Frequency-domain reduced order models for gravitational waves from aligned-spin compact binaries

Pürrer, M.

doi:10.1088/0264-9381/31/19/195010

Cited by 205 publications

(291 citation statements)

References 118 publications

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“…[35] using NR waveforms from Ref. [36], enhanced with reduced-order modeling [37] to speed up waveform generation [38,39] (henceforth, EOBNR), and the single effective spin, precessing waveform model of Refs. [40][41][42] (henceforth, IMRPHENOM).…”

mentioning

confidence: 99%

Tests of General Relativity with GW150914

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. Lett.

1,778

1,699

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The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10 13 km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity.

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mentioning

confidence: 99%

Tests of General Relativity with GW150914

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. Lett.

1,778

1,699

View full text Add to dashboard Cite

show abstract

“…PCA via Singular Value Decomposition (SVD) is applied to the catalog waveforms to create signal models that represent each explosion mechanism. Similar techniques have been used to extract physical parameters of GW signals from binary systems [71][72][73] and in characterizing noise sources in GW detectors [74,75].…”

Section: Smeementioning

confidence: 99%

Inferring the core-collapse supernova explosion mechanism with gravitational waves

et al. 2016

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A detection of a core-collapse supernova (CCSN) gravitational-wave (GW) signal with an Advanced LIGO and Virgo detector network may allow us to measure astrophysical parameters of the dying massive star. GWs are emitted from deep inside the core and, as such, they are direct probes of the CCSN explosion mechanism. In this study we show how we can determine the CCSN explosion mechanism from a GW supernova detection using a combination of principal component analysis and Bayesian model selection. We use simulations of GW signals from CCSN exploding via neutrino-driven convection and rapidly-rotating core collapse. Previous studies have shown that the explosion mechanism can be determined using one LIGO detector and simulated Gaussian noise. As real GW detector noise is both non-stationary and non-Gaussian we use real detector noise from a network of detectors with a sensitivity altered to match the advanced detectors design sensitivity. For the first time we carry out a careful selection of the number of principal components to enhance our model selection capabilities. We show that with an advanced detector network we can determine if the CCSN explosion mechanism is neutrino-driven convection for sources in our Galaxy and rapidly-rotating core collapse for sources out to the Large Magellanic Cloud.

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“…At present EOB waveforms for spinning BH binaries are computationally expensive to generate (although far faster than doing NR simulations) and hence not suitable for use in Markov Chain Monte Carlo-based parameter estimation methods. Quite importantly, accelerated waveform generation techniques that use reduced-order algorithms or singular-value decomposition techniques have been proposed to address such problems [411][412][413][414][415].…”

Section: Challengesmentioning

confidence: 99%