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Dr.  Benjamin  Knispel
Dr. Benjamin Knispel
Press Officer AEI Hannover
Phone:+49 511 762-19104Fax:+49 511 762-17182

Publication

1.
Lionel London, Sebastian Khan, Edward Fauchon-Jones, Cecilio García, Mark Hannam, Sascha Husa, Xisco Jiménez-Forteza, Chinmay Kalaghatgi, Frank Ohme, and Francesco Pannarale
First Higher-Multipole Model of Gravitational Waves from Spinning and Coalescing Black-Hole Binaries

Gravitational waveforms with higher modes from merging black holes

The first higher-multipole model of spinning and coalescing black-hole binaries improves accuracy of waveforms and measurement of astrophysical parameters

April 19, 2018

Together with international colleagues, AEI researchers have for the first time created a higher-multipole model of gravitational waves from binary black holes during inspiral, merger, and ringdown by combining post-Newtonian and pertubation theoretical methods. Their PhenomHM model is an extension of the widely used PhenomD model and is more accurate than the latter for all binary configurations, typically improves the measurement of binary properties, and will also be valuable in strengthening current tests of general relativity.
A GW signal decomposed into its multipolar contributions, for a system with mass ratio 1:8 and spin on the larger BH is χ1=S1/m12=(0,0,−0.5). Our model (PhenomHM) is included as solid (m=l) and dashed (m=l−1) black lines. NR multipoles are displayed in gray, thick lines. Axes are in dimensionless units, where M is the total system mass and dL is the source’s luminosity distance. Zoom Image
A GW signal decomposed into its multipolar contributions, for a system with mass ratio 1:8 and spin on the larger BH is χ1=S1/m12=(0,0,−0.5). Our model (PhenomHM) is included as solid (m=l) and dashed (m=l−1) black lines. NR multipoles are displayed in gray, thick lines. Axes are in dimensionless units, where M is the total system mass and dL is the source’s luminosity distance. [less]

Paper abstract

Gravitational-wave observations of binary black holes currently rely on theoretical models that predict the dominant multipoles (l=2, |m|=2) of the radiation during inspiral, merger, and ringdown. We introduce a simple method to include the subdominant multipoles to binary black hole gravitational waveforms, given a
frequency-domain model for the dominant multipoles. The amplitude and phase of the original model are appropriately stretched and rescaled using post-Newtonian results (for the inspiral), perturbation theory (for the ringdown), and a smooth transition between the two. No additional tuning to numerical-relativity simulations is required. We apply a variant of this method to the nonprecessing PhenomD model. The result, PhenomHM, constitutes the first higher-multipole model of spinning and coalescing black-hole binaries, and currently includes the (l,|m|)=(2,2),(3,3),(4,4),(2,1),(3,2),(4,3) radiative moments. Comparisons with numerical-relativity waveforms demonstrate that PhenomHM is more accurate than dominant-multipole-only models for all binary configurations, and typically improves the measurement of binary properties.

 
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