Time-domain effective-one-body gravitational waveforms for coalescing compact binaries with nonprecessing spins, tides, and self-spin effects

Alessandro Nagar, Sebastiano Bernuzzi, Walter Del Pozzo, Gunnar Riemenschneider, Sarp Akcay, Gregorio Carullo, Philipp Fleig, Stanislav Babak, Ka Wa Tsang, Marta Colleoni, Francesco Messina, Geraint Pratten, David Radice, Piero Rettegno, Michalis Agathos, Edward Fauchon-Jones, Mark Hannam, Sascha Husa, Tim Dietrich, Pablo Cerdá-Duran, José A. Font, Francesco Pannarale, Patricia Schmidt, and Thibault Damour

Phys. Rev. D 98, 104052 – Published 28 November 2018

Abstract

We present TEOBResumS, a new effective-one-body (EOB) waveform model for nonprecessing (spin-aligned) and tidally interacting compact binaries. Spin-orbit and spin-spin effects are blended together by making use of the concept of centrifugal EOB radius. The point-mass sector through merger and ringdown is informed by numerical relativity (NR) simulations of binary black holes (BBHs) computed with the SpEC and bam codes. An improved, NR-based phenomenological description of the postmerger waveform is developed. The tidal sector of TEOBResumS describes the dynamics of neutron star binaries up to merger and incorporates a resummed attractive potential motivated by recent advances in the post-Newtonian and gravitational self-force description of relativistic tidal interactions. Equation-of-state-dependent self-spin interactions (monopole-quadrupole effects) are incorporated in the model using leading order post-Newtonian results in a new expression of the centrifugal radius. TEOBResumS is compared to 135 SpEC and 19 bam BBH waveforms. The maximum unfaithfulness to SpEC data $\bar{F}$ —at design Advanced LIGO sensitivity and evaluated with total mass $M$ with a variance of $10 M_{⊙} \leq M \leq 200 M_{⊙}$ —is always below $2.5 \times 10^{- 3}$ except for a single outlier that grazes the $7.1 \times 10^{- 3}$ level. When compared to bam data, $\bar{F}$ is smaller than 0.01 except for a single outlier in one of the corners of the NR-covered parameter space that reaches the 0.052 level. TEOBResumS is also compatible, up to merger, to high-end NR waveforms from binary neutron stars with spin effects and reduced initial eccentricity computed with the bam and thc codes. The data quality of binary neutron star waveforms is assessed via rigorous convergence tests from multiple resolution runs and takes into account systematic effects estimated by using the two independent high-order NR codes. The model is designed to generate accurate templates for the analysis of LIGO-Virgo data through merger and ringdown. We demonstrate its use by analyzing the publicly available data for GW150914.

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Received 5 June 2018

DOI:https://doi.org/10.1103/PhysRevD.98.104052

Physics Subject Headings (PhySH)

Gravitation Gravitational waves

Gravitation, Cosmology & Astrophysics

Authors & Affiliations

Alessandro Nagar^1,2,3, Sebastiano Bernuzzi^4,5,6, Walter Del Pozzo⁷, Gunnar Riemenschneider^2,8, Sarp Akcay⁴, Gregorio Carullo⁷, Philipp Fleig⁹, Stanislav Babak^10,11, Ka Wa Tsang¹¹, Marta Colleoni¹², Francesco Messina^13,14, Geraint Pratten¹², David Radice^15,16, Piero Rettegno^2,8, Michalis Agathos¹⁷, Edward Fauchon-Jones¹⁸, Mark Hannam¹⁸, Sascha Husa¹², Tim Dietrich^11,19, Pablo Cerdá-Duran²⁰, José A. Font^20,21, Francesco Pannarale^18,22, Patricia Schmidt²³, and Thibault Damour³

¹Centro Fermi—Museo Storico della Fisica e Centro Studi e Ricerche Enrico Fermi,00184 Rome, Italy
²INFN Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy
³Institut des Hautes Etudes Scientifiques, 91440 Bures-sur-Yvette, France
⁴Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, 07743 Jena, Germany
⁵Istituto Nazionale di Fisica Nucleare, Sezione Milano Bicocca, gruppo collegato di Parma, I-43124 Parma, Italy
⁶Department of Mathematical, Physical and Computer Sciences, University of Parma, I-43124 Parma, Italy
⁷Dipartimento di Fisica “Enrico Fermi”, Università di Pisa, and INFN sezione di Pisa, Pisa I-56127, Italy
⁸Dipartimento di Fisica, Università di Torino, via P. Giuria 1, I-10125 Torino, Italy
⁹Max Planck Institute for Dynamics and Self-Organization, 37077 Göttingen, Germany
¹⁰APC, CNRS-Université Paris 7, 75205 Paris CEDEX 13, France
¹¹Moscow Institute of Physics and Technology, Dolgoprudny, Moscow region, Russia
¹²Universitat de les Illes Balears, IAC3-IEEC, 07122 Palma de Mallorca, Spain
¹³Dipartimento di Fisica, Università degli studi di Milano Bicocca, Piazza della Scienza 3, 20126 Milano, Italy
¹⁴INFN, Sezione di Milano Bicocca, Piazza della Scienza 3, 20126 Milano, Italy
¹⁵Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, New Jersey 08544, USA
¹⁶Institute for Advanced Study, 1 Einstein Drive, Princeton, New Jersey 08540, USA
¹⁷DAMTP, Centre for Mathematical Sciences, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA, United Kingdom
¹⁸Gravity Exploration Institute, School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA, United Kingdom
¹⁹Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, Potsdam 14476, Germany
²⁰Departament d’Astronomia i Astrofśica, Universitat de València, Doctor Moliner 50, 46100 Burjassot, València, Spain
²¹Observatori Astronòmic, Universitat de València, C/Catedrático José Beltrán 2, 46980, Paterna, València, Spain
²²Dipartimento di Fisica, Università di Roma “Sapienza” and Sezione INFN Roma1, piazzale A. Moro 5, 00185, Roma, Italy
²³Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6525 GL Nijmegen, The Netherlands

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Vol. 98, Iss. 10 — 15 November 2018

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