Constructing gravitational waves from generic spin-precessing compact binary inspirals

Chatziioannou, Katerina; Klein, Antoine; Yunes, Nicolás; Cornish, N.

doi:10.1103/physrevd.95.104004

Cited by 176 publications

(218 citation statements)

References 71 publications

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“…We compare the 90% credible interval presented in Fig. 5 of [17] for GW150914 signal to the Fisher matrix calculations using the approximate relation ∆ 90% ≈ 1.64 × σ Fisher 10 [35][36][37]. We see that the Fisher matrix underestimates the errors considerably 11 .…”

Section: A On the Statistical Errormentioning

confidence: 88%

Ringdown overtones, black hole spectroscopy, and no-hair theorem tests

et al. 2020

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Validating the black-hole no-hair theorem with gravitational-wave observations of compact binary coalescences provides a compelling argument that the remnant object is indeed a black hole as described by the general theory of relativity. This requires performing a spectroscopic analysis of the post-merger signal and resolving the frequencies of either different angular modes or overtones (of the same angular mode). For a nearly-equal mass binary black-hole system, only the dominant angular mode (l = m = 2) is sufficiently excited and the overtones are instrumental to perform this test. Here we investigate the robustness of modelling the post-merger signal of a binary black hole coalescence as a superposition of overtones. Further, we study the bias expected in the recovered frequencies as a function of the start time of a spectroscopic analysis and provide a computationally cheap procedure to choose it based on the interplay between the expected statistical error due to the detector noise and the systematic errors due to waveform modelling. Moreover, since the overtone frequencies are closely spaced, we find that resolving the overtones is particularly challenging and requires a loud ringdown signal. Rayleigh's resolvability criterion suggests that -in an optimistic scenario -a ringdown signal-to-noise ratio larger than ∼ 30 (achievable possibly with LIGO at design sensitivity and routinely with future interferometers such as Einstein Telescope, Cosmic Explorer, and LISA) is necessary to resolve the overtone frequencies. We then conclude by discussing some conceptual issues associated with black-hole spectroscopy with overtones.

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Section: A On the Statistical Errormentioning

confidence: 88%

Ringdown overtones, black hole spectroscopy, and no-hair theorem tests

et al. 2020

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“…For a geometric depiction, see Figure 1 in Ref. [36] 2 . This procedure was used to produce the first precessing IMR models [20,21,23].…”

Section: B Modeling Precessing Bbhsmentioning

confidence: 99%

“…In this paper we take another step towards a computationally-tractable GW model that accurately models generic BBH systems by introducing the frequency-domain fully-precessing phenomenological model, IMRPhenomPv3, that describes the inspiral, merger, and ringdown phases of spinning BBHs. Our upgrade from IMRPhenomPv2 to IMRPhenomPv3 hinges on a novel closed-form solution to the differential equations that describe precession including the effects of radiation reaction in the Post Newtonian (PN) regime where the binary components are well-separated [36,37]. This closed-form solution to the precession equations including the effects of radiation reaction has been shown to accurately describe precession for systems with generic masses and spins [36].…”

Section: Introductionmentioning

confidence: 99%

Phenomenological model for the gravitational-wave signal from precessing binary black holes with two-spin effects

et al. 2019

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The properties of compact binaries, such as masses and spins, are imprinted in the gravitationalwaves they emit and can be measured using parameterised waveform models. Accurately and efficiently describing the complicated precessional dynamics of the various angular momenta of the system in these waveform models is the object of active investigation. One of the key models extensively used in the analysis of LIGO and Virgo data is the single-precessing-spin waveform model IMRPhenomPv2. In this article we present a new model IMRPhenomPv3 which includes the effects of two independent spins in the precession dynamics. Whereas IMRPhenomPv2 utilizes a single-spin frequency-dependent post-Newtonian rotation to describe precession effects, the improved model, IMRPhenomPv3, employs a double-spin rotation that is based on recent developments in the description of precessional dynamics. Besides double-spin precession, the improved model benefits from a more accurate description of precessional effects. We validate our new model against a large set of precessing numerical-relativity simulations. We find that IMRPhenomPv3 has better agreement with the inspiral portion of precessing binary-black-hole simulations and is more robust across a larger region of the parameter space than IMRPhenomPv2. As a first application we analyse, for the first time, the gravitational-wave event GW151226 with a waveform model that describes two-spin precession. Within statistical uncertainty our results are consistent with published results. IMRPhenomPv3 will allow studies of the measurability of individual spins of binary black holes using GWs and can be used as a foundation upon which to build further improvements, such as modeling precession through merger, extending to higher multipoles, and including tidal effects.PACS numbers: 04.80. Nn, 04.25.dg, 95.85.Sz, 97.80.-d arXiv:1809.10113v1 [gr-qc]

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“…The GWB amplitude is near the threshold level identified in Figure 2, and in the combined search yielded a Bayes factor of BF GWB = 1.18 +0. 39 −0.29 . Figure 5 shows the identified sources with their BF CW values and f GW − log 10 h GW posterior samples.…”

Section: Stochastic Background and Continuous Wavesmentioning

confidence: 99%

Joint search for isolated sources and an unresolved confusion background in pulsar timing array data

Bazzan

Cornish

2020

Class. Quantum Grav.

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Supermassive black hole binaries are the most promising source of gravitational-waves in the frequency band accessible to pulsar timing arrays. Most of these binaries will be too distant to detect individually, but together they will form an approximately stochastic background that can be detected by measuring the correlation pattern induced between pairs of pulsars. A small number of nearby and especially massive systems may stand out from this background and be detected individually. Analyses have previously been developed to search for stochastic signals and isolated signals separately. Here we present BayesHopper, an algorithm capable of jointly searching for both signal components simultaneously using transdimensional Bayesian inference. Our implementation uses the Reversible Jump Markov Chain Monte Carlo method for sampling the relevant parameter space with changing dimensionality. We have tested BayesHopper on various simulated datasets. We find that it gives results consistent with fixed-dimensional methods when tested on data with a stochastic background or data with a single binary. For the full problem of analyzing a dataset with both a background and multiple black hole binaries, we find two kinds of interactions between the binary and background components. First, the background effectively increases the noise level, thus making individual binary signals less significant. Second, weak binary signals can be absorbed by the background model due to the natural parsimony of Bayesian inference. Because of its flexible model structure, we anticipate that BayesHopper will outperform existing approaches when applied to realistic data sets produced from population synthesis models.

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Constructing gravitational waves from generic spin-precessing compact binary inspirals

Cited by 176 publications

References 71 publications

Ringdown overtones, black hole spectroscopy, and no-hair theorem tests

Ringdown overtones, black hole spectroscopy, and no-hair theorem tests

Phenomenological model for the gravitational-wave signal from precessing binary black holes with two-spin effects

Joint search for isolated sources and an unresolved confusion background in pulsar timing array data

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