Numerical binary black hole collisions in dynamical Chern-Simons gravity

Okounkova, Maria; Stein, Leo C.; Scheel, Mark A.; Teukolsky, Saul A.

doi:10.1103/physrevd.100.104026

Cited by 104 publications

(91 citation statements)

References 60 publications

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“…It is also a small improvement on the bound of m g ≤ 6.76 × 10 −23 eV=c 2 (90% confidence level) obtained from Solar System ephemerides in [121]. 20 However, these bounds are complementary, since the GW bound comes from the radiative sector, while the Solar System bound considers the static modification to the Newtonian potential. See, e.g., [123] for a review of bounds on the mass of the graviton.…”

mentioning

confidence: 87%

“…Postprocessing techniques to subtract noise contributions and frequency lines from the data around gravitational-wave 1 There are very preliminary simulations of scalar waveforms from binary black holes in the effective field theory (EFT) framework in alternative theories [18,19], and the leading corrections to the gravitational waveforms in head-on collisions [20], but these simulations require much more development before their results can be used in gravitational-wave data analysis. There are also concerns about the mathematical viability of the theories considered when they are not treated in the EFT framework.…”

Section: Data Calibration and Cleaningmentioning

confidence: 99%

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Tests of general relativity with the binary black hole signals from the LIGO-Virgo catalog GWTC-1

Abbott¹,

Abbott²,

Abbott³

et al. 2019

Phys. Rev. D

997

1,218

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The detection of gravitational waves by Advanced LIGO and Advanced Virgo provides an opportunity to test general relativity in a regime that is inaccessible to traditional astronomical observations and laboratory tests. We present four tests of the consistency of the data with binary black hole gravitational waveforms predicted by general relativity. One test subtracts the best-fit waveform from the data and checks the consistency of the residual with detector noise. The second test checks the consistency of the low-and high-frequency parts of the observed signals. The third test checks that phenomenological deviations introduced in the waveform model (including in the post-Newtonian coefficients) are consistent with 0. The fourth test constrains modifications to the propagation of gravitational waves due to a modified dispersion relation, including that from a massive graviton. We present results both for individual events and also results obtained by combining together particularly strong events from the first and second observing runs of Advanced LIGO and Advanced Virgo, as collected in the catalog GWTC-1. We do not find any inconsistency of the data with the predictions of general relativity and improve our previously presented combined constraints by factors of 1.1 to 2.5. In particular, we bound the mass of the graviton to be m g ≤ 4.7 × 10 −23 eV=c 2 (90% credible level), an improvement of a factor of 1.6 over our previously presented results. Additionally, we check that the four gravitational-wave events published for the first time in GWTC-1 do not lead to stronger constraints on alternative polarizations than those published previously.

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mentioning

confidence: 87%

Section: Data Calibration and Cleaningmentioning

confidence: 99%

Tests of general relativity with the binary black hole signals from the LIGO-Virgo catalog GWTC-1

Abbott¹,

Abbott²,

Abbott³

et al. 2019

Phys. Rev. D

997

1,218

View full text Add to dashboard Cite

show abstract

“…Simple EFT analysis reveals that for the values of parameters testable by GW observatories these theories also must have a cutoff at the scale of order of the inverse Schwarzschild radius and require the same assumption about the short-distance behavior as our EFT [15]. These features, required by theoretical consistency, are often missed since these theories are not properly treated as EFTs (see, however, the recent works [15,[24][25][26]). Possible infrared modifications of gravity, like theories of massive gravity, also require a similar sort of assumption about the UV completion [27].…”

