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#### Bayesian inference of binary black holes with inspiral-merger-ringdown waveforms using two eccentric parameters

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2309.15528.pdf

(Preprint), 4MB

PhysRevD.108.124063.pdf

(Publisher version), 5MB

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##### Citation

Ramos-Buades, A., Buonanno, A., & Gair, J. (2023). Bayesian inference of binary
black holes with inspiral-merger-ringdown waveforms using two eccentric parameters.* Physical Review
D,* *108*(12): 124063. doi:10.1103/PhysRevD.108.124063.

Cite as: https://hdl.handle.net/21.11116/0000-000D-CC5E-5

##### Abstract

Orbital eccentricity is a crucial physical effect to unveil the origin of

compact-object binaries detected by ground- and spaced-based gravitational-wave

(GW) observatories. Here, we perform for the first time a Bayesian inference

study of inspiral-merger-ringdown eccentric waveforms for binary black holes

with non-precessing spins using two (instead of one) eccentric parameters:

eccentricity and relativistic anomaly. We employ for our study the multipolar

effective-one-body (EOB) waveform model SEOBNRv4EHM, and use initial conditions

such that the eccentric parameters are specified at an orbit-averaged

frequency. We show that this new parametrization of the initial conditions

leads to a more efficient sampling of the parameter space. We also assess the

impact of the relativistic-anomaly parameter by performing mock-signal

injections, and we show that neglecting such a parameter can lead to

significant biases in several binary parameters. We validate our model with

mock-signal injections based on numerical-relativity waveforms, and we

demonstrate the ability of the model to accurately recover the injected

parameters. Finally, using standard stochastic samplers employed by the

LIGO-Virgo-KAGRA Collaboration, we analyze a set of real GW signals observed by

the LIGO-Virgo detectors during the first and third runs. We do not find clear

evidence of eccentricity in the signals analyzed, more specifically we measure

$e^{\text{GW150914}}_{\text{gw, 10Hz}}= 0.08^{+0.09}_{-0.06}$,

$e^{\text{GW151226}}_{\text{gw, 20Hz}}= {0.04}^{+0.05}_{-0.04} $, and

$e^{\text{GW190521}}_{\text{gw, 5.5Hz}}= 0.15^{+0.12}_{-0.12}$.

compact-object binaries detected by ground- and spaced-based gravitational-wave

(GW) observatories. Here, we perform for the first time a Bayesian inference

study of inspiral-merger-ringdown eccentric waveforms for binary black holes

with non-precessing spins using two (instead of one) eccentric parameters:

eccentricity and relativistic anomaly. We employ for our study the multipolar

effective-one-body (EOB) waveform model SEOBNRv4EHM, and use initial conditions

such that the eccentric parameters are specified at an orbit-averaged

frequency. We show that this new parametrization of the initial conditions

leads to a more efficient sampling of the parameter space. We also assess the

impact of the relativistic-anomaly parameter by performing mock-signal

injections, and we show that neglecting such a parameter can lead to

significant biases in several binary parameters. We validate our model with

mock-signal injections based on numerical-relativity waveforms, and we

demonstrate the ability of the model to accurately recover the injected

parameters. Finally, using standard stochastic samplers employed by the

LIGO-Virgo-KAGRA Collaboration, we analyze a set of real GW signals observed by

the LIGO-Virgo detectors during the first and third runs. We do not find clear

evidence of eccentricity in the signals analyzed, more specifically we measure

$e^{\text{GW150914}}_{\text{gw, 10Hz}}= 0.08^{+0.09}_{-0.06}$,

$e^{\text{GW151226}}_{\text{gw, 20Hz}}= {0.04}^{+0.05}_{-0.04} $, and

$e^{\text{GW190521}}_{\text{gw, 5.5Hz}}= 0.15^{+0.12}_{-0.12}$.