gravitational-Wave Background

Smith

Thrane²

2018

Phys. Rev. X

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110

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Roughly every 2-10 minutes, a pair of stellar mass black holes merge somewhere in the Universe. A small fraction of these mergers are detected as individually resolvable gravitational-wave events by advanced detectors such as LIGO and Virgo. The rest contribute to a stochastic background. We derive the statistically optimal search strategy (producing minimum credible intervals) for a background of unresolved binaries. Our method applies Bayesian parameter estimation to all available data. Using Monte Carlo simulations, we demonstrate that the search is both "safe" and effective: it is not fooled by instrumental artifacts such as glitches and it recovers simulated stochastic signals without bias. Given realistic assumptions, we estimate that the search can detect the binary black hole background with about one day of design sensitivity data versus ≈ 40 months using the traditional cross-correlation search. This framework independently constrains the merger rate and black hole mass distribution, breaking a degeneracy present in the cross-correlation approach. The search provides a unified framework for population studies of compact binaries, which is cast in terms of hyper-parameter estimation. We discuss a number of extensions and generalizations including: application to other sources (such as binary neutron stars and continuous-wave sources), simultaneous estimation of a continuous Gaussian background, and applications to pulsar timing.

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“…We use nested sampling implementation of LALInference [75] to stochastically explore the parameter space and produce posterior distributions for θ. To reduce the computational cost of the likelihood evaluations, we use the reduced order quadrature (ROQ) approximation [78]. Sampling the parameter space to measure the properties of weak signals in presence of strong priors can be challenging.…”

Section: B Bayesian Parameter Estimationmentioning

confidence: 99%

Characterization of low-significance gravitational-wave compact binary sources

Huang

Middleton

et al. 2018

Phys. Rev. D

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Advanced LIGO and Virgo have so far detected gravitational waves from 10 binary black hole mergers (BBH) and 1 binary neutron star merger (BNS). In the future, we expect the detection of many more marginal sources, since compact binary coalescences detectable by advanced ground-based instruments are roughly distributed uniformly in comoving volume. In this paper we simulate weak signals from compact binary coalescences of various morphologies and optimal network signal-to-noise ratios (henceforth SNRs), and analyze if and to which extent their parameters can be measured by advanced LIGO and Virgo in their third observing run. We show that subthreshold binary neutron stars, with SNRs below 12 (10) yield uncertainties in their sky position larger than 400 (700) deg 2 (90% credible interval). The luminosity distance, which could be used to measure the Hubble constant with standard sirens, has relative uncertainties larger than 40% for BNSs and neutron star black hole mergers. For sources with SNRs below 8, it is not uncommon that the extrinsic parameters, sky position and distance, cannot be measured. Next, we look at the intrinsic parameters, masses and spins. We show that the detector-frame chirp mass can sometimes be measured with uncertainties below 1% even for sources at SNRs of 6, although multimodality is not uncommon and can significantly broaden the posteriors. The effective inspiral spin is best measured for neutron star black hole mergers, for which the uncertainties can be as low as ∼ 0.08 (∼ 0.2) at SNR 12 (8). The uncertainty is higher for systems with comparable component masses or lack of spin precession. * ywh@mit.edu † salvatore.vitale@ligo.org possibility of multimessenger observations. This has been spectacularly shown with the joint detection of GW and EM signals from the BNS source GW170817 [30]. The host of GW170817 was identified, together with radiation in the whole EM spectrum, from radio to γ-rays [30][31][32][33][34]. The science output of this discovery is too rich to be fully described here. We thus only mention a few highlights. GW170817 was used to set constraints on the equation of state of neutron stars [35], search for evidence of p-g modes [36] and put bounds on the component neutron star masses and spins [13]. The EM data confirmed the connection between short gamma-ray bursts and BNS sources, lead to the observation of the kilonova, and yielded insights on the details of the EM emission [37][38][39][40]. Information from both the GW and the EM sides was used to measure the Hubble constant in a way that is independent of the cosmic distance ladder [41]. As more BNSs are detected in the next years, we will be able to gain a more solid understanding of the properties of compact binaries, their progenitors, and the electromagnetic radiation they emit.Given the current detections, it is possible to estimate the local merger rates of binary neutron stars [12] and binary black holes [5,8,15]. Neutron star black hole mergers (NSBHs) are also promising sources, but have not been detected...

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Fast and accurate inference on gravitational waves from precessing compact binaries

Cited by 161 publications

References 48 publications

Constructing gravitational waves from generic spin-precessing compact binary inspirals

Constructing gravitational waves from generic spin-precessing compact binary inspirals

Optimal Search for an Astrophysical Gravitational-Wave Background

Characterization of low-significance gravitational-wave compact binary sources

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