How should spin-weighted spherical functions be defined?

Boyle, Michael

doi:10.1063/1.4962723

Cited by 30 publications

(30 citation statements)

References 32 publications

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“…We use the sign conventions for spin-weighted spherical harmonics as given in Ref. [126,235]. In terms of θ and φ we give the spin-weight −2 spherical harmonics for l = 2 as an example, −2 Y 2 ±2 = 5 64π…”

Section: Sign Conventionsmentioning

confidence: 99%

The SXS collaboration catalog of binary black hole simulations

Boyle

Hemberger

Iozzo

et al. 2019

Class. Quantum Grav.

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361

409

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Accurate models of gravitational waves from merging black holes are necessary for detectors to observe as many events as possible while extracting the maximum science. Near the time of merger, the gravitational waves from merging black holes can be computed only using numerical relativity. In this paper, we present a major update of the Simulating eXtreme Spacetimes (SXS) Collaboration catalog of numerical simulations for merging black holes. The catalog contains 2018 distinct configurations (a factor of 11 increase compared to the 2013 SXS catalog), including 1426 spin-precessing configurations, with mass ratios between 1 and 10, and spin magnitudes up to 0.998. The median length of a waveform in the catalog is 39 cycles of the dominant = m = 2 gravitational-wave mode, with the shortest waveform containing 7.0 cycles and the longest 351.3 cycles. We discuss improvements such as correcting for moving centers of mass and extended coverage of the parameter space. We also present a thorough analysis of numerical errors, finding typical truncation errors corresponding to a waveform mismatch of ∼ 10 −4 . The simulations provide remnant masses and spins with uncertainties of 0.03% and 0.1% (90 th percentile), about an order of magnitude better than analytical models for remnant properties. The full catalog is publicly available at https://www.black-holes.org/waveforms . black holes and of the surrounding spacetime [31,32]. Simulations have also been used for visualizations of curved spacetime [33][34][35][36][37][38][39][40], investigations of spin quantities [41], and the relaxation of spacetime to the Kerr solution following merger [42][43][44]. The motion of the black hole horizons and horizon curvature quantities have been used to explore eccentric dynamics [45][46][47][48], spin precession [49][50][51][52], and the first law of binary black hole mechanics [53][54][55][56][57]. These in turn have been compared to analytic post-Newtonian and self-force approximations (see also [58][59][60]), mapping out the bounds of validity of these approximations.A key application of BBH simulations is the accurate modeling of gravitational waves emitted by these systems during their late inspiral, merger, and final ringdown. Waveforms extracted from BBH simulations are essential for analyzing observed gravitational-wave signals from black hole binaries. Indeed, all BBH observations by LIGO and Virgo were analyzed using waveform families that rely on numerical relativity for their construction, most notably effective-one-body waveform models [61-65] and phenomenological waveform models [66][67][68]. Numerical simulations are also central in validating such waveform models [69][70][71][72][73][74][75][76], and were used to validate GW searches [77][78][79]. Waveforms from numerical relativity are also used directly in parameter estimation [80,81], to construct template banks [82], and to construct waveform families without intermediate analytical models, using methods such as reduced order modeling [83][84][85][86]. Today's simula...

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Section: Sign Conventionsmentioning

confidence: 99%

The SXS collaboration catalog of binary black hole simulations

Boyle

Hemberger

Iozzo

et al. 2019

Class. Quantum Grav.

Self Cite

361

409

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“…We follow the conventions of [17], section 4.15. Instructive alternative presentations and perspectives can be found in [96][97][98][99], section 1.10, [100,101].…”

Section: Jhep06(2021)079mentioning

confidence: 99%

Coadjoint representation of the BMS group on celestial Riemann surfaces

Barnich

Ruzziconi

2021

J. High Energ. Phys.

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“…[139][140][141][142][143][144] (see also e.g. [145][146][147][148]). First of all, the spin operators are defined in the following way…”

Section: Discussionmentioning

confidence: 99%

Relativistic wide-angle galaxy bispectrum on the light cone

et al. 2018

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Given the important role that the galaxy bispectrum has recently acquired in cosmology and the scale and precision of forthcoming galaxy clustering observations, it is timely to derive the full expression of the large-scale bispectrum going beyond approximated treatments which neglect integrated terms or higher-order bias terms or use the Limber approximation. On cosmological scales, relativistic effects that arise from observing the past light cone alter the observed galaxy number counts, therefore leaving their imprints on N-point correlators at all orders. In this paper we compute for the first time the bispectrum including all general relativistic, local and integrated, effects at second order, the tracers' bias at second order, geometric effects as well as the primordial non-Gaussianity contribution. This is timely considering that future surveys will probe scales comparable to the horizon where approximations widely used currently may not hold; neglecting these effects may introduce biases in estimation of cosmological parameters as well as primordial non-Gaussianity.

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How should spin-weighted spherical functions be defined?

Cited by 30 publications

References 32 publications

The SXS collaboration catalog of binary black hole simulations

The SXS collaboration catalog of binary black hole simulations

Coadjoint representation of the BMS group on celestial Riemann surfaces

Relativistic wide-angle galaxy bispectrum on the light cone

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