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Effective-one-body model for black-hole binaries with generic mass ratios and spins

Andrea TaracchiniDepartment of Physics, Maryland Center for Fundamental Physics and Joint Space-Science Institute, University of Maryland, College Park, Maryland 20742, USAAlessandra BuonannoDepartment of Physics, Maryland Center for Fundamental Physics and Joint Space-Science Institute, University of Maryland, College Park, Maryland 20742, USAYi PanDepartment of Physics, Maryland Center for Fundamental Physics and Joint Space-Science Institute, University of Maryland, College Park, Maryland 20742, USATanja HindererDepartment of Physics, Maryland Center for Fundamental Physics and Joint Space-Science Institute, University of Maryland, College Park, Maryland 20742, USAMichael BoyleCenter for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853, USADaniel A. HembergerCenter for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853, USALawrence E. KidderCenter for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853, USAGeoffrey LovelaceGravitational Wave Physics and Astronomy Center, California State University Fullerton, Fullerton, California 92831, USAAbdul MrouéCanadian Institute for Theoretical Astrophysics, 60 St. George Street, University of Toronto, Toronto, Ontario M5S 3H8, CanadaHarald PfeifferCanadian Institute for Advanced Research, 180 Dundas Street West, Toronto, Ontario M5 G 1Z8, CanadaMark ScheelTheoretical Astrophysics 350-17, California Institute of Technology, Pasadena, California 91125, USABéla SzilágyiTheoretical Astrophysics 350-17, California Institute of Technology, Pasadena, California 91125, USANicholas TaylorTheoretical Astrophysics 350-17, California Institute of Technology, Pasadena, California 91125, USAAnıl ZenginoğluTheoretical Astrophysics 350-17, California Institute of Technology, Pasadena, California 91125, USA

2014en

ABI

Annotatsiya

Gravitational waves emitted by black-hole binary systems have the highest signal-to-noise ratio in LIGO and Virgo detectors when black-hole spins are aligned with the orbital angular momentum and extremal. For such systems, we extend the effective-one-body inspiral-merger-ringdown waveforms to generic mass ratios and spins calibrating them to 38 numerical-relativity nonprecessing waveforms produced by the SXS Collaboration. The numerical-relativity simulations span mass ratios from 1 to 8, spin magnitudes up to 98% of extremality, and last for 40 to 60 gravitational-wave cycles. When the total mass of the binary is between 20 and $200{M}_{\ensuremath{\bigodot}}$, the effective-one-body nonprecessing (dominant mode) waveforms have overlap above 99% (using the advanced-LIGO design noise spectral density) with all of the 38 nonprecessing numerical waveforms, when maximizing only on initial phase and time. This implies a negligible loss in event rate due to modeling. We also show that---without further calibration--- the precessing effective-one-body (dominant mode) waveforms have overlap above 97% with two very long, strongly precessing numerical-relativity waveforms, when maximizing only on the initial phase and time.

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Identifikatorlar

DOI: 10.1103/physrevd.89.061502

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