Section: B Soft Ultraviolet Completion Of the Effective-fieldtheory mentioning

confidence: 99%

Gravitational-wave constraints on an effective-field-theory extension of general relativity

et al. 2020

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Gravitational-wave observations of coalescing binary systems allow for novel tests of the strong-field regime of gravity. Using data from the Gravitational Wave Open Science Center (GWOSC) of the LIGO and Virgo detectors, we place the first constraints on an effective-field-theory based extension of general relativity, in which only higher-order curvature terms are added to the Einstein-Hilbert action. We construct gravitational-wave templates describing the quasicircular, adiabatic inspiral phase of binary black holes in this extended theory of gravity. Then, after explaining how to properly take into account the region of validity of the effective field theory when performing tests of general relativity, we perform Bayesian model selection using the two lowest-mass binary-black-hole events reported to date by LIGO and Virgo-GW151226 and GW170608-and constrain this theory with respect to general relativity. We find that these data disfavor the appearance of new physics on distance scales around ∼150 km. Finally, we describe a general strategy for improving constraints as more observations will become available with future detectors on the ground and in space.

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“…In addition, there is in general no analog of the Teukolsky equation [6,58,59] beyond GR. In general the perturbation equations are not separable [60], and this requires the solution of an elliptic system of partial differential equations [61] or the extraction of QNM frequencies from numerical-relativity simulations of BH mergers [62][63][64][65].…”

Section: Introductionmentioning

confidence: 99%

Parametrized ringdown spin expansion coefficients: A data-analysis framework for black-hole spectroscopy with multiple events

et al. 2020

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Black-hole spectroscopy is arguably the most promising tool to test gravity in extreme regimes and to probe the ultimate nature of black holes with unparalleled precision. These tests are currently limited by the lack of a ringdown parametrization that is both robust and accurate. We develop an observable-based parametrization of the ringdown of spinning black holes beyond general relativity, which we dub ParSpec (Parametrized Ringdown Spin Expansion Coefficients). This approach is perturbative in the spin, but it can be made arbitrarily precise (at least in principle) through a high-order expansion. It requires O(10) ringdown detections, which should be routinely available with the planned space mission LISA and with third-generation ground-based detectors. We provide a preliminary analysis of the projected bounds on parametrized ringdown parameters with LISA and with the Einstein Telescope, and discuss extensions of our model that can be straightforwardly included in the future. arXiv:1910.12893v1 [gr-qc] 28 Oct 2019where J = 1, 2, ..., q labels the mode; M i and χ i 1 are the detector-frame mass and spin of the i-th source, both measured assuming GR (see below); D is the order of the spin expansion; w (n) J and t (n) J are the dimensionless coefficients of the spin expansion for a Kerr BH in GR (provided in Table I for a few representative modes); γ i are dimensionless coupling constants, which can depend on the source i -see Eq. (6) below -but do not depend 1 The QNMs are identified by three integer numbers: the angular momentum number l, the azimuthal number m ∈ [−l, l], and the overtone number, which we set to zero in this paper, i.e. we only consider fundamental modes. For ease of notation we leave these indices implicit, i.e. ω (J) ≡ ω (0lm) , where J is an index that labels the mode. (n) J and δt (n) J (n) J and δt (n) J (or, equivalently, δW (n) J and δT (n) J ), these corrections depend only on the theory and not on the source.It is easy to check that, to leading order in α, the redefinitionsbring Eqs. (A1) and (A2) to the form in Eqs.(3) and (4) used in the main text. The above redefinitions also show that there is some degeneracy among the beyond-GR parameters, and that one can only constrain the combinations δw (n) J and δt (n) J , which contains the intrinsic mode corrections (δW (n) J and δT (n) J ) and the mass and spin corrections (δm and δχ).(n) J and δt (n) J are unconstrained by the data.

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Numerical binary black hole collisions in dynamical Chern-Simons gravity

Cited by 104 publications

References 60 publications

Tests of general relativity with the binary black hole signals from the LIGO-Virgo catalog GWTC-1

Tests of general relativity with the binary black hole signals from the LIGO-Virgo catalog GWTC-1

Gravitational-wave constraints on an effective-field-theory extension of general relativity

Parametrized ringdown spin expansion coefficients: A data-analysis framework for black-hole spectroscopy with multiple events

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